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This thesis explores what can be accomplished in the ways of time-domain astrophysics with a variety of scales of millimeter interferometry. I touch upon techniques in instrumentation, theory, observation, and computation, showcasing the breadth and richness of the field.
\r\n\r\nThe transient millimeter sky is largely comprised of synchrotron sources whose physical properties are just beginning to be revealed. We are entering an age where new wide-field surveys will exponentially increase the number of known transients, including the first wide-field millimeter survey capable of significant transient detections. As we approach this era, resources dedicated to monitoring and follow-up become increasingly more important.
\r\n\r\nA significant part of my work involves design and commissioning for a new single baseline millimeter interferometer at the Owens Valley Radio Observatory called SPRITE. Uniquely positioned as a dedicated transient follow-up telescope, SPRITE has the ability to observe nearby transients with a relatively high cadence. In this thesis, I also highlight two specific classes of sources for which millimeter observations may be particularly interesting. I present predictions for millimeter emission from supernovae interacting with dense circumstellar media and discuss their rates of detection in upcoming surveys. I additionally present lower frequency spatially-resolved radio observations of an X-ray binary in an active state.
\r\n\r\nOn the other extreme, this thesis also explores the use of very long baseline interferometry to investigate how high resolution images of supermassive black holes vary over the timescale of a year. In 2017, the Event Horizon Telescope Collaboration (EHTC) observed the supermassive black hole in nearby galaxy M87, producing the first resolved image of the shadow of a black hole and potentially revealing intra-day variability of the observed synchrotron emission around the shadow. I present work on the imaging and preliminary analysis of the 2018 epoch of EHT observations of the black hole in M87, and discuss the EHTC\u2019s conclusions of intra-day and year-long variations in the images.
", "date": "2024", "date_type": "degree", "id_number": "CaltechTHESIS:08172023-032920075", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08172023-032920075", "related_url": { "items": [ { "description": "Article adapted for Chapter 2", "type": "doi", "url": "https://doi.org/10.3847/2041-8213/abea19" }, { "description": "Article adapted for Chapter 3", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/ac771f/" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Foundation", "grant_number": "AST-1935980" }, { "agency": "National Science Foundation", "grant_number": "AST-2034306" }, { "agency": "Alan Moffet Funds" }, { "agency": "Mt Cuba Astronomical Foundation" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "suggestions": "request for a full embargo received 2023-08-16. sent to committee.\r\n\r\nFull embargo until 25 February 2024.", "deposited_by": "Nitika Yadlapalli", "deposited_on": "2023-08-28 23:57:29", "doi": "10.7907/g8fs-5q44", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "vikram@astro.caltech.edu", "id": "Ravi-V", "name": { "family": "Ravi", "given": "Vikram" }, "orcid": "0000-0002-7252-5485", "role": "advisor" }, { "email": "klbouman@caltech.edu", "id": "Bouman-Katherine-L", "name": { "family": "Bouman", "given": "Katherine L." }, "orcid": "0000-0003-0077-4367", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "orcid": "0000-0002-3330-5439", "role": "chair" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" }, { "email": "esp@caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "vikram@astro.caltech.edu", "id": "Ravi-V", "name": { "family": "Ravi", "given": "Vikram" }, "orcid": "0000-0002-7252-5485", "role": "member" }, { "email": "klbouman@caltech.edu", "id": "Bouman-Katherine-L", "name": { "family": "Bouman", "given": "Katherine L." }, "orcid": "0000-0003-0077-4367", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2023-06-30", "gradofc_approval_date": "2023-08-25", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2024", "author_list": "Yadlapalli, Nitika" }, { "id": "/id/eprint/15128", "eprint_id": 15128, "rev_number": 32, "documents": [ { "id": "/id/document/138307", "doc_id": 138307, "rev_number": 6, "files": [ { "id": "/id/file/404881", "fileid": 404881, "datasetid": "document", "objectid": 138307, "filename": "DongDillon_Caltech_PhD_thesis_final.pdf", "mime_type": "application/pdf", "hash": "34cc311158b7609c1abaf0b187287bb9", "hash_type": "MD5", "filesize": 7437155, "mtime": "2023-04-04 21:18:30", "url": "/15128/1/DongDillon_Caltech_PhD_thesis_final.pdf" } ], "eprint_id": 15128, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "DongDillon_Caltech_PhD_thesis_final.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/138308", "doc_id": 138308, "rev_number": 1, "files": [ { "id": "/id/file/404884", "fileid": 404884, "datasetid": "document", "objectid": 138308, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "2cab45ac8ed69211be524b5bcb5613c8", "hash_type": "MD5", "filesize": 50425, "mtime": "2023-04-04 21:18:56", "url": "/15128/2/indexcodes.txt" } ], "eprint_id": 15128, "pos": 2, "placement": 2, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/138307" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/138307" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/138307" } ] } }, { "id": "/id/document/138316", "doc_id": 138316, "rev_number": 4, "files": [ { "id": "/id/file/404921", "fileid": 404921, "datasetid": "document", "objectid": 138316, "filename": "PhD thesis.zip", "mime_type": "application/zip", "hash": "de867c887e76dfee0ec63d72d82b3101", "hash_type": "MD5", "filesize": 14602334, "mtime": "2023-04-07 18:51:09", "url": "/15128/3/PhD thesis.zip" } ], "eprint_id": 15128, "pos": 3, "placement": 3, "mime_type": "application/zip", "format": "application/zip", "format_desc": "Source files", "language": "en", "security": "internal", "license": "other", "main": "PhD thesis.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" } ], "eprint_status": "archive", "userid": 13039, "dir": "disk0/00/01/51/28", "datestamp": "2023-04-14 18:18:28", "lastmod": "2023-04-21 15:45:56", "status_changed": "2023-04-14 18:18:28", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ddong@nrao.edu", "id": "Dong-Dillon-Zhejun", "name": { "family": "Dong", "given": "Dillon Zhejun" }, "orcid": "0000-0001-9584-2531", "show_email": "YES" } ] }, "title": "Shocks, Jets, and Emerging Nebulae: Direct Detection and Characterization of Extragalactic Radio Transients in the VLA Sky Survey", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy, Radio, Transients", "abstract": "For most of their lives, massive stars and supermassive black holes evolve steadily, changing only gradually on human timescales. But on occasion, these cosmic engines erupt, lighting up their surroundings like flashes in the dark. Under the right conditions, the eruptions can manifest as slow radio transients, rising and fading on timescales of weeks to decades. By finding these transients and observing their evolution, we can study otherwise inaccessible aspects of the engines' lives, and piece together their influence on their surroundings.
\r\n\r\nUntil recently, most of our knowledge of slow radio transients came from follow-up observations of explosions first discovered as optical and high-energy transients. This avenue of discovery, while illuminating, provides an indelibly incomplete picture of the radio transient landscape. Moreover, each successful follow-up detection typically comes at the cost of many unsuccessful attempts (measured in both telescope and human time).
\r\n\r\nMy thesis helps address these issues by finding and characterizing transients directly in radio surveys. By applying novel transient detection techniques to data from the Very Large Array Sky Survey (VLASS), I produced the first uniformly selected sample of radio transients associated with local universe galaxies. The 64 transients in my sample have roughly doubled the total number of directly detected slow radio transients in the literature. This sample has enabled the first volume-limited characterization of the demographics of extragalactic slow radio transients. It has also facilitated the discovery of two previously unseen transient types: the merger of a compact object with a massive star and a decades-old emerging pulsar wind nebula.
\r\n\r\nThese early results used only ~15% of the currently available data from VLASS and focused only on extragalactic transients at low redshift. By applying the same techniques to the full survey, I have found ~2000 new transients, increasing the number of known slow radio transients (detected by any means) by a further order of magnitude. With this new sample, my collaborators and I are beginning to shift the study of slow radio transients from the domain of single-object deep-dives to the domain of statistical samples.
", "date": "2023", "date_type": "degree", "id_number": "CaltechTHESIS:04042023-210926442", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04042023-210926442", "related_url": { "items": [ { "description": "Article adapted for Ch. 3", "type": "doi", "url": "https://doi.org/10.1126/science.abg6037" }, { "description": "Article adapted for Ch. 4", "type": "doi", "url": "https://doi.org/10.48550/arXiv.2206.11911" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST- 165481" }, { "agency": "United States \u2013 Israel Binational Science Foundation", "grant_number": "018154" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Restricted to [Staff Use Only] until 21 April 2023. Released 2023-04-21.", "deposited_by": "Dillon Dong", "deposited_on": "2023-04-14 18:18:28", "doi": "10.7907/xwy9-tc17", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kchatziioannou@caltech.edu", "id": "Chatziioannou-Katerina", "name": { "family": "Chatziioannou", "given": "Katerina" }, "orcid": "0000-0002-5833-413X", "role": "chair" }, { "email": "vikram@astro.caltech.edu", "id": "Ravi-V", "name": { "family": "Ravi", "given": "Vikram" }, "orcid": "0000-0002-7252-5485", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "jfuller@caltech.edu", "id": "Fuller-James", "name": { "family": "Fuller", "given": "James" }, "orcid": "0000-0002-4544-0750", "role": "member" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2022-12-16", "gradofc_approval_date": "2023-04-21", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2023", "author_list": "Dong, Dillon Zhejun" }, { "id": "/id/eprint/15061", "eprint_id": 15061, "rev_number": 44, "documents": [ { "id": "/id/document/137937", "doc_id": 137937, "rev_number": 4, "files": [ { "id": "/id/file/400860", "fileid": 400860, "datasetid": "document", "objectid": 137937, "filename": "Understanding_the_Cosmological_Evolution_of_Galaxies_with_Intensity_Mapping.pdf", "mime_type": "application/pdf", "hash": "ca9d200fe8cf67bdaa6be62d03ab6c39", "hash_type": "MD5", "filesize": 14263442, "mtime": "2022-11-05 14:25:32", "url": "/15061/1/Understanding_the_Cosmological_Evolution_of_Galaxies_with_Intensity_Mapping.pdf" } ], "eprint_id": 15061, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Understanding_the_Cosmological_Evolution_of_Galaxies_with_Intensity_Mapping.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/137938", "doc_id": 137938, "rev_number": 1, "files": [ { "id": "/id/file/400863", "fileid": 400863, "datasetid": "document", "objectid": 137938, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "96731c63ade610932ce1d1d9e2588190", "hash_type": "MD5", "filesize": 48719, "mtime": "2022-11-05 14:35:44", "url": "/15061/2/indexcodes.txt" } ], "eprint_id": 15061, "pos": 2, "placement": 2, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/137937" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/137937" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/137937" } ] } }, { "id": "/id/document/137956", "doc_id": 137956, "rev_number": 3, "files": [ { "id": "/id/file/401929", "fileid": 401929, "datasetid": "document", "objectid": 137956, "filename": "Understanding_the_Cosmological_Evolution_of_Galaxies_with_Intensity_Mapping.zip", "mime_type": "application/zip", "hash": "3f83a286047913760af66c28b8f0817d", "hash_type": "MD5", "filesize": 14704035, "mtime": "2022-11-15 16:52:19", "url": "/15061/3/Understanding_the_Cosmological_Evolution_of_Galaxies_with_Intensity_Mapping.zip" } ], "eprint_id": 15061, "pos": 3, "placement": 3, "mime_type": "application/zip", "format": "application/zip", "format_desc": "source files", "language": "en", "security": "internal", "license": "other", "main": "Understanding_the_Cosmological_Evolution_of_Galaxies_with_Intensity_Mapping.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" } ], "eprint_status": "archive", "userid": 12883, "dir": "disk0/00/01/50/61", "datestamp": "2022-12-01 19:06:01", "lastmod": "2023-06-16 16:43:44", "status_changed": "2022-12-01 19:06:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jsun.astro@gmail.com", "id": "Sun-Guochao", "name": { "family": "Sun", "given": "Guochao" }, "orcid": "0000-0003-4070-497X", "show_email": "YES" } ] }, "title": "Understanding the Cosmological Evolution of Galaxies with Intensity Mapping", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies: formation; galaxies: evolution; dark ages, reionization, first stars; cosmic background radiation; large-scale structure of Universe", "abstract": "The intensity mapping (IM) technique has been proven to be a powerful addition to the toolkit for understanding the cosmology and astrophysics behind cosmic structure formation. From the nearby universe to the epochs of cosmic dawn and reionization, by mapping the large-scale structure traced by a certain intensity field, IM provides an economical and a holistic view of the formation and evolution of galaxies in the cosmological text, in a way that is highly complementary to traditional methods based on individual galaxy detections. In this thesis, I present a number of theoretical perspectives on how the IM technique, especially line intensity mapping (LIM), can help us better understand the cosmological evolution of galaxies --- all the way to the intriguing era of first galaxy formation.
\r\n\r\nIn the first part of this thesis, I use the Tomographic Ionized-carbon Mapping Experiment (TIME), a pathfinder for LIM observations of the 158-micron [CII] line emission from the epoch of reionization (EoR), as an example to demonstrate the aspects of high-redshift star-forming galaxies that can be practically studied with LIM. In Chapter 2, I elaborate the science cases of TIME for the investigations of the EoR using the redshifted [CII] line as a star formation rate tracer, and the cosmic molecular gas content near cosmic noon using CO rotational lines redshifted into the same observing bandpass. The results also guide the design of future phases of TIME. In Chapter 3, I introduce and demonstrate an effective masking strategy for the cleaning of line interlopers such as CO from the [CII] data TIME will measure. Using proxies of CO emitters built from stacking analysis of deep, near-infrared selected galaxies, it provides a practical solution to the notoriously challenging line confusion problem for LIM data analysis.
\r\n\r\nThe second part of this thesis focuses on the concept of multi-tracer LIM, namely the synergies among LIM observations of multiple distinct tracers. Forward modeling and inference tools based on semi-analytic models and semi-numerical simulations are developed to explore and showcase the scientific potential of multi-tracer LIM. In Chapter 4, I describe a self-consistent, semi-analytic framework for modeling a variety of LIM signals from the multi-phase interstellar medium (ISM) of galaxies, and use it to illustrate the potential application of LIM to shed light on mean ISM properties of galaxies. In Chapters 5 and 6, I present a new semi-numerical simulation called LIMFAST that is developed for efficiently and self-consistently simulating a plethora of IM signals in the high-redshift universe. The LIMFAST code is particularly tailored for revealing the connection between the EoR and the first galaxy formation with multiple cosmological probes.
\r\n\r\nFinally, in the last part of thesis, I show two example case studies where the IM technique is applied to investigate the astrophysics of star formation in galaxies. In Chapter 7, I present an updated analysis of the contributions from star-forming galaxies at z\u22735 to the observed cosmic near-infrared background. Imprints that reveal the formation histories of first stars, including the prospects for detecting them with the forthcoming space missions, are also studied. In Chapter 8, I describe a novel way to constrain the global star formation law of galaxies using LIM measurements of the baryonic acoustic oscillations.
\r\n\r\nAs an emerging technique in observational cosmology, IM is no doubt still in its early days, promising exciting scientific returns while facing various practical challenges. Studies described in this thesis represent only a tiny fraction of the theoretical efforts from the community, but they pave the way for more follow-up investigations that will eventually turn IM into a truly rewarding endeavor.
", "date": "2023", "date_type": "degree", "id_number": "CaltechTHESIS:11052022-133519365", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:11052022-133519365", "related_url": { "items": [ { "description": "Article adapted for Ch. 2", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/abfe62" }, { "description": "Article adapted for Ch. 3", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/aab3e3" }, { "description": "Article adapted for Ch. 4", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/ab55df" }, { "description": "Article adapted for Ch. 5", "type": "arxiv", "url": "https://arxiv.org/abs/2206.14185" }, { "description": "Article adapted for Ch. 6", "type": "arxiv", "url": "https://arxiv.org/abs/2206.14186" }, { "description": "Article adapted for Ch. 7", "type": "doi", "url": "https://doi.org/10.1093/mnras/stab2697" }, { "description": "Article adapted for Ch. 8", "type": "doi", "url": "https://doi.org/10.3847/2041-8213/ac7138" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released 2022-12-08 after 1-week embargo.", "deposited_by": "Guochao Sun", "deposited_on": "2022-12-01 19:06:01", "doi": "10.7907/fzqw-2m61", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "chair" }, { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "member" }, { "email": "tzu@caltech.edu", "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "Tzu-Ching" }, "orcid": "0000-0001-5929-4187", "role": "member" }, { "email": "sfurlane@astro.ucla.edu", "id": "Furlanetto-S-R", "name": { "family": "Furlanetto", "given": "Steven R." }, "orcid": "0000-0002-0658-1243", "role": "member" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2022-07-11", "gradofc_approval_date": "2022-12-01", "thesis_awards": "France A. C\u00f3rdova Graduate Student Fund, 2022.", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2023", "author_list": "Sun, Guochao" }, { "id": "/id/eprint/15203", "eprint_id": 15203, "rev_number": 59, "documents": [ { "id": "/id/document/138854", "doc_id": 138854, "rev_number": 4, "files": [ { "id": "/id/file/408447", "fileid": 408447, "datasetid": "document", "objectid": 138854, "filename": "AhmedSoliman_Thesis_Final.pdf", "mime_type": "application/pdf", "hash": "52baaae270a28968c4d45bb980138061", "hash_type": "MD5", "filesize": 32483299, "mtime": "2023-05-25 20:56:38", "url": "/15203/1/AhmedSoliman_Thesis_Final.pdf" } ], "eprint_id": 15203, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "AhmedSoliman_Thesis_Final.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/138855", "doc_id": 138855, "rev_number": 3, "files": [ { "id": "/id/file/408451", "fileid": 408451, "datasetid": "document", "objectid": 138855, "filename": "AhmedSoliman_Thesis_Final.zip", "mime_type": "application/zip", "hash": "46bffaefac1aae105f401cfd7bec98b8", "hash_type": "MD5", "filesize": 54742323, "mtime": "2023-05-25 20:57:35", "url": "/15203/2/AhmedSoliman_Thesis_Final.zip" } ], "eprint_id": 15203, "pos": 2, "placement": 2, "mime_type": "application/zip", "format": "application/zip", "format_desc": "My Latex thesis.zip that includes everything", "language": "en", "security": "internal", "license": "other", "main": "AhmedSoliman_Thesis_Final.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/138856", "doc_id": 138856, "rev_number": 1, "files": [ { "id": "/id/file/408467", "fileid": 408467, "datasetid": "document", "objectid": 138856, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "a6b1703210be67b27f4ff189abccfbab", "hash_type": "MD5", "filesize": 27072, "mtime": "2023-05-25 21:27:04", "url": "/15203/3/indexcodes.txt" } ], "eprint_id": 15203, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/138854" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/138854" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/138854" } ] } } ], "eprint_status": "archive", "userid": 13076, "dir": "disk0/00/01/52/03", "datestamp": "2023-05-26 22:37:04", "lastmod": "2023-11-08 00:45:39", "status_changed": "2023-05-26 22:37:04", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "dr.amsoliman2020@gmail.com", "id": "Mohamed-Soliman-Ahmed-Mohamed", "name": { "family": "Mohamed Soliman", "given": "Ahmed Mohamed" }, "orcid": "0009-0007-9335-1326", "show_email": "YES" } ] }, "title": "BICEP Array Detectors and Instrumentation at 30/40 GHz: Design, Performance, and Deployment to the South Pole for Constraining Primordial Gravitational Waves", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmic Microwave Background; cosmology; Big Bang; Inflation; primordial gravitational waves; cryogenic instrumentation; BICEP Array; CMB polarimeters; Galactic Foregrounds, telescopes; detectors.", "abstract": "The discovery of the Cosmic Microwave Background (CMB) in the 1960s has provided strong observational evidence for the Big Bang cosmological model to describe the origin and evolution of the universe. The theory of cosmic inflation was developed in the 1980s to account for the initial density perturbations by a period of exponential expansion in the early Universe to solve the horizon, flatness and monopole problems. Many inflation models predict potentially detectable primordial gravitational-waves (PGWs) background that imprint a B-mode polarization pattern in the CMB. The amplitude of the inflationary B-mode polarization depends on the energy scale of inflation and is parameterized by the tensor-to-scalar ratio r. The detection of a B-mode pattern would open a new window to probe the energy scale at the beginning of time when the universe was a mere fraction of a second old after the Big Bang.
\r\n\r\nThe BICEP/Keck collaboration is building a series of experiments located at the Amundsen-Scott South Pole Station to map the polarization of the CMB at degree angular scales using small-aperture telescopes. Our latest BICEP/Keck publications use data collected through 2018 and report the strongest constraints r0.05 < 0.036 at 95% confidence. The current sensitivity on r is limited by the variance from the gravitational lensing. BICEP/Keck is starting a collaboration with the South Pole Telescope (SPT) team to develop delensing techniques to improve future constraints on r. Characterizing Galactic foregrounds, especially synchrotron emission, remains a priority in order to improve constraints as statistical sensitivity continues to improve. The motivation for this thesis is to develop a highly sensitive receiver at 30 and 40 GHz, at frequencies where the synchrotron foreground dominates. BICEP Array represents the latest phase in the BICEP/Keck experiments, and will map the polarization of the CMB at 30/40, 95, 150, and 220/270 GHz. BICEP Array will search for PGWs with unprecedented sensitivity levels on r by characterizing and removing Galactic synchrotron and dust emission from our maps of the CMB.
\r\n\r\nMy PhD thesis focuses on the technology development for high sensitivity detectors and instrumentation to successfully deploy the first BICEP Array receiver at 30 GHz and 40 GHz to the South Pole in order to constrain the Galactic synchrotron foreground. My dissertation presents the receiver design and performance. I will first explain the engineering design principles, the fabrication and a laboratory demonstration of single-color antenna-coupled Transition Edge Sensor (TES) bolometers. Secondly, I will discuss the design and demonstration of dual-color detectors at 30 and 40 GHz that gain receiver sensitivity by increasing the optical throughput and bandwidth of each pixel. I also developed microstrip diplexer circuits that divide the detector bandwidth into two CMB observing channels. I optimized this approach to design the dual-color bowtie-coupled detector at 90/150 GHz. Thirdly, I will introduce a new wide-band corrugated focal plane module design to minimize the beam mismatch systematic at 30 and 40 GHz bands simultaneously. Our receivers map polarization of the CMB by taking the difference between co-located and orthogonally polarized pair of detectors. Polarized beam difference measurements show a differential beam response due to a shift between the polarization beam centers within a pixel due to an electromagnetic interaction with the focal plane frame. The residual beams leak a temperature to polarization (T-P) in the CMB polarization maps and can produce a false B-mode signal that introduces non-negligible systematic errors for BICEP Array measurements to come with improved sensitivity. The wide-band design reduces this effect and associated systematic errors for 30 and 40 GHz receiver. I also developed a new single-band corrugated focal plane module design for 150 GHz receiver. I performed laboratory measurements of these designs at 30, 40, and 150 GHz to verify the modelled response. The corrugation design will also be extended to the 220/270 GHz receiver. Fourthly, I will show my contributions to the receiver deployment, integration and calibration during the first 2020 observing season. The measurements will include the full optical characterization of the detector camera, in-lab and on-sky sensitivity at the South Pole. I will also describe the tests done to diagnose the challenges during the first season and new upgrades during the second 2022 season to improve the overall sensitivity of the receiver. Improved detector modules have been installed during the 2023 season to further boost the mapping speed for measuring the synchrotron foreground.
\r\n\r\nThe technologies developed for BICEP Array feed into capabilities for the upcoming CMB-S4 program. For example, I used similar methods to design a diplexer for a CMB-S4 dual-color feedhorn-coupled detector design at 90/150 GHz. I will also detail my work on the cryogenic implementation and test of an Adiabatic Demagnetization Refrigerator suitable for demonstrating 100 mK CMB-S4 detector arrays in a prototype 95/150 GHz telescope planned to observe on the BICEP Array.
", "date": "2023", "date_type": "degree", "id_number": "CaltechTHESIS:05232023-174453276", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05232023-174453276", "related_url": { "items": [ { "description": "Improved constraints on primordial gravitational waves using Planck, WMAP, and BICEP/Keck observations through the 2018 observing season", "type": "doi", "url": "https://doi.org/10.1103/PhysRevLett.127.151301" }, { "description": "BICEP Array: a multi-frequency degree-scale CMB polarimeter", "type": "doi", "url": "https://doi.org/10.1117/12.2311725" }, { "description": "Design and performance of the First BICEP Array receiver", "type": "doi", "url": "https://doi.org/10.1007/s10909-020-02394-6" }, { "description": "Optical design and characterization of 40-GHz detector and module for the BICEP Array", "type": "doi", "url": "https://doi.org/10.1007/s10909-019-02299-z" }, { "description": "Design and performance of wide-band corrugated walls for the BICEP Array detector modules at 30/40 GHz", "type": "doi", "url": "https://doi.org/10.1117/12.2312942" }, { "description": "Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole", "type": "doi", "url": "https://doi.org/10.48550/arXiv.2012.04047" }, { "description": "2022 upgrade and improved low frequency camera sensitivity for CMB observation at the South Pole", "type": "doi", "url": "https://doi.org/10.1117/12.2628058" }, { "description": "A demonstration of improved constraints on primordial gravitational waves with delensing", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.103.022004" }, { "description": "Bicep/Keck XV: The Bicep3 cosmic microwave background polarimeter and the first three-year data set", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/ac4886" }, { "description": "BICEP2/Keck Array XI: Beam characterization and temperature-to-polarization leakage in the BK15 data set", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/ab391d" } ] }, "projects": { "items": [ "The National Science Foundation \"Collaborative Research: Imaging the Beginning of Time from the South Pole: The next Stage of the BICEP Program\"", "The National Science Foundation \"MRI: Development of a 150 GHz Receiver for the BICEP Array CMB Polarimeter\"", "NASA \"Superconducting Antenna-Coupled Detectors and Readouts for CMB polarimetry in PICO\"" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released 2023-06-02 after 1-week embargo.", "deposited_by": "Ahmed Mohamed Mohamed", "deposited_on": "2023-05-26 22:37:04", "doi": "10.7907/srdx-w019", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "chair" }, { "email": "barish@caltech.edu", "id": "Barish-B-C", "name": { "family": "Barish", "given": "Barry C." }, "role": "member" }, { "email": "roger.c.obrient@jpl.nasa.gov", "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "Roger" }, "orcid": "0000-0002-4987-6375", "role": "member" }, { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2023-02-06", "gradofc_approval_date": "2023-05-26", "thesis_awards": "Everhart Distinguished Graduate Student Lecturer Award, 2023. \r\nThe Antarctica Service Medal of the United States of America, 2020, awarded by the National Science Foundation and Department of Defense in recognition of valuable contributions to exploration and scientific achievement under the U.S. Antarctic program, for BICAP Array receiver deployment to the South Pole during 2020 and 2022 seasons. The National Science Foundation Award for two projects as a contributor. The Second Prize for the Best Student Paper Award, IEEE Asia Pacific Radio Science Conference, South Korea, 2016.", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2023", "author_list": "Mohamed Soliman, Ahmed Mohamed" }, { "id": "/id/eprint/14581", "eprint_id": 14581, "rev_number": 63, "documents": [ { "id": "/id/document/136339", "doc_id": 136339, "rev_number": 6, "files": [ { "id": "/id/file/391608", "fileid": 391608, "datasetid": "document", "objectid": 136339, "filename": "main.pdf", "mime_type": "application/pdf", "hash": "57549eb868d6718932c3b293de2615ae", "hash_type": "MD5", "filesize": 6635412, "mtime": "2022-05-16 19:30:16", "url": "/14581/1/main.pdf" } ], "eprint_id": 14581, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis", "language": "en", "security": "public", "license": "cc_by_nc_sa", "main": "main.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/136342", "doc_id": 136342, "rev_number": 3, "files": [ { "id": "/id/file/391616", "fileid": 391616, "datasetid": "document", "objectid": 136342, "filename": "delosReyes_thesis.zip", "mime_type": "application/zip", "hash": "b360c32b2424170e7fe3cd4d692b7849", "hash_type": "MD5", "filesize": 51409260, "mtime": "2022-05-16 19:34:28", "url": "/14581/2/delosReyes_thesis.zip" } ], "eprint_id": 14581, "pos": 2, "placement": 2, "mime_type": "application/zip", "format": "application/zip", "format_desc": "LaTeX source files for final version of thesis", "language": "en", "security": "internal", "license": "other", "main": "delosReyes_thesis.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/136345", "doc_id": 136345, "rev_number": 5, "files": [ { "id": "/id/file/391633", "fileid": 391633, "datasetid": "document", "objectid": 136345, "filename": "delosReyes_supp.zip", "mime_type": "application/zip", "hash": "55f4d3e8dcd4b0ecb764ba3b272e22e8", "hash_type": "MD5", "filesize": 156869, "mtime": "2022-05-16 19:53:52", "url": "/14581/3/delosReyes_supp.zip" } ], "eprint_id": 14581, "pos": 3, "placement": 3, "mime_type": "application/zip", "format": "application/zip", "format_desc": "Supplemental data tables", "language": "en", "security": "public", "license": "cc_by_nc_sa", "main": "delosReyes_supp.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "supplemental" }, { "id": "/id/document/136356", "doc_id": 136356, "rev_number": 1, "files": [ { "id": "/id/file/391674", "fileid": 391674, "datasetid": "document", "objectid": 136356, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "9a0c89b6c53d6b98f66cee9f67f4c8db", "hash_type": "MD5", "filesize": 46263, "mtime": "2022-05-16 19:55:54", "url": "/14581/4/indexcodes.txt" } ], "eprint_id": 14581, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/136339" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/136339" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/136339" } ] } } ], "eprint_status": "archive", "userid": 12803, "dir": "disk0/00/01/45/81", "datestamp": "2022-05-27 23:10:58", "lastmod": "2022-08-04 23:13:44", "status_changed": "2022-05-27 23:10:58", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mithidelosreyes@gmail.com", "id": "de-los-Reyes-Mithi-Alexa-Caballes", "name": { "family": "de los Reyes", "given": "Mithi Alexa Caballes" }, "orcid": "0000-0002-4739-046X", "show_email": "NO" } ] }, "title": "Dwarf Galaxies in the Local Universe as Probes of Stellar and Galactic Evolution", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies; dwarf galaxies; chemical abundances; star formation; Local Group", "abstract": "Low-mass \"dwarf\" galaxies are numerous, diverse, and relatively simple, making them excellent laboratories for understanding both stellar and galactic evolution. Dwarf galaxies (galaxies with stellar masses 107-109 solar masses) in the nearby universe (out to distances of ~10 Mpc from our own Milky Way, or redshifts z \u227e 0.01), are a particularly interesting population due to their proximity, which allows us to study them in detail on both spatially-resolved and global scales. In this thesis, I present a variety of observational studies investigating star formation and chemical enrichment within nearby dwarf galaxies.
\r\n\r\nI first use the chemical abundances of individual stars within Local Group dwarf spheroidal galaxies (dSphs) to understand how past stars lived and died. I use this \"galactic archaeology\" approach to test theoretical models of Type Ia supernovae by investigating the nucleosynthetic products of these supernovae. For example, using medium-resolution spectra from DEIMOS, I measure manganese abundances that place observational constraints on the masses of Type Ia progenitors. I also describe a novel method to measure the delay-time distribution of Type Ia SNe in an individual dSph, which probes the number of white dwarfs involved in Type Ia SNe. Finally, I show how galactic archaeology can also be used to trace star formation using a simple chemical evolution model.
\r\n\r\nFor more distant galaxies, in which individual stars cannot be resolved, galaxy properties can be measured on larger scales. Using the integral field spectrograph KCWI, I produce spatially-resolved maps of dwarf galaxies located in extremely under-dense regions called cosmic voids. The dynamical properties of these galaxies provide insight into the formation of dwarf galaxies in the absence of large-scale environmental effects. On even larger spatial scales, I use photometry to measure the global properties of galaxies and understand the physical processes that drive star formation on galaxy-wide scales.
\r\n\r\nThese studies pave the way for future work with ongoing and upcoming surveys that will map out our local universe---and the dwarf galaxies around us---in unprecedented detail.
", "date": "2022", "date_type": "degree", "id_number": "CaltechTHESIS:05162022-191523325", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05162022-191523325", "related_url": { "items": [ { "description": "Article adapted for ch. 2", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/ab736f" }, { "description": "Article adapted for ch. 4", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/ac332b" }, { "description": "Article adapted for ch. 6", "type": "doi", "url": "https://doi.org/10.3847/ 1538-4357/aafa82" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NSF", "grant_number": "AST-1847909" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "3MT Competition (Caltech)", "Astronomy Department" ] }, "suggestions": "2022-06-03 released PDF and supplemental data after 1-week embargo.", "deposited_by": "Mithi Alexa de los Reyes", "deposited_on": "2022-05-27 23:10:58", "doi": "10.7907/4bz3-2t66", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "enk@astro.caltech.edu", "id": "Kirby-Evan-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mansi@astro.caltech.edu", "id": "Kasliwal-Mansi-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938", "role": "chair" }, { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162", "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "vikram@caltech.edu", "id": "Ravi-V", "name": { "family": "Ravi", "given": "Vikram" }, "orcid": "0000-0002-7252-5485", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2022-05-09", "gradofc_approval_date": "2022-05-27", "thesis_awards": "Caltech Three Minute Thesis (3MT) competition, 2021, 1st Place & People\u2019s Choice.", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2022", "author_list": "de los Reyes, Mithi Alexa Caballes" }, { "id": "/id/eprint/14158", "eprint_id": 14158, "rev_number": 29, "documents": [ { "id": "/id/document/119171", "doc_id": 119171, "rev_number": 4, "files": [ { "id": "/id/file/361950", "fileid": 361950, "datasetid": "document", "objectid": 119171, "filename": "CBochenekThesis.pdf", "mime_type": "application/pdf", "hash": "4cb2cd080dce98805b2f93479f23cb02", "hash_type": "MD5", "filesize": 7479981, "mtime": "2021-06-01 00:51:58", "url": "/14158/1/CBochenekThesis.pdf" } ], "eprint_id": 14158, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "CBochenekThesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/119172", "doc_id": 119172, "rev_number": 2, "files": [ { "id": "/id/file/361953", "fileid": 361953, "datasetid": "document", "objectid": 119172, "filename": "CBochenekThesis.zip", "mime_type": "application/zip", "hash": "2358cf83d88a596045f4f1cccdab80d3", "hash_type": "MD5", "filesize": 7871298, "mtime": "2021-06-01 00:53:47", "url": "/14158/2/CBochenekThesis.zip" } ], "eprint_id": 14158, "pos": 2, "placement": 2, "mime_type": "application/zip", "format": "application/zip", "language": "en", "security": "internal", "license": "other", "main": "CBochenekThesis.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/131616", "doc_id": 131616, "rev_number": 1, "files": [ { "id": "/id/file/377059", "fileid": 377059, "datasetid": "document", "objectid": 131616, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "af63d76e806e7a8dd56b81df242f9233", "hash_type": "MD5", "filesize": 26773, "mtime": "2021-06-24 18:06:48", "url": "/14158/3/indexcodes.txt" } ], "eprint_id": 14158, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/119171" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/119171" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/119171" } ] } } ], "eprint_status": "archive", "userid": 12375, "dir": "disk0/00/01/41/58", "datestamp": "2021-06-02 23:15:57", "lastmod": "2022-01-12 00:01:49", "status_changed": "2021-06-02 23:15:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "bochenekchristopher@gmail.com", "id": "Bochenek-Christopher-David", "name": { "family": "Bochenek", "given": "Christopher David" }, "orcid": "0000-0003-3875-9568", "show_email": "NO" } ] }, "title": "The Progenitors of Fast Radio Bursts", "ispublished": "unpub", "full_text_status": "public", "keywords": "Radio transient sources; Radio bursts; Magnetars; Neutron stars; Galaxy: general; instrumentation: detectors; methods: observational; radio continuum: general;\r\nSun: radio radiation", "abstract": "Fast radio bursts (FRBs) are millisecond duration pulses of radio emission that are bright enough to be seen from other galaxies. The nature of the objects that produce fast radio bursts has captivated the interest of astronomers since their discovery in 2007. The durations and energetics of FRBs imply a compact, highly magnetized progenitor, making magnetars a popular progenitor candidate. However, it is difficult to pin down the progenitors of FRBs because they occur so far away. In this thesis, I will present the Survey for Transient Astronomical Radio Emission 2 (STARE2), an experiment designed to detect FRBs in the Milky Way. I will present a formalism through which to interpret the results of this experiment and demonstrate our experiment's effectiveness with the detection of a solar burst. Using STARE2, we discovered the first FRB that originated within the Milky Way, FRB 200428. This FRB was traced back to the Galactic magnetar SGR J1935+2154. The energetics, spectro-temporal properties, host galaxy, environment, and X-ray counterpart are all consistent with the properties of extragalactic FRBs. In addition, the high volumetric rate of these bright radio bursts from magnetars is consistent with the volumetric rate of FRBs, implying that magnetars are the dominant channel of FRB production. I will then develop a novel statistical technique to compare transient host galaxies in order to evaluate whether the hosts of extragalactic FRBs are consistent with a magnetar origin. I will find that the hosts of FRBs are consistent with the hosts of core-collapse supernovae, supporting the hypothesis that magnetars produce FRBs. Finally, I will present two ideas for future observing campaigns to find FRBs from M82 and more extremely bright pulses from Galactic magnetars.
", "date": "2021", "date_type": "degree", "id_number": "CaltechTHESIS:05192021-014425301", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05192021-014425301", "related_url": { "items": [ { "description": "Article adapted for Chapter 2", "type": "doi", "url": "https://doi.org/10.1088/1538-3873/ab63b3" }, { "description": "Article adapted for Chapter 3", "type": "doi", "url": "https://doi.org/10.1038/s41586-020-2872-x" }, { "description": "Article adapted for Chapter 4", "type": "doi", "url": "https://doi.org/10.3847/2041-8213/abd634" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Alan Moffet Funds" }, { "agency": "JPL President's and Director's Fund" }, { "agency": "Heising-Simons Foundation" }, { "agency": "NSF", "grant_number": "AST-1836018" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Christopher Bochenek", "deposited_on": "2021-06-02 23:15:57", "doi": "10.7907/7tsx-x524", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "vikram@astro.caltech.edu", "id": "Ravi-V", "name": { "family": "Ravi", "given": "Vikram" }, "orcid": "0000-0002-7252-5485", "role": "co-advisor" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "vikram@astro.caltech.edu", "id": "Ravi-V", "name": { "family": "Ravi", "given": "Vikram" }, "orcid": "0000-0002-7252-5485", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "esp@astro.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2021-05-18", "gradofc_approval_date": "2021-06-02", "thesis_awards": "France A. C\u00f3rdova Graduate Student Fund, 2019. Garmire Scholar.", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2021", "author_list": "Bochenek, Christopher David" }, { "id": "/id/eprint/14184", "eprint_id": 14184, "rev_number": 42, "documents": [ { "id": "/id/document/119173", "doc_id": 119173, "rev_number": 4, "files": [ { "id": "/id/file/361955", "fileid": 361955, "datasetid": "document", "objectid": 119173, "filename": "Yanjun_Xu_PhD_Thesis_2021.pdf", "mime_type": "application/pdf", "hash": "725d512ce74db3722a0611b2d4e1eb9f", "hash_type": "MD5", "filesize": 8993893, "mtime": "2021-06-01 00:54:19", "url": "/14184/1/Yanjun_Xu_PhD_Thesis_2021.pdf" } ], "eprint_id": 14184, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis file in PDF", "language": "en", "security": "public", "license": "other", "main": "Yanjun_Xu_PhD_Thesis_2021.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/119174", "doc_id": 119174, "rev_number": 3, "files": [ { "id": "/id/file/361957", "fileid": 361957, "datasetid": "document", "objectid": 119174, "filename": "Yanjun_Xu_PhD_Thesis_2021.zip", "mime_type": "application/zip", "hash": "b7a88fb23e4b4023ded7f8b059f98358", "hash_type": "MD5", "filesize": 7468933, "mtime": "2021-06-01 01:02:19", "url": "/14184/2/Yanjun_Xu_PhD_Thesis_2021.zip" } ], "eprint_id": 14184, "pos": 2, "placement": 2, "mime_type": "application/zip", "format": "application/zip", "format_desc": "source TEX file in .zip", "language": "en", "security": "internal", "license": "other", "main": "Yanjun_Xu_PhD_Thesis_2021.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/131615", "doc_id": 131615, "rev_number": 1, "files": [ { "id": "/id/file/377058", "fileid": 377058, "datasetid": "document", "objectid": 131615, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "861422aabbcc1bd49c45d66b1c9f33b1", "hash_type": "MD5", "filesize": 36787, "mtime": "2021-06-24 18:06:42", "url": "/14184/3/indexcodes.txt" } ], "eprint_id": 14184, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/119173" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/119173" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/119173" } ] } } ], "eprint_status": "archive", "userid": 12430, "dir": "disk0/00/01/41/84", "datestamp": "2021-06-03 17:59:44", "lastmod": "2021-06-10 15:48:07", "status_changed": "2021-06-03 17:59:44", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "yjxu723@gmail.com", "id": "Xu-Yanjun", "name": { "family": "Xu", "given": "Yanjun" }, "orcid": "0000-0003-2443-3698", "show_email": "NO" } ] }, "title": "Probing the Inner Accretion Flow Properties Around Black Holes with X-ray Observations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Accretion; black hole physics; black hole X-ray binaries; active galactic nuclei", "abstract": "Accretion, governed by gravity, is a fundamental source of energy in the universe. Accretion is important to the growth and evolution of black holes, as well as the structure in the universe on larger scales. Accretion disks around supermassive black holes are likely to have produced most of the ionizing radiation in the universe since the epoch of reionization. Outflows launched from the accretion disk of black holes, either in the form of disk winds or jets, provide a feedback mechanism that plays an important role in the co-evolution of black holes and their host galaxies. It has been decades since the fundamental theories about black hole accretion were established. Black hole accretion has been widely studied in active galactic nuclei (AGNs) and black hole binaries ever since the early days of X-ray astronomy. However, important questions still remain regarding the fundamental physical properties of black holes, the structure and geometry of accretion disks and coronae, and the nature of disk winds and jets.
\r\n\r\nIn this thesis, I report results from recent X-ray observations of an ultra-luminous infrared galaxy with a central AGN, IRAS 05189\u20132524, and several black hole X-ray binaries (or black hole candidates for those currently lacking dynamical mass determinations), IGR J17091\u20133624, MAXI J1535\u2013571, Swift J1658.2\u20134242, MAXI J1631\u2013479, and MAXI J1820+070. Most of the black hole X-ray binaries studied in this thesis were uncatalogued sources and were discovered as bright Galactic X-ray transients over the past few years, offering great opportunities for investigating black hole accretion with high quality datasets. The launch of the NuSTAR telescope in 2012 has brought the advanced capabilities of performing high sensitivity observations in the hard X-ray band and remaining free from pile-up for bright Galactic sources, providing new angles for the detailed study of observational phenomena around both supermassive and stellar-mass accreting black holes. I study the inner accretion flow properties around black holes in the above objects by conducting spectral and timing analyses of the NuSTAR observations and the simultaneous soft X-ray band data from the Swift or XMM-Newton telescope. I have searched for and analyzed various accretion related observational features in these systems (disk reflection spectra, ionized absorption caused by disk winds, quasi periodic oscillations (QPOs) in the X-ray light curves, and unusual aperiodic flux variations or accretion state changes), and interpret the results in terms of the physical properties about the inner accretion flows and the central black holes.
\r\n\r\nBy modeling the relativistic disk reflection spectra, I have found that the inner edge of the optically-thick accretion disk is truncated in IGR J17091\u20133624 during the bright hard state, in MAXI J1631\u2013479 during the very high state, and in MAXI J1820+070 during the faint hard state, whereas the inner accretion disk is consistent with extending down to the ISCO in MAXI J1535\u2013571 and Swift J1658.2\u20134242 during their bright hard states, and in MAXI J1631\u2013479 during its soft state. Based on all the observational evidence gathered in this thesis, the general picture about the accretion flow geometry at different accretion states seems to be more complicated than that from previously well accepted theoretical predictions. In addition, I have measured the black holes spins and inner accretion disk inclinations for IRAS 05189\u20132524, MAXI J1535\u2013571, Swift J1658.2\u20134242, and MAXI J1631\u2013479 using the disk reflection modeling method, where the central black holes are all found to be rapidly spinning. There are also evidence for strong disk winds detected in the X-ray spectra of some of the objects studied in this thesis with interesting implications. I summarize my studies of these individual objects at the end of this thesis in a more broader context of the characteristic behaviors of the population and their general physical implications, and discuss about the possibilities of extending my research in this direction with the upcoming new X-ray missions.
", "date": "2021", "date_type": "degree", "id_number": "CaltechTHESIS:05272021-232230617", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05272021-232230617", "related_url": { "items": [ { "description": "Published paper adapted for Chapter 2", "type": "doi", "url": "https://iopscience.iop.org/article/10.3847/1538-4357/aa5df4" }, { "description": "Published paper adapted for Chapter 3", "type": "doi", "url": "https://iopscience.iop.org/article/10.3847/1538-4357/aa9ab4" }, { "description": "Published paper adapted for Chapter 4", "type": "doi", "url": "https://iopscience.iop.org/article/10.3847/2041-8213/aaa4b2" }, { "description": "Published paper adapted for Chapter 5", "type": "doi", "url": "https://iopscience.iop.org/article/10.3847/1538-4357/aada03" }, { "description": "Published paper adapted for Chapter 6", "type": "doi", "url": "https://iopscience.iop.org/article/10.3847/1538-4357/ab24bf" }, { "description": "Published paper adapted for Chapter 7", "type": "doi", "url": "https://iopscience.iop.org/article/10.3847/1538-4357/ab7dc0" }, { "description": "Published paper adapted for Chapter 8", "type": "doi", "url": "https://iopscience.iop.org/article/10.3847/1538-4357/ab7cdb" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Yanjun Xu", "deposited_on": "2021-06-03 17:59:44", "doi": "10.7907/9kkg-4b58", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "chair" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" }, { "email": "martinc@caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2021-05-19", "gradofc_approval_date": "2021-06-03", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"family": "Leask", "given": "Ellen Kathleen" }, "orcid": "0000-0002-3220-4003", "show_email": "NO" } ] }, "title": "Investigating the Evolution of Surface Water on Mars through Spectroscopy of Secondary Minerals", "ispublished": "unpub", "full_text_status": "public", "keywords": "Mars, mineralogy, remote sensing, spectroscopy", "abstract": "Despite its current arid climate, Mars\u2019 surface preserves a wide variety of morphologies and minerals that point to a water-rich past. However, the mechanisms and timing of this environmental change are not yet well understood. In this dissertation, we explore a variety of water-related minerals through visible-shortwave infrared (VSWIR) reflectance spectroscopy to better understand the environmental conditions at the time of their formation, and trace the evolution of surface water on Mars over time. We also demonstrate the capabilities of VSWIR spectroscopy at laboratory and field scales in a Mars analogue environment (Samail Ophiolite, Oman)\u2014an emerging technique for use on future landed missions that enables us to differentiate between spectrally-similar minerals and spot rare minerals that help to constrain environmental conditions and better understand the geologic context of samples. On Mars, we use orbital datasets (predominantly CRISM, the Compact Reconnaissance Imaging Spectrometer for Mars) to investigate secondary minerals in the southern highlands of Mars, focusing on perchlorate, chloride, and sulphate minerals. We identify a previously unknown artifact in the CRISM dataset, which mimics perchlorate absorptions; previous orbital perchlorate detections (including those associated with recurring slope lineae) are not robust when data are reprocessed, suggesting that there may not be orbitally-detectable reservoirs of perchlorate on Mars, which would enable liquid brines to exist at the surface today. A detailed investigation of chloride deposits across the southern highlands of Mars points to an episodic surface-runoff water source rather than upwelling groundwater, a process which continued to create chloride deposits into the Amazonian era. Where chloride and sulphate deposits are in close proximity (Terra Sirenum, Mars), they do not appear to be genetically related as they often are on Earth; instead, they point to chemically distinct groundwater vs. surface water reservoirs in Terra Sirenum through the Hesperian and into the Amazonian. Together, these studies indicate that briny and/or acidic volumes of water at the surface capable of creating mineral deposits continued to exist \u2014 at least episodically \u2014 on Mars into the Amazonian, rather than ceasing much earlier in Mars\u2019 history.
", "date": "2020", "date_type": "degree", "id_number": "CaltechTHESIS:02192020-182835054", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:02192020-182835054", "related_url": { "items": [ { "description": "Chapter 2 publication.", "type": "pub", "url": "https://ieeexplore.ieee.org/abstract/document/8071774" }, { "description": "Chapter 4 publication.", "type": "doi", "url": "https://doi.org/10.1029/2018GL080077" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "2021-09-30 file released with advisor permission.\r\n\r\nCourtesy extension to 30 September 2021 by Kathy. // Contact Bethany Ehlmann directly about any further extensions, as she will be taking over the manuscripts. skj 12152020//\r\nEmbargo extension request pending but recommended as of 2020-08-17. Restricted to Caltech community until 14 February 2021. // \r\n\r\nFrom author: As a direct result of the COVID-19 pandemic, I have been unable to convert unpublished thesis chapters into papers, and there is an known unscrupulous scientist in the field who has already recreated a portion of my work (presented at a conference), and included it in their own paper without citation or acknowledgement. If possible, I would like to extend the embargo to enable me to submit the papers for publication before the thesis chapters are publicly available. All data analyzed in two unpublished chapters are from NASA missions and therefore publicly available. \r\n\r\n// Original embargo request // Restricted to Caltech community until 20 August 2020. // From author: Unpublished chapters in thesis, intending to submit to JGR:Planets in the near future.", "deposited_by": "Ellen Leask", "deposited_on": "2020-02-20 22:09:35", "doi": "10.7907/TWR4-N128", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "grr@gps.caltech.edu", "id": "Rossman-G-R", "name": { "family": "Rossman", "given": "George Robert" }, "role": "chair" }, { "email": "grotz@gps.caltech.edu", "id": "Grotzinger-J-P", "name": { "family": "Grotzinger", "given": "John P." }, "role": "member" }, { "email": "wfischer@caltech.edu", "id": "Fischer-W-W", "name": { "family": "Fischer", "given": "Woodward W." }, "role": "member" }, { "email": "cfranken@caltech.edu", "id": "Frankenberg-C", "name": { "family": "Frankenberg", "given": "Christian" }, "role": "member" }, { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2020-01-09", "gradofc_approval_date": "2020-02-02", "review_status": "approved", "option_major": { "items": [ "geol" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2020", "author_list": "Leask, Ellen Kathleen" }, { "id": "/id/eprint/11803", "eprint_id": 11803, "rev_number": 90, "documents": [ { "id": "/id/document/104382", "doc_id": 104382, "rev_number": 4, "files": [ { "id": "/id/file/313638", "fileid": 313638, "datasetid": "document", "objectid": 104382, "filename": "AndersonDana_thesis.zip", "mime_type": "application/x-zip", "hash": "696a642cb994fead38370e77903f643b", "hash_type": "MD5", "filesize": 18406463, "mtime": "2019-11-12 19:36:16", "url": "/11803/2/AndersonDana_thesis.zip" } ], "eprint_id": 11803, "pos": 2, "placement": 2, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "Source Files", "language": "en", "security": "internal", "license": "other", "main": "AndersonDana_thesis.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", 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Breakdown Spectroscopy (LIBS), MSL Curiosity", "abstract": "The formation of planets begins with collisions of tiny, micron-sized, dust grains. These grains reside in structures known as protoplanetary disks, rotating disks consisting of gas and dust that encircle young protostars as a natural outcome of star formation. Although the processes of planet formation and evolution take place over millions and billions of years, in our limited view we can only see snapshots of the different stages. Many of the formative processes are difficult, if not impossible, to observe directly. However, evidence of these events exists in the chemical composition of the bulk material and surfaces of planets themselves, the gas and solid components of protoplanetary disks, and planetary debris such as asteroids and comets. This thesis utilizes modeling and observations of the carbon and nitrogen content of protoplanetary disks to shed light on key factors that control the formation and chemical composition of planets. In addition, this thesis advances techniques for the elemental analysis of planetary surfaces facilitating the detection of salts on the surface of Mars.
\r\n\r\nChapter 2 estimates the maximum potential destruction of solid, refractory carbon in protoplanetary disks in an effort to explain the lack of carbon found in meteorites and the bulk silicate Earth relative to the interstellar materials that seeded their formation. In a T-Tauri disk assuming uniform turbulence and passive heating from stellar photons destruction of refractory carbon sources via oxidation and UV photolysis is limited to the warm, photochemically-active disk surface layers. Exploration of distinct disk environments, considering non-idealized mass transport or enhanced disk heating due to active stellar mass accretion, is needed to explain the widespread lack of carbon in rocky solar-system bodies.
\r\n\r\nChapters 3 and 4 present spectral observations by the Atacama Large Millimeter/submillimeter Array (ALMA) of mature, 5-11 Myr-old, protoplanetary disks in the Upper Scorpius region that indicate diverging behavior of the key carbon and nitrogen species in the disk gas as disks evolve. Selective depletion of CO from the gas may cause disk gas masses to be underestimated if based on CO measurements alone and further investigation of additional gas tracers is warranted.
\r\n\r\nDepletion of CO from the gas in the outer regions of disks observed by ALMA may be the result of sequestration of carbon into less volatile species such as CO2 and CH3OH. Chapter 5 explores the fate of CO2 and CH3OH ices entering the inner regions of protoplanetary disks. Carbon returns to CO in unshielded transparent regions of the inner disk surface, consistent with infrared observations, but carbon reservoirs in the disk midplane may be distinct depending on the efficiency of mass transport in the disk.
\r\n\r\nChapter 6 examines the abilities of the Laser-Induced Breakdown Spectroscopy (LIBS) instrument ChemCam on the Mars rover Curiosity in regards to the detection of salts. LIBS analysis of a set of prepared sample pellets containing decreasing concentrations of salt identifies elemental emission lines of Cl, C, and S that are sensitive to changes in chloride, carbonate, and sulfate salt concentrations, respectively, and provides detection limits for ChemCam measurements of these salts.
", "date": "2020", "date_type": "degree", "id_number": "CaltechTHESIS:09282019-173537468", "refereed": "FALSE", "official_url": "http://resolver.caltech.edu/CaltechTHESIS:09282019-173537468", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/aa7da1" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/ab2cb5" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "https://doi.org/10.1002/2016JE005164" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "DGE-1144469" }, { "agency": "NSF", "grant_number": "AST-1514918" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Dana Anderson", "deposited_on": "2019-12-04 17:41:58", "doi": "10.7907/GZSA-DK98", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "orcid": "0000-0002-2745-3240", "role": "chair" }, { "email": "kbatygin@caltech.edu", "id": "Batygin-K", "name": { "family": "Batygin", "given": "Konstantin" }, "orcid": "0000-0002-7094-7908", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-08-12", "gradofc_approval_date": "2019-11-26", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. 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"2020-12-18 02:19:11", "status_changed": "2020-01-21 22:24:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jacob.jencson@gmail.com", "id": "Jencson-Jacob-Edmund", "name": { "family": "Jencson", "given": "Jacob Edmund" }, "orcid": "0000-0001-5754-4007", "show_email": "NO" } ] }, "title": "Hunting for Hidden Explosions: Exploring the Transient Infrared Sky with the Spitzer Space Telescope", "ispublished": "unpub", "full_text_status": "public", "keywords": "Time-domain astrophysics; transients; stars; infrared; supernovae", "abstract": "The study of time-variable astronomical phenomena is undergoing an explosive renaissance ushered in by recent advancements in capabilities to monitor the sky from radio to gamma rays. The infrared region of the electromagnetic spectrum provides a unique window to uncover a vast array of stellar eruptions and explosions that are otherwise obscured; however, the dynamic infrared sky has remained largely unexplored.
\r\n\r\nTo uncover these hidden cosmic explosions, I undertook a systematic search in the infrared with the Spitzer Space Telescope called SPIRITS \u2014 the SPitzer InfraRed Intensive Transients Survey. Targeting a specially chosen sample of nearby galaxies, the search revealed a bounty of exceptionally red events, and may have discovered entirely new and diverse populations, including deeply embedded supernovae, catastrophic stellar mergers, and giant eruptions of massive, violently unstable stars. Providing a first census of stellar infrared transients, SPIRITS has paved the way for new and upcoming surveys to further expand our exploration of the dynamic infrared sky.
", "date": "2020", "date_type": "degree", "id_number": "CaltechTHESIS:01132020-093113401", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01132020-093113401", "related_url": { "items": [ { "description": "Article adapted for Ch. 2.", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/aa618f" }, { "description": "Article adapted for Ch. 3.", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/aacf8b" }, { "description": "Article adapted for Ch. 4.", "type": "doi", "url": "https://doi.org/10.3847/2041-8213/ab2c05" }, { "description": "Article adapted for Ch. 5.", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/ab4a01" } ] }, "projects": { "items": [ "SPitzer InfraRed Intensive Transients Survey" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Foundation Graduate Research Fellowship", "grant_number": "DGE-1144469" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Jacob Jencson", "deposited_on": "2020-01-21 22:24:26", "doi": "10.7907/Y9H7-XA93", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mansi@astro.caltech.edu", "id": "Kasliwal-Mansi-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "chair" }, { "email": "mansi@astro.caltech.edu", "id": "Kasliwal-Mansi-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "role": "member" }, { "email": "eps@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/104427" } ] } } ], "eprint_status": "archive", "userid": 11524, "dir": "disk0/00/01/35/59", "datestamp": "2019-12-04 18:21:24", "lastmod": "2020-03-27 23:55:23", "status_changed": "2019-12-04 18:21:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ginaeduggan@gmail.com", "id": "Duggan-Gina-Elizabeth", "name": { "family": "Duggan", "given": "Gina Elizabeth" }, "orcid": "0000-0002-9256-6735", "show_email": "NO" } ] }, "title": "Signatures of the r-Process in Ancient Stellar Populations Using Barium Abundances", "ispublished": "unpub", "full_text_status": "public", "keywords": "Galaxies: abundances \u2013 galaxies: dwarf \u2013 galaxies: evolution \u2013 Local Group \u2013 nuclear reactions,\r\nnucleosynthesis, abundances \u2013 stars: abundances", "abstract": "For over sixty years scientists have known that a large percentage of heavy elements are created by the rapid neutron-capture process (r-process). However, a clear picture of where the r-process occurs has remained elusive. Many astrophysical origins have been proposed -- each with a range of possible chemical yields and rates. Discovering which origin (or combinations of origins) truly produce the heavy elements we see on Earth is a daunting task.
\r\n\r\nThis thesis seeks to provide observational constraints to pinpoint the dominant origin of the r-process. The majority of this thesis uses Galactic Archaeology to look for r-process signatures in ancient stellar populations (e.g., dwarf galaxies and globular clusters). These ancient stellar populations provide the clearest \"experiments\" to observe how quickly and how much r-process was created. The r-process signature we observe is the amount of barium in individual red giant branch stars in these stellar populations. Chapter 2 discusses how these barium measurements are made from individual extragalactic stars and presents the largest catalog of barium abundances in dwarf galaxies to date.
\r\n\r\nChapter 3 compares the r-process signature -- barium -- to other elements (e.g., magnesium and iron) in the same galaxy to see how the timescale of r-process enrichment compares to the other abundances (whose origins are known). This analysis found that the r-process timescale was more delayed than core-collapse supernovae. This points to neutron star mergers (NSMs) as the dominant source of r-process in the early history of dwarf galaxies.
\r\n\r\nChapter 4 uses a galactic chemical evolution model to test what r-process timescales, yields, and rates are needed to recreate the observations presented in Chapter 2. Preliminary results indicate that NSMs must be included in order for the model to match the observations. In addition, Chapter 4 presents what yield of barium is needed from NSMs to recreate the observations.
\r\n\r\nChapter 5 tests if the stars in the globular cluster M15 were enriched by the r-process after they were born. M15 has an unusual abundance pattern with ~ 1 dex variation in r-process abundances even though most other elements, including iron, do not show a variation. New measurements of barium abundances in main sequence and red giant branch stars of M15 show that the stars were born with their r-process enrichment. This means that an r-process event occurred quickly after the cluster was born -- while it was still forming stars -- and resulted in uneven enrichment.
\r\n\r\nFinally, Chapter 6 presents a solution to one of the technical challenges in locating the sites of r-process nucleosynthesis. Chapter 6 describes how to accurately measure the position and orientation of the CCDs in Zwicky Transient Facility's (ZTF's) camera. ZTF is a transient survey that -- among other science goals -- searches for the electromagnetic counterpart of NSM detections with LIGO. The work included in this chapter increased the survey efficiency of ZTF, which will aid ZTF in localizing transient events, including NSMs. Following up NSMs found by LIGO can provide direct measurements of the amount of r-process material created by NSMs.
\r\n\r\nAltogether, this thesis has made strides to identifying the origin of the r-process. Chapters 3 and 4 identify NSMs as the dominant source of r-process elements in dwarf galaxies. However, Chapter 5 found that globular cluster M15 needs a r-process event to occur quickly -- quicker than is typically expected from a NSM. The observational constraints that have resulted from this thesis provide important clues to where the heaviest elements are made.
", "date": "2020", "date_type": "degree", "id_number": "CaltechTHESIS:11082019-215827632", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:11082019-215827632", "related_url": { "items": [ { "description": "Article adapted for Chapters 2 and 3.", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/aaeb8e" }, { "description": "Proceedings adapted for Chapter 7.", "type": "doi", "url": "https://doi.org/10.1117/12.2309994" }, { "description": "Machine-readable tables from Chapter 2.", "type": "doi", "url": "https://doi.org/10.22002/d1.1308" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "DGE\u20101745301" }, { "agency": "NSF", "grant_number": "AST-1614081" }, { "agency": "NSF", "grant_number": "AST-1440341" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Gina Duggan", "deposited_on": "2019-12-04 18:21:24", "doi": "10.7907/D0A8-BM50", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "enk@astro.caltech.edu", "id": "Kirby-Evan-N", "name": { "family": "Kirby", "given": "Evan N." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "chair" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "jlm@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "member" }, { "email": "raja@ucolick.org", "id": "Guhathakurta-Puragra", "name": { "family": "Guhathakurta", "given": "Puragra" }, "role": "member" }, { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-10-21", "gradofc_approval_date": "2019-11-26", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2020", "author_list": "Duggan, Gina Elizabeth" }, { "id": "/id/eprint/13698", "eprint_id": 13698, "rev_number": 45, "documents": [ { "id": "/id/document/107659", "doc_id": 107659, "rev_number": 5, "files": [ { "id": "/id/file/330020", "fileid": 330020, "datasetid": "document", "objectid": 107659, "filename": "giesler_thesis_2020.pdf", "mime_type": "application/pdf", "hash": "274e31fb6cddea0a3e661a1fb232487d", "hash_type": "MD5", "filesize": 13899204, "mtime": "2020-05-08 04:58:12", "url": "/13698/1/giesler_thesis_2020.pdf" } ], "eprint_id": 13698, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "giesler_thesis_2020.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/107659" } ] } } ], "eprint_status": "archive", "userid": 12287, "dir": "disk0/00/01/36/98", "datestamp": "2020-05-12 16:08:12", "lastmod": "2020-06-12 18:49:45", "status_changed": "2020-05-12 16:08:12", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mattgiesler@gmail.com", "id": "Giesler-Matthew-David", "name": { "family": "Giesler", "given": "Matthew David" }, "orcid": "0000-0003-2300-893X", "show_email": "NO" } ] }, "title": "Probing the Nature of Black Holes with Gravitational Waves", "ispublished": "unpub", "full_text_status": "public", "keywords": "Black holes; numerical relativity; general relativity; gravitational waves; ringdown;", "abstract": "In this thesis, I present a number of studies intended to improve our understanding of black holes using gravitational waves. Although black holes are relatively well understood from a theory perspective, many questions remain about the nature of the black holes in our Universe. According to general relativity, astrophysical black holes are fully described by just their mass and spin. Yet, relying on electromagnetic-based observatories alone, we still know very little about the distribution of black hole masses or spins. Moreover, as merging black holes are invisible to these electromagnetic observatories, we cannot rely on them to provide us with information about the binary black hole merger rate or binary black hole formation channels. However, by observing gravitational wave signals from these inherently dark binaries, we will soon have some answers to these questions. Indeed, the Laser Interferometer Gravitational-Wave Observatory (LIGO) has already revealed a great deal of new information about binary black holes; giving us an early glimpse into their mass and spin distributions and placing the first constraints on the binary black hole merger rate. This thesis contributes to the goal of probing the nature of black holes with gravitational waves.
\r\n\r\nBinary black holes can form as an isolated binary in the galactic field or through dynamical encounters in high-density environments. Dynamical formation can significantly alter the binary parameters, which then become imprinted on the gravitational waveform. By simulating varying black hole populations in high-density globular clusters, we identify a population of highly eccentric binary black hole mergers that are characteristic of dynamical formation. Although these systems would circularize by the time they are visible in LIGO's frequency band, the future Laser Interferometer Space Antenna (LISA) is capable of distinguishing this population of eccentric mergers from the circular mergers expected of isolated field-formed binaries. As these dynamically formed binaries depend on the size of the underlying black hole population in globular clusters, we can utilize the dynamically formed merger rate to infer globular cluster black hole populations -- allowing us to reveal information about binary black hole birth environments.
\r\n\r\nIn order to properly estimate the parameters of binary black holes from detected gravitational wave signals, such as their masses and spins, high-accuracy waveforms are a needed. The highest accuracy waveforms are those produced by numerical relativity simulations, which solve the full Einstein equations. Using the Spectral Einstein Code (SpEC), we expand the reach of numerical relativity to simulate binary black holes with nearly extremal spins, i.e., black holes with spins near the maximal value \u03c7 = 1. These waveforms are used to calibrate existing waveform approximants used in LIGO data analyses. This ensures that the systematic errors in these approximants are small enough that if highly-spinning systems are observed, the spins are recovered without bias. Although rapidly spinning binaries have remained elusive thus far, these waveforms ensure that the highest-spin systems can be detected in the quest to uncover the spin distribution of black holes.
\r\n\r\nThe end state of a binary black hole merger is a newly born, single black hole that rings down like a struck bell, sending its last few ripples of gravitational waves out into the spacetime. Embedded in this 'ringdown' signal are a multitude of specific frequencies. Einstein's theory of general relativity precisely predicts the ringdown frequencies of a black hole with a given mass and spin. The statement that a black hole is entirely described by just these two parameters is known as the no-hair theorem. For black holes that obey the laws of general relativity (and consequently, the no-hair theorem), these frequencies serve as a fingerprint for the black hole. However, if the objects we observe are not Einstein's black holes, but instead something more exotic, the frequencies will not have this property and this would be a spectacular surprise. A minimum of two tones are required for this test, each with an associated frequency and damping time that depend only on the mass and spin. The conventional no-hair test relies on the so-called 'fundamental' tones of a black hole. A test relying on the fundamental modes is not expected to be feasible for another ~10-15 years, after detector sensitivity has improved significantly. However, by analyzing the ringdown of high-accuracy numerical relativity waveforms, we show that modes beyond the fundamental, known as 'overtones', are detectable in current detectors. The overtones are short-lived, but this is countered by the fact that they can initially be much stronger than the fundamental mode. By measuring two tones in the ringdown of GW150914 we perform a first test of the no-hair theorem. While the current constraints are rather loose, this first test serves as a proof of principle. This is just one example of the powerful tests that can be employed with overtones using present day detectors and the even more precise tests that can be accomplished with LISA in the future.
", "date": "2020", "date_type": "degree", "id_number": "CaltechTHESIS:05062020-201707675", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05062020-201707675", "related_url": { "items": [ { "description": "Chapter 2", "type": "doi", "url": "https://doi.org/10.1093/mnras/sty659" }, { "description": "Chapter 3", "type": "doi", "url": "https://doi.org/10.1088/0264-9381/32/10/105009" }, { "description": "Chapter 4", "type": "doi", "url": "https://doi.org/10.1103/PhysRevX.9.041060" }, { "description": "Chapter 5", "type": "doi", "url": "https://doi.org/10.1103/PhysRevLett.123.111102" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-1151197" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "NSF", "grant_number": "ACI-1440083" }, { "agency": "NSF", "grant_number": "PHY-1440083" }, { "agency": "NSF", "grant_number": "AST-1333520" }, { "agency": "NSF", "grant_number": "TG-PHY990007N" }, { "agency": "NSF", "grant_number": "PHY-1708212" }, { "agency": "NSF", "grant_number": "PHY-1708213" }, { "agency": "NSF", "grant_number": "PHY-1606654" }, { "agency": "NSF", "grant_number": "ACI-1713678" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Matthew Giesler", "deposited_on": "2020-05-12 16:08:12", "doi": "10.7907/akwv-r373", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "saul@caltech.edu", "id": "Teukolsky-Saul-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "chair" }, { "email": "saul@caltech.edu", "id": "Teukolsky-Saul-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "role": "member" }, { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "role": "member" }, { "email": "rana@caltech.edu", "id": "Adhikari-R", "name": { "family": "Adhikari", "given": "Rana" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2020-02-25", "gradofc_approval_date": "2020-05-11", "thesis_awards": "Robert F. Christy Prize for an Outstanding Doctoral Thesis in Theoretical Physics, 2020.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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that surround young stars. Thus, to understand how these solar systems come to be, it is necessary to study the conditions within these disks. Until recently, such studies have required a focus on intrinsically brighter and younger disks that are easier to observe. However, a full picture of planet formation requires the characterization of older disks to determine how these systems change over time. The unprecedented capabilities of the Atacama Large Millimeter/submillimeter Array (ALMA) now present the opportunity to study populations of these disks in detail for the first time. In this thesis, I present a study of over 100 such disks in the 5-11 Myr old Upper Scorpius OB Association (Upper Sco) using ALMA, as well as Keck Observatory, with the aim of comparing the properties of these systems to younger disks in order to shed new light on disk evolution.
\r\n\r\n\r\nFollowing background discussion on disks and their evolution, ALMA measurements of the continuum and CO line fluxes of these disks at 0.88 mm are reported in Chapter 3. The continuum fluxes are used to show that the majority of these systems contain less than 1 M\u2295 of dust. It is then shown that dust masses around these stars are on average a factor of \u223c4.5 lower than their younger counterparts in the Taurus star-forming region, placing important constraints on the mass evolution of these systems. Finally, constraints on depletion of gas in these disks are discussed using the CO measurements.
\r\n\r\n\r\nThe spatial distributions of the gas and dust within these Upper Sco disks are modeled in Chapter 4. The radial extents of gas and dust are measured and compared, with several systems showing evidence of the gas being more extended. The sizes of the dust disks are compared to younger systems, showing that these disks shrink by a factor of approximately three as they age. These results suggest that dust evolves from the outside-in within disks, perhaps through radial drift. Despite this evolution, dust disks in Upper Sco fall on the same correlation between size and millimeter luminosity as their younger counterparts. This implies a link between the radial structures of disks of different ages, perhaps indicating that these systems are composed of optically-thick dust substructure.
\r\n\r\n\r\nOf course, an understanding of planetary system formation would be incomplete without accounting for the presence of stellar companions, which are common around young stars and are expected to shorten disk lifetimes by truncating their sizes. As such, Chapter 5 presents a search for stellar companions in the Upper Sco disk sample analyzed in Chapters 3 and 4. Using adaptive optics imaging and aperture masking observations with the NIRC2 instrument on the Keck II telescope, stellar companions are identified in 27 of 112 systems. It is then shown that the companion fraction of systems with disks is lower than those without, confirming the harmful effects of stellar companions on disks seen in younger systems. However, the fraction of disk systems in Upper Sco with a close companion is shown to match that of younger disks in Taurus. This indicates that these effects occur within the first \u223cMyr of disk evolution, after which stellar companions have little to no effect. Additionally, while the millimeter luminosities of disks with stellar companions are observed to be lower than those around single stars in Taurus, there exists no such difference in Upper Sco. This provides further support for outside-in dust evolution, as the shrinking of disks around single stars would cause them by the 5-11 Myr age of Upper Sco to match the sizes and brightnesses of truncated disks in binary systems.
\r\n\r\n\r\nTaken together, the results presented in this thesis show the masses and radial extents of the dust-component of circumstellar disks decrease with age. This thesis concludes by summarizing these results and discussing their link within a scenario of outside-in dust evolution involving radial drift and dust substructure. To close, potential avenues are presented to continue the study of disk evolution with ALMA.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05152019-180537558", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05152019-180537558", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Scott Barenfeld", "deposited_on": "2019-05-17 21:42:57", "doi": "10.7907/5DK0-H549", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "John.Carpenter@alma.cl", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "co-advisor" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "John.Carpenter@alma.cl", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "member" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "member" }, { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-10-05", "gradofc_approval_date": "2019-05-17", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. 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"archive", "userid": 11998, "dir": "disk0/00/01/17/08", "datestamp": "2019-06-10 22:26:16", "lastmod": "2023-05-30 22:21:07", "status_changed": "2019-06-10 22:26:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mike.grudich@gmail.com", "id": "Grudi\u0107-Michael-Yvan", "name": { "family": "Grudi\u0107", "given": "Michael Yvan" }, "orcid": "0000-0002-1655-5604", "show_email": "NO" } ] }, "title": "The Role of Stellar Feedback in Star Cluster Formation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Star formation; stellar feedback; magnetohydrodynamics; numerical methods; Star clusters; Galaxy formation; astrophysics\r\n", "abstract": "A methodology for numerical magnetohydrodynamics simulations of star cluster formation, accounting for all mechanisms of stellar feedback from massive stars, is developed and used to address a range of problems regarding the formation of stars and star clusters in giant molecular clouds (GMCs). These studies culminate in a new theoretical framework that connects properties of GMCs to those of the star clusters that form in them.
\r\n\r\nThe simulation methodology is established and tested, and the problem of the star formation efficiency (SFE) of molecular clouds is addressed. It is found that SFE is set by the balance of feedback and gravity, with very weak dependence upon other factors. A simple dimensional scaling law with cloud surface density emerges from the complex interplay of different feedback physics. Parameter space is found where feedback must fail, and the SFE is high, and the implications of this prediction are explored.
\r\n\r\nThe star clusters formed in the simulations are found to resemble observed young, massive star clusters in the form of their surface brightness profiles, leading to the hypothesis that this structure is a result of the star formation process. It is shown that the shallow, power-law density profiles characteristic of young clusters is predicted by the hierarchical star formation scenario. It is shown that the SFE law, when coupled to an analytic cloud collapse model, predicts that gas should be exhausted by highly-efficient star formation at a stellar surface density of \u223c 105 \u2212 106 Msun pc-2, consistent with the maximum observed.
\r\n\r\nA new suite of simulations is developed to specifically model GMCs in the Milky Way. It is found that the picture of feedback-disrupted star formation is able to account for both the normalization and the scatter in the measured SFE of GMCs in the Milky Way, the first theory to do so.
\r\n\r\nThe uncertainty in the simulated SFE due to the choice of feedback prescription is quantified, by running a controlled methods study of several different prescriptions in the literature. In the cloud model simulated, the choice of prescription affects the simulated SFE at the factor of \u223c 3 level, explaining discrepancies in the literature and identifying the small-scale details of massive star formation as the main uncertainty in cluster formation simulations.
\r\n\r\nFinally, the simulation suite is extended to model massive GMCs in local spiral galaxies, and to simulate 10 random realizations at each point in parameter space, mapping out the stochastic nature of star cluster formation in GMCs. A model is calibrated to the simulation results, taking the cloud bulk properties as input parameters, and predicting the detailed properties of the star clusters formed in it. A star cluster catalogue is synthesized from observed GMCs in M83, and good agreement is found with observed star cluster properties, including the fraction of stars in bound clusters, the maximum cluster mass, and the distribution of cluster sizes.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:06072019-111646558", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06072019-111646558", "related_url": { "items": [ { "description": "Article in Chapter 2", "type": "doi", "url": "https://doi.org/10.1093/mnras/sty035" }, { "description": "Article in Chapter 3", "type": "doi", "url": "https://doi.org/10.1093/mnras/sty2303" }, { "description": "Article in Chapter 4", "type": "doi", "url": "https://doi.org/10.1093/mnras/sty3386" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Michael Grudic", "deposited_on": "2019-06-10 22:26:16", "doi": "10.7907/7FBG-TE87", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162", "role": "chair" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "murray@cita.utoronto.ca", "id": "Murray-N-M", "name": { "family": "Murray", "given": "Norman" }, "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-22", "gradofc_approval_date": "2019-06-10", "thesis_awards": "Robert F. Christy Prize for an Outstanding Doctoral Thesis in Theoretical Physics, 2019. James A. Cullen Memorial Fellowship Fund, 2018.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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23, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/105224" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/105224" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/105224" } ] } } ], "eprint_status": "archive", "userid": 10901, "dir": "disk0/00/01/17/11", "datestamp": "2019-06-07 23:55:30", "lastmod": "2020-03-10 23:48:47", "status_changed": "2019-06-10 22:50:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "nancy.h.thomas@gmail.com", "id": "Thomas-Nancy-Helen", "name": { "family": "Thomas", "given": "Nancy Helen" }, "orcid": "0000-0003-1989-4860", "show_email": "NO" } ] }, "title": "Remotely Sensing Aqueous Alteration on Mars: Innovative Statistical and Analytical Methods for Large Spectral Datasets", "ispublished": "unpub", "full_text_status": "public", "keywords": "Mars, aqueous alteration, remote sensing, spectroscopy, MSL Curiosity", "abstract": "Liquid water once flowed on Mars and altered the crust. Aqueous minerals and salts record a rich history of aqueous processes and environmental changes. In this dissertation, I developed and applied innovative analytical and statistical methods to large spectral datasets to better characterize aqueous alteration on Mars. The Mars Science Laboratory (MSL) Curiosity rover is investigating the sedimentary sequence at Gale crater recording a potentially global transition from clay-enriched to sulfate-enriched rocks. Volatile elements like H and Cl are important for investigating aqueous processes but are difficult to quantify in the large ChemCam laser-induced breakdown spectroscopy (LIBS) dataset. In the first part of this dissertation, I measured aqueously altered samples with LIBS in the laboratory under Mars-relevant conditions to develop analytical methods for application to ChemCam. The Murray formation, the lowest exposed strata of the sedimentary sequence, contains 2.6 \u00b1 2.1 wt. % H2O. Carriers of H enrichment including clays, opal, Mg-sulfates, Ca-sulfates, hydrous Mn-oxides, akageneite, and jarosite are identified. Variability in the H content of the Murray formation records multiple aqueous alteration events as well as potential increases in salinity in the Gale crater lake. In the fourth chapter, I measured chlorine in Gale crater using multiple MSL instruments. Cl-enrichments correlated with increased Na2O are detected in the bedrock, in nodular textures, and at vein margins, indicating halite. The scattered, isolated occurrences of chlorides are consistent with late groundwater reworking and remobilization. Halite is concentrated in particular members of the Murray formation; the chlorides may have been emplaced as primary deposits in these members, consistent with varying salinity in the past lakewaters. In the second part of this dissertation, I adapted and applied semi-automated statistical methods called factor analysis and target transformation to the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) dataset to systematically search for hematite in stratified, candidate sedimentary outcrops. Few outcrops containing hematite are found and no obvious analogs to terrestrial iron formations are identified. Future studies will search for hematite in other geologic settings as well as other Fe-bearing phases such as Fe-phyllosilicates and Fe-sulfates to better characterize aqueous processes on Mars.", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:06072019-115333958", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06072019-115333958", "related_url": { "items": [ { "description": "Article adapted for ch. 2", "type": "doi", "url": "https://doi.org/10.1029/2017JE005467" }, { "description": "Article adapted for ch. 4", "type": "doi", "url": "https://doi.org/10.1029/2019GL082764" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "NASA MSL Participating Scientist Program" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released to public view 1/7/2020 // Restricted to Caltech community only until 10 December 2019. // From author: Thesis Chapter 4 'Mars Science Laboratory Observations of Chloride Salts in Gale Crater, Mars' under revision with Geophysical Research Letters.\r\n", "deposited_by": "Nancy Thomas", "deposited_on": "2019-06-07 23:55:30", "doi": "10.7907/8JFC-BY64", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "role": "chair" }, { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "member" }, { "email": "wfischer@caltech.edu", "id": "Fischer-W-W", "name": { "family": "Fischer", "given": "Woodward W." }, "role": "member" }, { "email": "grotz@caltech.edu", "id": "Grotzinger-J-P", "name": { "family": "Grotzinger", "given": "John P." }, "role": "member" }, { "email": "grr@caltech.edu", "id": "Rossman-G-R", "name": { "family": "Rossman", "given": "George Robert" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-28", "gradofc_approval_date": "2019-06-10", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2019", "author_list": "Thomas, Nancy Helen" }, { "id": "/id/eprint/11315", "eprint_id": 11315, "rev_number": 31, "documents": [ { "id": "/id/document/95410", "doc_id": 95410, "rev_number": 4, "files": [ { "id": "/id/file/273005", "fileid": 273005, "datasetid": "document", "objectid": 95410, "filename": "songming_du_2018_thesis.pdf", "mime_type": "application/pdf", "hash": "32b8cd79203710dffa673911ac482c5f", "hash_type": "MD5", "filesize": 10077885, "mtime": "2018-12-14 19:11:19", "url": "/11315/1/songming_du_2018_thesis.pdf" } ], "eprint_id": 11315, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "songming_du_2018_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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"eprint_status": "archive", "userid": 10158, "dir": "disk0/00/01/13/15", "datestamp": "2019-01-08 20:27:35", "lastmod": "2021-10-26 18:03:08", "status_changed": "2019-01-08 20:27:35", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "dusm4728@gmail.com", "id": "Du-Song-Ming", "name": { "family": "Du", "given": "Song Ming" }, "orcid": "0000-0003-0083-7014", "show_email": "YES" } ] }, "title": "Fundamental Physics Through Gravitational Waves: From No-Hair Theorem to Quantum Structures of Black Holes", "ispublished": "unpub", "full_text_status": "public", "keywords": "Black Hole, General Relativity, Gravitational Wave, Quantum Gravity", "abstract": "In general relativity, black hole is the simplest macroscopic object in the universe: any black hole can be completely described by its mass, charge and angular mo- mentum. However, such a simple picture might be changed if the gravitational field equations are modified or quantum effects are taken into consideration. These additional hairs of black hole, if exist, may provide valuable information to reveal the deepest mystery of the universe: quantum theory of gravity.
\r\n\r\nIn this thesis, we try to relate the hypothetical extra hairs of black hole with the ob- servational evidence as gravitational waves \u2013 another prediction of general relativity and are recently detected. In Chapter I, we provide a pedagogical introduction to the black hole hairs introduced by modified gravity and quantum mechanics, and lay out a mathematical framework to describe the gravitational wave emission with the existence of near-horizon quantum hair. In Chapter II we show that in scalar-tensor theory of gravity, the formation process of a black hole from gravitational collapse is accompanied with the emission of scalar hair. This mechanism gives rise to a scalar type memory effect of gravitational wave, which does not exist in general relativity. This phenomenon can further be used to study the parameter space of the scalar-tensor theory. In Chapter III, we find the scalar gravitational memory effect from stellar collapses provide the strongest sources for the stochastic gravita- tional wave background with scalar polarization in Brans-Dicke theory. The energy density spectrum for this background is provided and its model dependencies are studied. In Chapter IV, we provide a Green\u2019s function method to study the echoes, which are the gravitational waves reflected by the quantum hair near the event hori- zon of a black hole. In Chapter V, we build phenomenological models to describe the near-horizon quantum hair and predict its implication to the binary black hole stochastic gravitational wave background. Our study indicates that the existence of the quantum hair will significantly increases such a background and pins down the most relevant model parameter to be the area under the effective potential. Further, we also demonstrate that the result is rather robust against the uncertainties about the nature of the near-horizon quantum hair. In the end, a field theory based treatment to the gravitational waves in general relativity is provided as the appendix.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:12132018-230901638", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:12132018-230901638", "related_url": { "items": [ { "description": "Article adapted for Ch. 2", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.94.104063" }, { "description": "Article adapted for Ch. 4", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.96.084002" }, { "description": "Article adapted for Ch. 5", "type": "doi", "url": "https://doi.org/10.1103/PhysRevLett.121.051105" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Walter Burke Institute for Theoretical Physics", "Astronomy Department" ] }, "deposited_by": "Song Ming Du", "deposited_on": "2019-01-08 20:27:35", "doi": "10.7907/YSDX-J506", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "chair" }, { "email": "saul@caltech.edu", "id": "Teukolsky-Saul-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526", "role": "member" }, { "email": "fcp@caltech.edu", "id": "Porter-F-C", "name": { "family": "Porter", "given": "Frank C." }, "orcid": "0000-0003-1948-8889", "role": "member" }, { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-12-20", "gradofc_approval_date": "2019-01-08", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "option_minor": { "items": [ "compsci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"disk0/00/01/13/87", "datestamp": "2019-02-20 20:38:57", "lastmod": "2021-10-26 18:02:38", "status_changed": "2019-02-20 20:38:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kevinbarkett@gmail.com", "id": "Barkett-Kevin-Michael-Canice", "name": { "family": "Barkett", "given": "Kevin Michael Canice" }, "orcid": "0000-0001-8230-4363", "show_email": "YES" } ] }, "title": "Computational Methods for Gravitational Wave Physics: Spectral Cauchy-Characteristic Extraction and Tidal Splicing", "ispublished": "unpub", "full_text_status": "public", "keywords": "Numerical Relativity; Gravitational Waves; Binary Black Hole; Cauchy-Characteristic Extraction; Binary Neutron Star; Tidal Splicing\r\n", "abstract": "As the aLIGO and Virgo detectors continue to improve their sensitivity for observing gravitational waves from merging compact binaries, they will require ever more precise theoretical predictions to extract a detailed understanding of the physics governing these merging systems. This thesis discusses advancements within computing the gravitational waveforms along two avenues of research: the continued development of a spectral Cauchy-Characteristic Extraction (CCE) code and the presentation of a novel method called 'Tidal Splicing' for generating waveforms for binary neutron star (BNS), black hole-neutron star (BHNS), and even Beyond GR systems.
\r\n\r\nDue to the finite extents of typical 3+1 simulations of merging binaries, the waveforms they generate can suffer from near-zone effects and lingering gauge ambiguities. CCE was developed in order evolve radiating gravitational waves as they propagate outward to future null infinity, allowing studies connecting the dynamical spacetime of binary evolutions to effects seen by distant observers, such as superkicks, and angluar and linear momentum fluxes. A recent spectral version of CCE showed promising improvements in accuracy and efficiency over the older finite-differencing code, PittNull. However, lingering issues with the numerics and implementation of the theory prevented it from wide spread use. We detail the developments updated its initial release and demonstrate the enhancement in accuracy they yield beyond the capabilities of PittNull.
\r\n\r\nThe method of Tidal Splicing enhances the inexpensive Post-Newtonian (PN) tidal corrections with BBH waveforms from numerical simulations to generate waveforms corresponding to inpsiraling BNS or BHNS systems. This leverages the accuracy of numerical BBH waveforms to effectively replace the corresponding unknown PN terms. In addition, by picking individual terms in the PN tidal expansions to include, then comparing with existing numerical simulations, we are able to probe the significance of each contribution to the total difference in evolution between BBH and BNS or BHNS inspirals. We also demonstrate how the splicing concepts used for tidal effects can extended in order to model waveforms with corrections according to theories beyond GR using an example case of a resonating ultra-compact object.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:02082019-160046031", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:02082019-160046031", "related_url": { "items": [ { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.93.044064" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Kevin Barkett", "deposited_on": "2019-02-20 20:38:57", "doi": "10.7907/3DH5-7773", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "chair" }, { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "member" }, { "email": "wise@caltech.edu", "id": "Wise-M-B", "name": { "family": "Wise", "given": "Mark B." }, "orcid": "0000-0002-9125-801X", "role": "member" }, { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-12-06", "gradofc_approval_date": "2019-02-20", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2019", "author_list": "Barkett, Kevin Michael Canice" }, { "id": "/id/eprint/11170", "eprint_id": 11170, "rev_number": 40, "documents": [ { "id": "/id/document/94338", "doc_id": 94338, "rev_number": 4, "files": [ { "id": "/id/file/266660", "fileid": 266660, "datasetid": "document", "objectid": 94338, "filename": "kleiser_thesis_2018_final.zip", "mime_type": "application/x-zip", "hash": "10ea8bca9849c5b92de1cdc6da3beed9", "hash_type": "MD5", "filesize": 15337265, "mtime": "2018-09-26 19:31:26", "url": "/11170/7/kleiser_thesis_2018_final.zip" } ], "eprint_id": 11170, "pos": 7, "placement": 7, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "Source Files", "language": "en", "security": "internal", "license": "other", "main": "kleiser_thesis_2018_final.zip", "media_duration": "0", "media_aspect_ratio": "0", 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As some of the most powerful explosions since the Big Bang, they influence not only the chemical but also mechanical evolution of the galaxies they inhabit. They induce star formation and produce the building blocks of planets, organisms, and ultimately, civilizations. Understanding the connections between the supernovae we observe and the stars that would have produced them is a critical piece of understanding this process.
\r\n\r\nUnfortunately, we rarely have the ability to observe the progenitor stars of supernovae directly; it is usually difficult to predict when a given star will explode, and most are in galaxies too distant to allow observation of individual stars. Instead, we typically must leverage our understanding of the explosions themselves to reveal the nature of the stars that produced them. Using analytical and numerical calculations, it is possible to predict the supernovae from certain types of stars and work backwards.
\r\n\r\nIn this thesis, we present a new model for previously elusive rapidly fading supernovae, which we believe are due to the core-collapse explosions of massive stars inside extended hydrogen-free envelopes or previously ejected mass shells. This model requires not only pre-explosion stellar radii of unprecedented size for hydrogen-free stars but also a lack of radioactive nickel, which is usually present in supernovae. We show our process from simple toy models to self-consistent explosions of stellar models and compare our results to existing rapidly fading supernovae. Understanding these unusual transients will shed light on the many possible ways stars behave shortly before death and also may be critical for understanding the population of core-collapse supernovae as a whole.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:09032018-174351545", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09032018-174351545", "related_url": { "items": [ { "description": "Article adapted for Ch. 6", "type": "ads", "url": "http://adsabs.harvard.edu/abs/2018arXiv180909103K" }, { "description": "Article adapted for Ch. 5", "type": "ads", "url": "http://adsabs.harvard.edu/abs/2018MNRAS.475.3152K" }, { "description": "Article adapted for Ch. 4", "type": "ads", "url": "http://adsabs.harvard.edu/abs/2014MNRAS.438..318K" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Nuclear Security Administration", "grant_number": "Krell Institute Fellowship Award" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Io Kleiser", "deposited_on": "2018-11-27 19:29:11", "doi": "10.7907/5YEJ-EX71", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" }, { "email": "kasen@berkeley.edu", "id": "Kasen-D", "name": { "family": "Kasen", "given": "Daniel" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "email": "srk@astro.caltech.edus", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "kasen@berkeley.edu", "id": "Kasen-D", "name": { "family": "Kasen", "given": "Daniel" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-04-20", "gradofc_approval_date": "2018-11-27", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2019", "author_list": "Kleiser, Io K." }, { "id": "/id/eprint/11507", "eprint_id": 11507, "rev_number": 29, "documents": [ { "id": "/id/document/98477", "doc_id": 98477, "rev_number": 4, "files": [ { "id": "/id/file/283615", "fileid": 283615, "datasetid": "document", "objectid": 98477, "filename": "Okounkova_Thesis_2019.pdf", "mime_type": "application/pdf", "hash": "48ac457abd3acd9ff8baed90eb15e49c", "hash_type": "MD5", "filesize": 6682017, "mtime": "2019-05-10 23:20:04", "url": "/11507/1/Okounkova_Thesis_2019.pdf" } ], "eprint_id": 11507, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Okounkova_Thesis_2019.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/98477" } ] } } ], "eprint_status": "archive", "userid": 11793, "dir": "disk0/00/01/15/07", "datestamp": "2019-05-14 21:54:58", "lastmod": "2021-10-26 18:05:51", "status_changed": "2019-05-14 21:54:58", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "m.okounkova@gmail.com", "id": "Okounkova-Maria", "name": { "family": "Okounkova", "given": "Maria" }, "orcid": "0000-0001-7869-5496", "show_email": "YES" } ] }, "title": "Numerical Relativity Beyond General Relativity", "ispublished": "unpub", "full_text_status": "public", "keywords": "General relativity, numerical relativity, gravitational waves", "abstract": "Einstein\u2019s theory of general relativity has passed all precision tests to date. At some length scale, however, general relativity (GR) must break down and be reconciled with quantum mechanics in a quantum theory of gravity (a beyond-GR theory). Binary black hole mergers probe the non-linear, highly dynamical regime of gravity, and gravitational waves from these systems may contain signatures of such a theory. In this thesis, we seek to make gravitational wave predictions for binary black hole mergers in a beyond-GR theory. These predictions can then be used to perform model-dependent tests of GR with gravitational wave detections.
\r\n\r\nWe make predictions using numerical relativity, the practice of precisely numerically solving the equations governing spacetime. This allows us to probe the behavior of a binary black hole system through full inspiral, merger, and ringdown. We choose to work in dynamical Chern-Simons gravity (dCS), a higher-curvature beyond-GR effective field theory that couples spacetime curvature to a scalar field, and has motivations in string theory and loop quantum gravity. In order to obtain a well-posed initial value formalism, we perturb this theory around GR. We compute the leading-order behavior of the dCS scalar field in a binary black hole merger, as well as the leading-order dCS correction to the spacetime metric and hence gravitational radiation. We produce the first numerical relativity beyond-GR waveforms in a higher-curvature theory of gravity.
\r\n\r\nThis thesis contains additional results, all of which harness the power of numerical relativity to test GR. We compute black hole shadows in dCS gravity, numerically prove the leading-order stability of rotating black holes in dCS gravity, and lay out a formalism for determining the start time of binary black hole ringdown using information from the strong-field region of a binary black hole simulation.
\r\n", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05102019-160621419", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05102019-160621419", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "arxiv", "url": "https://arxiv.org/abs/1705.07924" }, { "description": "Article adapted for Chapter 3.", "type": "arxiv", "url": "https://arxiv.org/abs/1810.05306" }, { "description": "Article adapted for Chapter 4.", "type": "arxiv", "url": "https://arxiv.org/abs/1811.10713" }, { "description": "Article adapted for Chapter 7.", "type": "arxiv", "url": "https://arxiv.org/abs/1711.00926" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Maria Okounkova", "deposited_on": "2019-05-14 21:54:58", "doi": "10.7907/WPAT-PS25", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "saul@caltech.edu", "id": "Teukolsky-Saul-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "chair" }, { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "member" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" }, { "email": "rana@caltech.edu", "id": "Adhikari-R", "name": { "family": "Adhikari", "given": "Rana" }, "orcid": "0000-0002-5731-5076", "role": "member" }, { "email": "gukov@theory.caltech.edu", "id": "Gukov-S", "name": { "family": "Gukov", "given": "Sergei" }, "orcid": "0000-0002-9486-1762", "role": "member" }, { "email": "saul@caltech.edu", "id": "Teukolsky-Saul-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-01", "gradofc_approval_date": "2019-05-14", "thesis_awards": "John Stager Stemple Memorial Prize in Physics, 2018.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"/id/document/100526" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/100526" } ] } } ], "eprint_status": "archive", "userid": 11945, "dir": "disk0/00/01/15/17", "datestamp": "2019-06-04 22:49:04", "lastmod": "2020-03-10 20:20:43", "status_changed": "2019-06-04 22:49:04", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "matt.orr.usc@gmail.com", "id": "Orr-Matthew-Edward", "name": { "family": "Orr", "given": "Matthew Edward" }, "orcid": "0000-0003-1053-3081", "show_email": "YES" } ] }, "title": "Spatially Resolved Star Formation in Cosmological Zoom-in Simulations: Understanding the Role of Feedback in Scaling Relations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Galaxies: ISM, formation, evolution, star formation, high-redshift, structure, kinematics and dynamics, ISM: kinematics and dynamics, instabilities, opacity", "abstract": "To understand the night sky is to understand how galaxies form their stars. Cosmological zoom-in simulations, which self-consistently evolve a small number of galaxies at very high resolution by embedding them within a fully cosmological box, have evolved over the last 25 years to a level of realism where they can begin to tackle questions of spatially resolved star formation within galaxies. Whereas a decade ago simulations faced difficulty in matching even global properties of observed galaxies (e.g., the ratio of stellar mass to total halo mass), the state of the art is now able to meaningfully recover resolved quantities in galaxies that were not put into the simulations by hand (e.g., the Kennicutt-Schmidt star formation scaling relation).
\r\n\r\nThe research presented in this thesis seeks to understand how the physics of star formation and stellar feedback from massive stars shape and regulate the interstellar medium (ISM) within galaxies. Particularly, the focus lies on the scale of the largest coherent structures in galaxies -- the disk scale height. To explore these physics, the cosmological zoom-in simulations of the Feedback in Realistic Environments (FIRE) project (Hopkins et al. 2014, 2018) are used.
\r\n\r\nThe chapters of this thesis explore various topics in spatially resolved star formation, including: the Kennicutt-Schmidt relation (Schmidt 1959, Kennicutt 1998), an empirical relation between gas surface density and star formation rates, in the FIRE-1 simulations (Orr et al. 2018), including an examination what set the extent of the star-forming disks in the simulations (i.e., what causes star formation to fire up in the outskirts); an examination of the observational method of analyzing stacks of galaxy observations, finding that temporal variations in spatially resolved star formation rates within individual galaxies were more than enough to bias stacking analysis of star formation rate profiles; a semi-analytic model of non-equilibrium star formation rates, relating to the competition between the feedback timescale associated with star formation and local dynamical times (Orr et al. 2019), which explores this as a source of scatter in the Kennicutt-Schmidt relation; and finally, investigating how gas velocity dispersions and star formation rates relate in FIRE-2 Milky Way-mass disk galaxies, exploring whether or not feedback is primarily driving the velocity dispersions in galaxies, and how quickly local patches can self-regulate with star formation (Orr et al. in prep.).
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05142019-152545186", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05142019-152545186", "related_url": { "items": [ { "description": "Published version of Chapter 2.", "type": "doi", "url": "http://doi.org/10.1093/mnras/sty1241" }, { "description": "Published version of Chapter 3.", "type": "doi", "url": "http://doi.org/10.3847/2041-8213/aa8f93" }, { "description": "Published version of Chapter 4.", "type": "doi", "url": "http://doi.org/10.1093/mnras/stz1156" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "1144469" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Matthew Orr", "deposited_on": "2019-06-04 22:49:04", "doi": "10.7907/WE1D-5586", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "nzs@caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "chair" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "email": "lee@ipac.caltech.edu", "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-28", "gradofc_approval_date": "2019-06-04", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"eprint_status": "archive", "userid": 11888, "dir": "disk0/00/01/15/44", "datestamp": "2019-05-31 21:56:48", "lastmod": "2022-11-08 00:22:35", "status_changed": "2022-11-08 00:22:35", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "vijay.varma392@gmail.com", "id": "Varma-Vadapalli-Vijay-S", "name": { "family": "Varma", "given": "Vadapalli Vijay S." }, "orcid": "0000-0002-9994-1761", "show_email": "YES" } ] }, "title": "Black Hole Simulations: From Supercomputers to Your Laptop", "ispublished": "unpub", "full_text_status": "public", "keywords": "gravitational waves; numerical relativity; surrogate models; LIGO.", "abstract": "In this thesis, I will present various advancements in the modeling of binary black holes (BBHs): two black holes (BHs) that are in orbit around each other. The BHs lose energy to gravitational waves, causing them to spiral towards each other until they eventually merge and leave behind a single BH. BBHs are primary sources for ground based detectors such as the Laser Interferometer Gravitational-Wave Observatory (LIGO).
\r\n\r\nAs the BHs are about to merge, they are moving at about half the speed of light and the spacetime is highly dynamical. All analytical methods break down at this stage, and numerical relativity (NR) simulations of the full Einstein\u2019s equations are necessary. These simulations, however, are very expensive, with each simulation taking a month on a supercomputer. For direct data analysis applications with LIGO, we need a model that can be evaluated in a fraction of a second. Therefore, several approximate but fast models that are calibrated to NR simulations have been developed over the years.
\r\n\r\nSurrogate modeling provides a more powerful alternative: trained directly against the NR simulations without added assumptions, these models can reproduce the simulations as accurately as the simulations themselves, while taking only a fraction of a second to evaluate on a laptop. In short, surrogate models take BBH NR simulations from supercomputers to your laptop, without a loss of accuracy.
\r\n\r\nIn this thesis, I will present several state-of-the-art surrogate models including (i) the first NR based surrogate model to span the full range of frequencies for ground based detectors, (ii) the first surrogate model for the mass, spin, and kick velocity of the final black hole after merger, and (iii) extension of an existing precessing surrogate model to higher mass ratios. In addition, I will present some work in improving the BBH initial data used in NR simulations, as well as in understanding the systematic biases introduced by approximate waveform models in LIGO data analysis.
\r\n\r\nAs we head into the imminent era of high-precision gravitational wave astronomy, accurate yet fast models such as surrogate models will play a crucial role in maximizing the science output of our detectors.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05252019-040137906", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05252019-040137906", "related_url": { "items": [ { "description": "Chapter 2", "type": "pub", "url": "https://journals.aps.org/prd/abstract/10.1103/PhysRevD.98.084032" }, { "description": "Chapter 3", "type": "pub", "url": "https://journals.aps.org/prd/abstract/10.1103/PhysRevD.98.104011" }, { "description": "Chapter 4", "type": "pub", "url": "https://journals.aps.org/prd/abstract/10.1103/PhysRevD.96.124024" }, { "description": "Chapter 5", "type": "pub", "url": "https://journals.aps.org/prd/abstract/10.1103/PhysRevD.99.064045" }, { "description": "Chapter 6", "type": "pub", "url": "https://journals.aps.org/prl/abstract/10.1103/PhysRevLett.122.011101" }, { "description": "Chapter 7", "type": "arxiv", "url": "https://arxiv.org/abs/1905.09300" }, { "description": "Chapter 8", "type": "pub", "url": "https://iopscience.iop.org/article/10.1088/1361-6382/ab0ee9/meta" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY\u2013170212" }, { "agency": "NSF", "grant_number": "PHY\u20131708213" }, { "agency": "Sherman Fairchild Foundation" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Vadapalli Vijay Varma", "deposited_on": "2019-05-31 21:56:48", "doi": "10.7907/YT07-Q639", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "advisor" }, { "email": "yanbei.chen@gmail.com", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "saul@caltech.edu", "id": "Teukolsky-Saul-A", "name": { "family": "Teukolsky", "given": "Saul A." }, "orcid": "0000-0001-9765-4526", "role": "chair" }, { "email": "ajw@ligo.caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" }, { "email": "wise@caltech.edu", "id": "Wise-M-B", "name": { "family": "Wise", "given": "Mark B." }, "orcid": "0000-0002-9125-801X", "role": "member" }, { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "member" }, { "email": "yanbei.chen@gmail.com", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-07", "gradofc_approval_date": "2019-05-31", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"eprint_status": "archive", "userid": 11736, "dir": "disk0/00/01/13/21", "datestamp": "2019-03-27 20:51:10", "lastmod": "2020-03-04 22:06:43", "status_changed": "2019-03-27 20:51:10", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "bassamhelou@gmail.com", "id": "Helou-Bassam-Mohamad", "name": { "family": "Helou", "given": "Bassam Mohamad" }, "orcid": "0000-0003-2760-7622", "show_email": "NO" } ] }, "title": "Testing Alternative Theories of Quantum Mechanics with Optomechanics, and Effective Modes for Gaussian Linear Optomechanics", "ispublished": "unpub", "full_text_status": "public", "keywords": "Quantum Mechanics, Optomechanics, Schroedinger-Newton theory, collapse models, non-linear quantum mechanics", "abstract": "Optomechanics has made great strides in theory and experiments over the past decade, which culminated in the first direct detection of gravitational waves in 2015 by LIGO. This thesis explores how optomechanics can be used to test fundamental physics other than the theory of general relativity. Our emphasis will be on falsifiable theories (ultimately, only experiments can decide whether a theory is correct) that address two outstanding issues in quantum mechanics: the measurement problem, and reconciling quantum mechanics with the theory of general relativity. In particular, we show that the space experiment LISA pathfinder places aggressive bounds on two objective collapse models, which are non-linear stochastic modifications of the Schroedinger equation that can resolve the measurement problem. Moreover, we show that state-of-the-art torsion pendulum experiments can test the Schroedinger-Newton theory, which is the non-relativistic limit of a non-linear theory combining quantum mechanics with a fundamentally classical spacetime.
\r\n\r\nAlong the way, we propose how to resolve two major difficulties with determining the predictions of non-linear quantum mechanics in an actual experiment. First, we cannot use the density matrix formalism in non-linear quantum mechanics and so we have to suggest and justify a particular ensemble for the thermal bath. Separating out quantum and classical fluctuations helped us propose a reasonable ensemble. Second, most researchers believe that deterministic non-linear quantum mechanics must violate the no-signaling condition. We show this isn't necessarily the case because different interpretations of quantum mechanics make different predictions in non-linear quantum mechanics. We propose an interpretation, the causal-conditional prescription, that doesn't violate causality by noticing that once we fix an initial state, the evolution of a system under many non-linear theories is equivalent to evolution under a linear Hamiltonian with feedback. The mapping allows us to leverage the tools of quantum control, and it tells us that if the non-linear parameters of a non-linear Hamiltonian respond causally (i.e. with an appropriate delay) to measurement results, then the theory can be made causal.
\r\n\r\nWe also contribute to the theory of quantum optomechanics. We introduce two new bases that one can view environment modes with. In linear optomechanics a system interacts with an infinite number of bath modes. We show that the interaction can be reduced to one with finite degrees of freedom. Moreover, at any particular time, the system is correlated with only a finite number of bath modes. We show that if we make the assumption that we can measure any commuting environment modes, then this basis allows us to understand the one-shot quantum Cramer-Rao bound in a simple way, and allows us to sweep large parameter regimes and so find promising optomechanics topologies for quantum state preparation tasks that we can then analyze without the assumption of being able to measure any observable of the environment. We also use this basis to show that when we are interested in the conditional dynamics of a test mass, we can only adiabatically eliminate a lossy cavity when we measure the optomechanical system at a slow enough rate. Finally, we develop an analytic filter for obtaining the state of a generic optomechanical system that interacts linearly with its environment and is driven by Gaussian states, and where the outgoing light is measured with a non-linear photon-counting measurement. We hope that our work will help researchers explore optomechanics topologies that make use of photon counters.
\r\n", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:12182018-142547647", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:12182018-142547647", "related_url": { "items": [ { "description": "PRD article adapted for Ch. 2", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.96.044008" }, { "description": "PRD article adapted for Ch. 3", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.95.084054" }, { "description": "arXiv article adapted for Ch. 4", "type": "arxiv", "url": "https://arxiv.org/abs/1709.06639" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Bassam Helou", "deposited_on": "2019-03-27 20:51:10", "doi": "10.7907/KJ1K-9268", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "schwab@caltech.edu", "id": "Schwab-K-C", "name": { "family": "Schwab", "given": "Keith C." }, "role": "chair" }, { "email": "opainter@caltech.edu", "id": "Painter-O-J", "name": { "family": "Painter", "given": "Oskar J." }, "role": "member" }, { "email": "haixing@star.sr.bham.ac.uk", "id": "Miao-Hiaoxing", "name": { "family": "Miao", "given": "Hiaoxing" }, "role": "member" }, { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-12-11", "gradofc_approval_date": "2019-03-27", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2019", "author_list": "Helou, Bassam Mohamad" }, { "id": "/id/eprint/11547", "eprint_id": 11547, "rev_number": 45, "documents": [ { "id": "/id/document/99220", "doc_id": 99220, "rev_number": 4, "files": [ { "id": "/id/file/285733", "fileid": 285733, "datasetid": "document", "objectid": 99220, "filename": "eastwood_michael_2019.pdf", "mime_type": "application/pdf", "hash": "229e762dd3232f929a7e58bb42847ee4", "hash_type": "MD5", "filesize": 40084935, "mtime": "2019-05-28 02:21:53", "url": "/11547/1/eastwood_michael_2019.pdf" } ], "eprint_id": 11547, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "cc_by_sa", "main": "eastwood_michael_2019.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/99220" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/99220" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/99220" } ] } } ], "eprint_status": "archive", "userid": 11965, "dir": "disk0/00/01/15/47", "datestamp": "2019-05-28 23:46:08", "lastmod": "2022-01-12 00:01:04", "status_changed": "2019-05-28 23:46:08", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "michael.w.eastwood@gmail.com", "id": "Eastwood-Michael-William", "name": { "family": "Eastwood", "given": "Michael William" }, "orcid": "0000-0002-4731-6083", "show_email": "YES" } ] }, "title": "Searching for the Cosmic Dawn with the Hyperfine Structure Transition of Hydrogen", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 dark ages, reionization, first stars, radio continuum: galaxies, radio continuum: ISM", "abstract": "The 21 cm hyperfine structure transition of neutral hydrogen promises to open a window into the first billion years of the Universe (z > 6). With the exception of rare lines of sight towards exceptionally distant and luminous galaxies, this period of the universe's history remains largely unexplored. During this time the 21 cm transition is expected to be detectable as a 10--100 mK perturbation in the thermal Cosmic Microwave Background (CMB) spectrum.
\r\n\r\nDue to the large field of view of low frequency radio telescopes (typically composed of dipole antennas) and the fact that the line of sight distance can be inferred from the measured frequency of the transition, the ultimate goal of 21 cm cosmology is to produce three dimensional tomographic maps of the 21 cm brightness temperature. In this way, the formation of the first stars and galaxies will be revealed through their influence on the neutral gas around them.
\r\n\r\nThis thesis saw the construction of the Owens Valley Radio Observatory Long Wavelength Array (OVRO-LWA), a new low frequency (27--85 MHz) radio telescope located near Bishop, California. Composed of 288 crossed-dipole antennas, the OVRO-LWA is capable of imaging the entire visible hemisphere in a single 13 s snapshot image with 8 arcmin angular resolution.
\r\n\r\nThe primary challenges faced by efforts to detect the highly redshifted 21 cm transition are seeing past the blinding glow of foreground radio emission that is five orders of magnitude brighter than the cosmological emission, and calibrating the instrument to a level where it's possible to make the separation between foreground emission and the 21 cm signal. In this thesis I will present foundational work using the OVRO-LWA to place upper limits on spatial fluctuations of the 21 cm transition during the Cosmic Dawn---the period of first star formation.
\r\n\r\nIn this thesis I present the highest angular resolution maps of the full sky below 100 MHz, and generated with a new widefield imaging technique that is specialized for drift scanning interferometers. These sky maps are a 10-fold improvement in angular resolution over existing maps at comparable frequencies, and are publicly available now for use in modeling and subtracting the contamination of foreground emission in 21 cm experiments.
\r\n\r\nUsing a 28 hr integration with the OVRO-LWA, I place to-date the most constraining upper limits on the amplitude of the 21 cm spatial power spectrum at the Cosmic Dawn, and the first limits at z > 18. Although the current constraints \u0394212 \u2272 (104mK)2 do not meaningfully restrict the parameter space of models of early star formation, they do inform the design and calibrations necessary for future measurements to push towards a detection of the high-redshift 21 cm transition. In making this measurement I demonstrate the application of a new foreground filter that accounts for the full covariance of the foreground emission, and provide an updated measurement of the foreground angular covariance. Finally, I interpret the limiting factors in this measurement and determine the instrumental calibration and characterization requirements the OVRO-LWA will need to achieve in order to make a detection of the 21 cm power spectrum of the Cosmic Dawn.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05272019-174203596", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05272019-174203596", "related_url": { "items": [ { "description": "Article adapted for Ch. 4", "type": "doi", "url": "https://doi.org/10.3847/1538-3881/aac721" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department", "Owens Valley Radio Observatory (OVRO)" ] }, "deposited_by": "Michael Eastwood", "deposited_on": "2019-05-28 23:46:08", "doi": "10.7907/DYPP-JP25", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "chair" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "tjp@astro.caltech.edu", "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "Timothy J." }, "orcid": "0000-0001-5213-6231", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-09-03", "gradofc_approval_date": "2019-05-28", "thesis_awards": "France A. C\u00f3rdova Graduate Student Fund, 2016.", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2019", "author_list": "Eastwood, Michael William" }, { "id": "/id/eprint/11535", "eprint_id": 11535, "rev_number": 34, "documents": [ { "id": "/id/document/99282", "doc_id": 99282, "rev_number": 6, "files": [ { "id": "/id/file/285976", "fileid": 285976, "datasetid": "document", "objectid": 99282, "filename": "Leethochawalit_Nicha_2019.pdf", "mime_type": "application/pdf", "hash": "6f02f20b8b669bdb1bff3bbd098e2354", "hash_type": "MD5", "filesize": 3258747, "mtime": "2019-05-29 00:04:41", "url": "/11535/1/Leethochawalit_Nicha_2019.pdf" } ], "eprint_id": 11535, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Leethochawalit_Nicha_2019.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", 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{ "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/99282" } ] } } ], "eprint_status": "archive", "userid": 11962, "dir": "disk0/00/01/15/35", "datestamp": "2019-05-31 22:04:06", "lastmod": "2019-10-04 00:25:47", "status_changed": "2019-05-31 22:04:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "nichaleet@gmail.com", "id": "Leethochawalit-Nicha", "name": { "family": "Leethochawalit", "given": "Nicha" }, "orcid": "0000-0003-4570-3159", "show_email": "NO" } ] }, "title": "Spectroscopy of Galaxies: Evolution of Escape Fractions, Metallicity Gradients and Stellar Metallicity", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy; Galaxy Evolution", "abstract": "We use spectroscopic observations to investigate galaxies from the age of reionization to the peak of star formation, and the local universe. This thesis presents three projects to better understand characteristics of galactic feedback, i.e., how it regulates galactic gas flows.
\r\n\r\nWe used deep absorption line spectroscopy to estimate the escape fractions fesc of star-forming gravitationally-lensed galaxies at z \u2243 5. The approach is to measure the covering fraction of neutral hydrogen in a galaxy from the amount of non-ionizing UV radiation absorbed by low-ionization metal species. With the boost of signal by gravitational lensing, we observed four 4 < z < 5 star-forming galaxies with DEIMOS, doubling the sample size of existing observations at the redshift range. We found that the escape fractions across our sample varies from galaxy to galaxy and appear to have no significant evolution over time. We inferred a median absolute escape fraction of Lyman continuum photons of 19 \u00b1 6%. Accounting for possible biases and uncertainties, the absolute escape fraction could be reduced to no less than fesc,abs ~ 11%. Moreover, we spatially resolved and detected variation of escape fraction within a galaxy for the first time. The significant variations within the galaxy suggest that the escape fraction is governed by small-scale structure. We found a tentative anti-correlation between the star-formation rate (local or integrated) and the inferred escape fraction. This supports that the escape fraction is associated with the delay time after an episode of star formation. Feedback seems to be more effective in governing both a low SFR and a smaller HI covering fraction.
\r\n\r\nSpatially resolved spectroscopic observations of galaxies at the peak era of star-formation activities are effective in providing insight into the primitive disks. Specifically, we used metallicity gradients to provide constraints on the amount and extent of feedback produced in star-forming galaxies. We observed 15 star-forming galaxies at z ~ 2 with OSIRIS to obtain their kinematic properties and gas-phase metallicity gradients. With helps from AO correction and gravitational lensing, the typical spatial resolution in our study is less than a half-light radius of a typical L* galaxies at z \u2243 2. Combining with the sample in Jones et al., 2013, we approximately tripled the existing metallicity gradient measurements. We found a lower fraction of rotationally-supported systems than reported from larger kinematic surveys with coarser spatial resolution, which might be partially due to a our improved spatial resolution. We demonstrated that a high spatial resolution is crucial for an accurate diagnosis of the kinematic properties and dynamical maturity of z \u2243 2 galaxies.
\r\n\r\nAs for metallicity gradients, we found a much higher fraction of z \u2243 2 galaxies having weak or flat metallicity gradients than in previous studies. We correlated the metallicity gradient with the total metallicity and found that all galaxies with low total metallicities have flat gradients (< 0.1 dex per kpc-1). For galaxies with high metallicities ([N II]/H\u03b1 > 0.1), there is a divergence between isolated or rotationally-supported and dynamically-immature systems with the latter showing zero gradients irrespective of the integrated metallicity. The results indicate that relatively strong feedback (e.g. high mass loading factors or high SN energy output) is required in order to explain the majority of the observed flat gradients.
\r\n\r\nIn the second part of the thesis, we observed quiescent galaxies at z < 1 and archaeologically constrained galactic feedback via its cumulative influence on stellar metallicities. First, we present the stellar mass-[Fe/H] relationship in the Cl0024+17 galaxy cluster at z ~ 0.4. We derived the metalliticies via full spectrum stellar population synthesis modeling of individual quiescent galaxies. Our results provide the metallicities of the lowest galaxy mass (M* = 109.7M\u2299) at which individual stellar metallicity has been measured beyond the local universe. We found that the mass-[Fe/H] relationship evolves with the redshift at which the galaxy is observed today. Furthermore, we found an even stronger evolution of the mass-[Fe/H] relation with the time at which the galaxy formed (rather than the time at which it is observed). Galaxies that formed earlier have lower Fe abundance than galaxies that formed later.
\r\n\r\nLastly, we measured magnesium (Mg) abundances and extended the observed redshift to z ~ 0.55. We found that while the mass-[Fe/H] relation evolves significantly over the observed redshift range, the mass-[Mg/H] relation does not. This is due to the shorter star formation histories of quiescent galaxies at higher redshifts. Fe is mainly produced in Type Ia SN. It has a longer recycling time than Mg, which is mainly produced in core-collapse SN. Using core-collapse SN elements as a metal indicator lessens the complication of delayed recycling time and allows us to effectively use galactic chemical models with instantaneous recycling to quantify average outflows that these galaxies experience over their lifetime. We found that the average mass-loading factor \u03b7 is a power-law function of galaxy stellar mass, \u03b7 \u221d M*-0.21\u00b10.09, consistent with the results of other observational methods and with the predictions where outflow is caused by star formation feedback in turbulent disks.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05232019-145750803", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05232019-145750803", "related_url": { "items": [ { "description": "Published content for Chapter 2.", "type": "doi", "url": "https://doi.org/10.3847/0004-637X/831/2/152" }, { "description": "Published content for Chapter 3.", "type": "doi", "url": "https://doi.org/10.3847/0004-637X/820/2/84" }, { "description": "Published content for Chapter 4.", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/aab26a" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Nicha Leethochawalit", "deposited_on": "2019-05-31 22:04:06", "doi": "10.7907/2GMR-3315", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "enk@astro.caltech.edu", "id": "Kirby-Evan-N", "name": { "family": "Kirby", "given": "Evan N." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "role": "member" }, { "email": "richard.ellis@ucl.ac.uk", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "co-chair" }, { "email": "ccs@astro.caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "member" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "role": "co-chair" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-15", "gradofc_approval_date": "2019-05-31", "thesis_awards": "France A. C\u00f3rdova Graduate Student Fund, 2018.", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/99344" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/99344" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/99344" } ] } } ], "eprint_status": "archive", "userid": 11957, "dir": "disk0/00/01/15/28", "datestamp": "2019-05-31 19:06:06", "lastmod": "2022-12-02 20:01:18", "status_changed": "2019-05-31 19:06:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "marinmallory@gmail.com", "id": "Anderson-Marin-Mallory", "name": { "family": "Anderson", "given": "Marin Mallory" }, "orcid": "0000-0003-2238-2698", "show_email": "NO" } ] }, "title": "Adventures Through Time and Phase Space: Characterizing the Dynamic Radio Sky, From MHz to GHz, From Seconds to Years", "ispublished": "unpub", "full_text_status": "public", "keywords": "radio astronomy, radio transients, time domain astronomy", "abstract": "Time domain radio astronomy is on the cusp of a revolution. This is particularly true at low radio frequencies, where wide-field arrays are conducting deeper surveys than ever before, in pursuit of elusive transient phenomena. This thesis has opened an unprecedented window on the dynamic radio sky, spanning a wide range in frequency -- from MHz to GHz -- and a wide range of phenomena -- from searches for coherent radio bursts indicative of coronal mass ejections from nearby stars, to the detection of incoherent synchrotron emission from an outflow associated with the tidal disruption of a star by a supermassive black hole at the center of a galaxy.
\r\n\r\nA significant part of this work has involved the building of the Owens Valley Radio Observatory Long Wavelength Array (OVRO-LWA), a uniquely powerful radio telescope, with the ability to image the entire viewable sky at a 10 second cadence and across nearly 60 MHz of bandwidth. With the OVRO-LWA, I have developed the methods and techniques necessary for pushing further into unexplored regions of radio transient phase space, in the pursuit of sources of radio emission that provide unique insight into various astrophysical phenomena. This includes the follow-up of gravitational wave events in order to search for the signatures of prompt, coherent radio emission associated with compact object mergers, as well as targeted searches for stellar and exoplanetary radio emission as a means of better understanding planetary habitability.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05222019-125805458", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05222019-125805458", "related_url": { "items": [ { "description": "Paper contained in Chapter 3 of thesis.", "type": "doi", "url": "https://doi.org/10.3847/1538-4357/aad2d7" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1745301" }, { "agency": "Rose Hills Foundation" }, { "agency": "NSF CAREER Award", "grant_number": "1654815" }, { "agency": "NSF", "grant_number": "1555629" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Marin Anderson", "deposited_on": "2019-05-31 19:06:06", "doi": "10.7907/D28A-YQ77", "alt_title": { "items": [ "Characterizing the Dynamic Radio Sky, From MHz to GHz, From Seconds to Years" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mansi@astro.caltech.edu", "id": "Kasliwal-Mansi-M", "name": { "family": "Kasliwal", "given": "Mansi M." }, "orcid": "0000-0002-5619-4938", "role": "chair" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-07", "gradofc_approval_date": "2019-05-31", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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The first part of the thesis concerns optimization of a CCD camera as a whole. CCDs for the WaSP imager at the Hale telescope are characterized using a minimal amount of data using just a flat-field illumination source. By measuring performance over the entire parameter space of (clock and bias) inputs and analyzing the multidimensional output (linearity, dynamic range, read noise etc), optimal operating conditions can be selected quickly (and possibly automatically). With ever growing sizes of detector arrays such as the recently launched Gaia mission, the upcoming Euclid mission and ground-based cameras such as the LSST (189 CCDs), the task of streamlining detector optimization will be increasingly important. In the second (larger) part, the optimization of Charge Transfer Efficiency (CTE) is explored in particular. In modern CCDs, CTE is caused by lattice defects in the bulk silicon and is significantly worsened by radiation exposure, which is unavoidable in space. As shown in the literature, just a year of exposure to high energy solar proton radiation at low earth orbit can result in CTE reducing to 0.9999 for a signal level of 10,000e- \u2014 problematic for most precision astronomical measurements. Here, CTE degrading traps are fully explored in an undamaged CCD to new levels of accuracy. Several unique species are identified, and their population statistics are analyzed by both wafer and sub-pixel location. Subsequently, easily applied CTE measurement techniques are presented, yielding results with new levels of accuracy, concluding in the presentation of a new trap mitigating readout clocking scheme. This scheme can be readily applied to any CCD employing a parallel transfer gate without readout speed penalty. It is proposed that the results herein may be used to construct a simple model to predict CTE given a temperature, readout timing and signal level. This model could then be used to automatically optimize CTE for any CCD, given only its trap parameter statistics.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05302019-172558320", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302019-172558320", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department", "GALCIT" ] }, "deposited_by": "Pavaman Bilgi", "deposited_on": "2019-06-03 19:36:09", "doi": "10.7907/CNKG-8Y84", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" }, { "email": "sergiop@caltech.edu", "id": "Pellegrino-S", "name": { "family": "Pellegrino", "given": "Sergio" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "dim@caltech.edu", "id": "Meiron-D-I", "name": { "family": "Meiron", "given": "Daniel I." }, "role": "chair" }, { "email": "rsmith@astro.caltech.edu", "id": "Smith-Roger-M", "name": { "family": "Smith", "given": "Roger M." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "sergiop@caltech.edu", "id": "Pellegrino-S", "name": { "family": "Pellegrino", "given": "Sergio" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-04-10", "gradofc_approval_date": "2019-06-03", "review_status": "approved", "option_major": { "items": [ "aeronautics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2019", "author_list": "Bilgi, Pavaman" }, { "id": "/id/eprint/11587", "eprint_id": 11587, "rev_number": 34, "documents": [ { "id": "/id/document/100393", "doc_id": 100393, "rev_number": 4, "files": [ { "id": "/id/file/288849", "fileid": 288849, "datasetid": "document", "objectid": 100393, "filename": "schmitz_denise_thesis_2019.pdf", "mime_type": "application/pdf", "hash": "63e7083a856cae49126b4095c3882a37", "hash_type": "MD5", "filesize": 899652, "mtime": "2019-06-03 22:10:16", "url": "/11587/1/schmitz_denise_thesis_2019.pdf" } ], "eprint_id": 11587, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "schmitz_denise_thesis_2019.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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"0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/132244", "doc_id": 132244, "rev_number": 1, "files": [ { "id": "/id/file/377689", "fileid": 377689, "datasetid": "document", "objectid": 132244, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "c302fb4a0c4f00842218addac92e8942", "hash_type": "MD5", "filesize": 19190, "mtime": "2021-06-24 18:43:49", "url": "/11587/7/indexcodes.txt" } ], "eprint_id": 11587, "pos": 7, "placement": 7, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/100393" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/100393" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/100393" } ] } } ], "eprint_status": "archive", "userid": 11979, "dir": "disk0/00/01/15/87", "datestamp": "2019-06-05 20:29:46", "lastmod": "2022-12-02 19:57:01", "status_changed": "2019-06-05 20:29:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "deniseschmitz42@gmail.com", "id": "Schmitz-Denise-Marie", "name": { "family": "Schmitz", "given": "Denise Marie" }, "orcid": "0000-0001-6297-9312", "show_email": "NO" } ] }, "title": "A Perturbative Model for the Intrinsic Alignments of Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy, astrophysics, cosmology, galaxy formation, galaxy evolution, large-scale structure, perturbation theory", "abstract": "Intrinsic alignments (IA), correlations between the intrinsic shapes and orientations of galaxies on the sky, are both a significant systematic in weak lensing and a probe of the effect of large-scale structure on galactic structure and angular momentum. In the era of precision cosmology, it is thus especially important to model IA with high accuracy.
\r\n\r\nEfforts to use cosmological perturbation theory to model the dependence of IA on the large-scale structure have thus far been relatively successful. However, extant models have not been made fully self-consistent to arbitrary order in perturbation theory and do not consistently account for time evolution. In particular, advection of galaxies due to peculiar velocities alters the impact of IA, because galaxy positions when observed are generally different from their positions at the epoch when IA is believed to be set.
\r\n\r\nIn this work, we evolve the galaxy IA from the time of galaxy formation to the time at which they are observed, including the effects of this advection, and show how this process naturally leads to a dependence of IA on the velocity shear. We then incorporate this time evolution into a fully self-consistent perturbative formalism for a passively evolving IA model. We demonstrate this formalism first at second order as a proof of concept, then at third order for application to observationally relevant two-point correlations at one-loop order.
\r\n\r\nWe also discuss the implications of the time-evolved IA model for systematic errors in weak lensing as well as for studies of galaxy formation and evolution. We find that considering advection introduces nonlocality into the bispectrum, and that the degree of nonlocality represents the memory of a galaxy's path from the time of its formation to the time of observation. We discuss how this result can be used to constrain the redshift at which IA is determined and provide Fisher estimation for the relevant measurements using the example of SDSS-BOSS.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05312019-144001688", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05312019-144001688", "related_url": { "items": [ { "description": "Adapted for chapters 2-4", "type": "doi", "url": "https://doi.org/10.1088/1475-7516/2018/07/030" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "2015192719" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Denise Schmitz", "deposited_on": "2019-06-05 20:29:46", "doi": "10.7907/HZ7G-1048", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "chair" }, { "email": "hirata.10@osu.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "member" }, { "email": "odore@caltech.edu", "id": "Dor\u00e9-Olivier-P", "name": { "family": "Dor\u00e9", "given": "Olivier P." }, "orcid": "0000-0001-7432-2932", "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-09", "gradofc_approval_date": "2019-06-05", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2019", "author_list": "Schmitz, Denise Marie" }, { "id": "/id/eprint/11518", "eprint_id": 11518, "rev_number": 46, "documents": [ { "id": "/id/document/100733", "doc_id": 100733, "rev_number": 4, "files": [ { "id": "/id/file/289778", "fileid": 289778, "datasetid": "document", "objectid": 100733, "filename": "Final_Caltech_Thesis_Kung-Yi_Su.pdf", "mime_type": "application/pdf", "hash": "4025820638b075c763f4f1bf8aff536d", "hash_type": "MD5", "filesize": 13734372, "mtime": "2019-06-06 09:47:04", "url": "/11518/1/Final_Caltech_Thesis_Kung-Yi_Su.pdf" } ], "eprint_id": 11518, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Final_Caltech_Thesis_Kung-Yi_Su.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", 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"uri": "/id/document/100733" } ] } } ], "eprint_status": "archive", "userid": 10914, "dir": "disk0/00/01/15/18", "datestamp": "2019-06-07 22:16:38", "lastmod": "2020-03-10 20:21:07", "status_changed": "2019-06-07 22:16:38", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kungyisu@gmail.com", "id": "Su-Kung-Yi", "name": { "family": "Su", "given": "Kung-Yi" }, "orcid": "0000-0003-1598-0083", "show_email": "YES" } ] }, "title": "Stellar Feedback, AGN Feedback and Fluid Microphysics in Galaxy Evolution", "ispublished": "unpub", "full_text_status": "public", "keywords": "MHD; conduction; cosmic rays; turbulence; Galaxy: evolution; ISM: jets and outflows, ISM: structure; galaxies: clusters: intra-cluster medium; X-rays: galaxies: clusters", "abstract": "Understanding how the baryonic physics affects the formation and evolution of galaxies is one of the most critical questions in modern astronomy. Significant progress in understanding stellar feedback and modeling them explicitly in simulations have made it possible to reproduce a wide range of observed galaxy properties. However, there are still various pieces of missing physics and uncertainties in galaxies of different mass range.
\r\n\r\nIn this thesis, I will explore these missing pieces in baryonic physics on top of the Feedback in Realistic Environments (FIRE) stellar feedback in the cosmological hydrodynamic zoom-in simulations (FIRE-2 suite) and isolated galaxy simulations. These high-resolution simulations with FIRE physics capture multi-phase realistic interstellar medium (ISM) with gas cooling down to 10K, and star formations in dense clumps in giant molecular clouds. They are, therefore, an ideal tool for investigating the missing pieces in baryonic physics.
\r\n\r\nIn the first part of the thesis, Chapter 2, I will focus on the discrete effects of stellar feedback like individual supernovae, hypernovae, and initial mass function (IMF) sampling in dwarfs (109-1010 M\u2299). These discrete processes of stellar feedback can have maximum effects on the small galaxies without being averaged out. I will show that the discretization of supernovae (SNe) is absolutely necessary, while the effects from IMF sampling and hypernovae (HNe) is not apparent, due to the strong clustering nature of star formation.
\r\n\r\nIn the second part of the thesis, Chapter 3-4, I will focus on fluid microphysics, exploring their effects on galaxy properties and their interplay with stellar feedback in sub-L* galaxies. I will demonstrate that, once the stellar feedback is explicitly implemented as FIRE stellar feedback model, fluid microphysics such as magnetic fields, conduction, and viscosity only have minor effects on the galaxy properties like star formation rate (SFR), phase structure, or outflows. Stellar feedback also strongly alters the amplifications and morphology of the magnetic fields, resulting in much more randomly-oriented field lines. However, despite the stellar feedback, the amplification of magnetic fields in ISM gas is primarily dominated by flux-freezing compression.
\r\n\r\nIn the final part of my thesis, I focus on the massive cluster ellipticals of 1012-1014 M\u2299, where the physical mechanisms that regulate the observation-inferred cooling flows are highly uncertain -- the classic \"cooling flow problem\". I showed that solutions in the literature not associated with an active galactic nucleus (AGN), including stellar feedback, the cosmic ray from stellar feedback, magnetic fields, conduction, and morphological quenching, cannot possibly quench the galaxies, mostly because of the insufficient energy and the limited size of the affected region. After ruling out the non-AGN feedback solutions to the cooling flow problem, I will go into the most accessible, and perhaps promising solution: \"AGN feedback\", exploring the generic classes of AGN feedback models proposed in the literature. I am going to show that enhancing turbulence and injecting cosmic ray are probably the most important aspects of AGN feedback in galaxy quenching. Since they provide non-thermal pressure support that stably suppresses the core density, they can stably reduce the cooling flows without overheating the galactic cores.
", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:05142019-161824896", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05142019-161824896", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1093/mnras/sty1928" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1093/mnras/stx1463" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1093/mnrasl/slx172" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "https://doi.org/10.1093/mnras/stz1494" }, { "description": "Article adapted for Chapter 6.", "type": "arxiv", "url": "https://arxiv.org/abs/1812.03997" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Kung Yi Su", "deposited_on": "2019-06-07 22:16:38", "doi": "10.7907/RQG9-NT50", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2019-05-23", "gradofc_approval_date": "2019-06-07", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/82661" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/82661" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/82661" } ] } } ], "eprint_status": "archive", "userid": 11351, "dir": "disk0/00/01/04/35", "datestamp": "2017-09-25 22:37:35", "lastmod": "2023-05-30 22:14:27", "status_changed": "2017-09-25 22:37:35", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "trevorjdavid@gmail.com", "id": "David-Trevor-Justin", "name": { "family": "David", "given": "Trevor Justin" }, "orcid": "0000-0001-6534-6246", "show_email": "NO" } ] }, "title": "On the Evolutionary Pathways of Stars and Extrasolar Planets", "ispublished": "unpub", "full_text_status": "public", "keywords": "Stellar astrophysics; stellar ages; stellar clusters; eclipsing binaries; extrasolar planets; planet formation; planet migration", "abstract": "In this thesis, I present several studies aimed at determining the evolutionary states of stars and the planets that orbit them. Multiple approaches are undertaken to determine the physical parameters of stars over a wide range of masses, and in the process I evaluate current theoretical models which are commonly used to indirectly determine the properties of stars and planets.
\r\n\r\nChapter II concerns the ages of nearby stars more massive than the Sun. These stars, because they are bright and young (less than 1 Gyr) on the average, constitute attractive targets for surveys aiming to directly capture light from planets in wide orbits. The precise masses of directly imaged companions are important for constraining star and planet formation theories, but rely critically on the host star ages. I show that sky-projected rotational velocity is a vital parameter in age-determination for intermediate-mass stars. Rapid rotation induces large pole-to-equator gradients in the photospheric temperature and surface gravity, such that a star seen pole-on appears hotter and higher gravity (and thus younger) than a star with identical properties seen edge-on. I use intermediate-band photometry centered on the hydrogen Balmer series and projected rotational velocities to determine atmospheric parameters and ages for approximately 3500 nearby stars with masses in the range of 1-10 solar masses. I validate the method using four open clusters, in the process finding ages for α Persei and the Hyades that are younger at ~70 Myr and older at ~830 Myr, respectively, than canonical values.
\r\n\r\nIn Chapters III through V, I present orbital solutions and fundamental parameters for eclipsing binaries (EBs), newly discovered from the K2 mission, in the Pleiades open cluster (125 Myr) and the Upper Scorpius OB association (5-10 Myr). EBs, particularly those in coeval stellar populations, are valuable benchmarks for evaluating evolutionary models. Such benchmarks are particularly rare at low masses and young ages, and my work has increased the sample by 80% for stars less massive than the Sun and younger than 150 Myr. By jointly fitting eclipse observations and radial velocity measurements, one can directly determine the masses and radii of stars in an EB with percent-level precision. I use newly determined masses and radii to demonstrate a systematic temperature offset of approximately 200 K between empirical relations and model predictions. This result is in agreement with literature on the temperature suppression observed in low-mass stars, believed to be related to magnetic activity and inhibited convection. I show that stellar ages determined from the mass-radius diagram appear systematically older than those determined for the same stars in a Hertzsprung-Russell (H-R) diagram. A precise distance determination for the Pleiades EB HCG 76 is in agreement with the literature consensus and formally excludes the now discredited trigonometric measurement from Hipparcos. The orbital periods, eccentricities, and stellar spin periods determined from K2 photometry are compared with theoretical expectations from tidal dissipation. In Chapter VI, I present preliminary results on more recently discovered EBs in Upper Scorpius, and updated interpretations of previously published systems. I use the combined data to pave the way for an empirical pre-main-sequence mass-radius relation over a broad range of masses and determine an age of Upper Scorpius which is intermediate to the canonical age (3-5 Myr, as derived from low-mass pre-main-sequence stars) and a more recent estimate (9-13 Myr, as derived from intermediate-mass stars) from H-R diagram analyses.
\r\n\r\nIn Chapter VII, I present observations of the low-mass pre-main-sequence star RIK-210. This star shows a variable eclipse-like signature, which persisted through 78 days of K2 photometry but was apparently absent in archival photometry. Follow-up observations demonstrate that RIK-210 is a single star with no massive companion orbiting at the period of the eclipse-like signature. The flux diminutions are in phase with the stellar rotation, behavior seen in some young stars that are periodically obscured by an accretion disk, but RIK-210 lacks such a protoplanetary disk. I consider various explanations for the observations and favor a model in which charged dust is trapped in a rigidly-rotating magnetosphere. The source of such dust could be from one or more close-in planets or residual planet-forming material drifting in towards the star.
\r\n\r\nIn Chapter VIII I present the discovery and characterization of K2-33 b, a Neptune-sized planet closely orbiting a low-mass star in Upper Scorpius and one of the youngest exoplanets currently known. K2-33 b provides evidence that planets with substantial gaseous envelopes can be found close to their stars shortly after dispersal of the primordial protoplanetary disk. Given the planet's age (5-10 Myr), in situ formation or migration through the protoplanetary disk are the only plausible formation scenarios. K2-33 b is unusually large in size when compared to planets with similar orbital periods around low-mass field stars. I interpret this as tentative evidence that the planet is still contracting, experiencing photoevaporative atmospheric mass-loss, or both. In Chapter IX I present preliminary results from a study aimed at determining the prevalence of close-in planets at the epoch of primordial disk dispersal. Using K2 photometry for hundreds of pre-main-sequence stars in Upper Scorpius I search for transiting planets, assess survey completeness, and determine the occurrence rates or upper limits to such rates for large planets in close orbits around low-mass stars. With the singular detection of K2-33 b, I determine a rate of close-in Neptune- to Jupiter-sized planets higher than that for low-mass field stars but in closer agreement with the rate for sub-Neptune planets. Given the extreme youth of K2-33 b, I tentatively interpret these results as an indication that the planet is a progenitor of the abundant class of close-in sub-Neptunes.
\r\n\r\nConsidered collectively, my results highlight the importance of benchmark systems. Nearly all branches of astrophysics are reliant in some regard on stellar evolutionary models, but the magnitude and sense of any particular systematic offset contained in these models is often poorly understood. Eclipsing binaries and planets located in stellar clusters provide firm anchors to theoretical models aiming to predict the evolution of such objects. The need for benchmarks and model calibration is particularly acute at young ages, when stars and planets are rapidly evolving and where theoretical evolutionary models are highly uncertain. While statistical studies of large populations can yield far-reaching results that move fields forward, it is the detailed characterization of individual systems that often reveal salient clues about the inaccuracies of assumptions underlying larger scale studies. Benchmark systems, whether they are clusters, eclipsing binaries, or well-characterized planets, offer the best path forward in refining our understanding of the evolution of stars and planets.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:09132017-153137420", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09132017-153137420", "related_url": { "items": [ { "description": "Article adapted for Chapter II, \"The Ages of Early-type Stars: Stro\u0308mgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets\"", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/804/2/146" }, { "description": "Article adapted for Chapter III, \"HII 2407: An Eclipsing Binary Revealed By K2 Observations of the Pleiades\"", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/814/1/62" }, { "description": "Article adapted for Chapter IV, \"New Pleiades Eclipsing Binaries and a Hyades Transiting System Identified by K2\"", "type": "doi", "url": "http://dx.doi.org/10.3847/0004-6256/151/5/112" }, { "description": "Article adapted for Chapter V, \"K2 Discovery of Young Eclipsing Binaries in Upper Scorpius: Direct Mass and Radius Determinations for the Lowest Mass Stars and Initial Characterization of an Eclipsing Brown Dwarf Binary\"", "type": "doi", "url": "http://dx.doi.org/10.3847/0004-637X/816/1/21" }, { "description": "Article adapted for Chapter VII, \"A Transient Transit Signature Associated with the Young Star RIK-210\"", "type": "doi", "url": "http://dx.doi.org/10.3847/1538-4357/835/2/168" }, { "description": "Article adapted for Chapter VIII, \"A Neptune-sized transiting planet closely orbiting a 5-10-million-year-old star\"", "type": "doi", "url": "http://dx.doi.org/10.1038/nature18293" } ] }, "referencetext": { "items": [ "Abt, H. 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H., Schneider, A., & Song, I., 2012, ApJ, 752, 58, 58" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Foundation Graduate Research Fellowship", "grant_number": "DGE-1144469" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Trevor David", "deposited_on": "2017-09-25 22:37:35", "doi": "10.7907/Z9J67F42", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "chair" }, { "email": "kbatygin@caltech.edu", "id": "Batygin-K", "name": { "family": "Batygin", "given": "Konstantin" }, "orcid": "0000-0002-7094-7908", "role": "member" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-08-14", "gradofc_approval_date": "2017-09-25", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"abstract": "Typically, we only have access to observations that directly probe the instantaneous state of a planet. However, these instantaneous properties are often set by the long-term interplay between several aspects of the planet. I thus use quantitative models of the interactions between the orbital, interior, surface, and atmospheric evolution in the case of three planetary bodies (Mars, Pluto, and the extrasolar planet HAT-P-13b) to gain insight into the underlying physical processes that govern the evolution of planets.
\r\n\r\nIn chapter 2, the interplay between the interior structure and orbital evolution of the gas giant exoplanet HAT-P-13b allows measurements of its orbit to reveal its interior structure. I use telescopic observations of HAT-P-13b to measure its orbit and thus determine its core mass.
\r\n\r\nIn chapter 3, cell-shaped landforms on Sputnik Planitia, the surface of a vast deposit of nitrogen ice covering 5% of Pluto\u2019s surface, are the surface expression of convection within the nitrogen ice that is driven by heat flow from Pluto\u2019s interior. The cells have sublimation pits on them, with smaller pits near their centers and larger pits near their edges. Using a simple model, I calculate the sublimation rate of these pits, which allows the determination of a size-age relationship. I then use the spatial size distribution of pits on cells to calculate their convection rate, which constrains the plutonian heat flow and thus the interior properties of Pluto.
\r\n\r\nIn chapter 4, the interplay of condensation and sublimation between the surface and atmosphere of Mars create a baffling array of uniquely martian morphologies carved into the martian residual south polar CO2 cap (RSPC). Using a multi-year baseline of high-resolution observations to track the evolution of these morphologies, I build a self-consistent conceptual framework capable of explaining the basic mechanisms that give rise to the diversity of landforms that make up the RSPC.
\r\n\r\nIn chapter 5, the secular evolution of Mars' orbit drives the evolution of the equilibrium relationship between the martian atmospheric pressure and the large CO2 ice deposit on the martian south polar cap. I construct the first self-consistent conceptual framework capable of predicting the existence and form of the martian residual south polar cap and the buried CO2 deposit. I then use this framework to compute the secular pressure history of Mars.
\r\n\r\nTogether, the results of these investigations provide new perspective into the fundamental processes driving the formation and evolution of planetary bodies.
\r\n", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:05312018-155112365", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05312018-155112365", "related_url": { "items": [ { "description": "Article adapted for ch. 2", "type": "doi", "url": "http://iopscience.iop.org/article/10.3847/0004-637X/821/1/26" }, { "description": "Article adapted for ch. 3", "type": "doi", "url": "https://doi.org/10.1016/j.icarus.2017.09.018" }, { "description": "Article adapted for ch. 4", "type": "doi", "url": "https://doi.org/10.1016/j.icarus.2017.01.012" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Peter Buhler", "deposited_on": "2018-06-01 20:04:36", "doi": "10.7907/MEXZ-2586", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "co-advisor" }, { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "email": "avouac@gps.caltech.edu", "id": "Avouac-J-P", "name": { "family": "Avouac", "given": "Jean-Philippe" }, "role": "member" }, { "email": "tsai@caltech.edu", "id": "Tsai-V-C", "name": { "family": "Tsai", "given": "Victor C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-17", "gradofc_approval_date": "2018-06-01", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"userid": 11646, "dir": "disk0/00/01/10/57", "datestamp": "2018-06-12 19:59:36", "lastmod": "2020-06-02 21:44:59", "status_changed": "2018-06-12 19:59:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "meetbelinda@gmail.com", "id": "Pang-Belinda-Heyun", "name": { "family": "Pang", "given": "Belinda Heyun" }, "orcid": "0000-0002-5697-2162", "show_email": "NO" } ] }, "title": "Theoretical Foundations for Quantum Measurement in a General Relativistic Framework", "ispublished": "unpub", "full_text_status": "public", "keywords": "Quantum mechanics, quantum measurement, general relativity, quantum fields, equivalence principle, decoherence, gravitational waves, atom interferometry, matter waves, optomechanics", "abstract": "In this work, we develop theoretical formulations to analyze experimentally relevant quantum measurement schemes in a general relativistic framework, and discuss their implications versus the Newtonian or non-relativistic viewpoints. Specifically, we address (i) matter waves in simple free fall, (ii) the Mach-Zehdner atom interferometer with light-matter interaction and (iii) optomechanical systems. The motivation is to explore the regime of physics where gravity and relativistic effects become pertinent for quantum experiments due to the increase in system size and complexity. Such experiments may illuminate a way forward to reconcile the independently successful but apparently paradoxical theories of gravity and quantum mechanics, where sound theoretical foundations are necessary to help guide the search for new physics at their interface. ", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:06082018-212416022", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06082018-212416022", "related_url": { "items": [ { "description": "Article adapted for ch. 2", "type": "doi", "url": "https://doi.org/10.1103/PhysRevLett.117.090401" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Institute for Quantum Information and Matter", "Astronomy Department" ] }, "deposited_by": "Belinda Pang", "deposited_on": "2018-06-12 19:59:36", "doi": "10.7907/dfyy-y188", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@caltech.edu", "name": { "family": "Chen", "given": "Yanbei" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "rana@caltech.edu", "id": "Adhikari-R", "name": { "family": "Adhikari", "given": "Rana" }, "role": "chair" }, { "email": "wise@theory.caltech.edu", "id": "Wise-M-B", "name": { "family": "Wise", "given": "Mark B." }, "role": "member" }, { "email": "schwab@caltech.edu", "id": "Schwab-K-C", "name": { "family": "Schwab", "given": "Keith C." }, "role": "member" }, { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-29", "gradofc_approval_date": "2018-06-12", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/91284" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/91284" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/91284" } ] } } ], "eprint_status": "archive", "userid": 11291, "dir": "disk0/00/01/04/23", "datestamp": "2017-09-18 23:24:47", "lastmod": "2023-05-30 22:22:28", "status_changed": "2017-09-18 23:24:47", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "allison.strom@gmail.com", "id": "Strom-Allison-Leigh", "name": { "family": "Strom", "given": "Allison Leigh" }, "orcid": "0000-0001-6369-1636", "show_email": "NO" } ] }, "title": "Unveiling the Physical Conditions in Star-Forming Galaxies at the Peak of Galaxy Assembly", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: high-redshift; galaxies: interstellar medium; interstellar medium: abundances; interstellar medium: H II regions", "abstract": "Galaxies at the peak of cosmic star formation (z~2-3) exhibit significantly higher star formation rates and gas fractions at fixed stellar mass than nearby galaxies. These z~2-3 galaxies are also distinct in terms of their nebular spectra, reflecting important differences not only in the physical conditions of their interstellar medium (e.g., electron density and gas-phase metallicity), but also in the details of their massive stellar populations. Jointly observing galaxies' HII regions, at rest-UV and rest-optical wavelengths, and massive stars, at rest-UV wavelengths, is central to constructing a framework for understanding the differences between z~2-3 and z~0 star-forming galaxies and also vital for self-consistently explaining the trends observed in the high-z population.
\r\n\r\nThis thesis presents the main results from the near-infrared (NIR) component of the Keck Baryonic Structure Survey (KBSS), a targeted spectroscopic survey of z~2-3 galaxies that uniquely combines observations in the rest-UV (1000-2000\u00c5) and rest-optical (3500-7500\u00c5) bandpasses. The NIR spectroscopic campaign conducted using Keck/MOSFIRE, described in Chapter 2, includes observations over 1200 high-z galaxies and represents one of the largest samples of high-quality rest-optical spectra of z~2-3 galaxies ever assembled. These measurements offer new insights regarding the physical conditions in galaxies forming during one of the most active periods in the universe's history.
\r\n\r\nChapter 3 describes the rest-optical spectra of ~380 KBSS galaxies at z~2-2.7 and shows that the primary difference between HII regions in z~2.3 galaxies and those at z~0 is an enhancement in the degree of nebular excitation. KBSS galaxies are also 10 times more massive than z~0 galaxies with similar ionizing spectra and have higher gas-phase N and O abundances at fixed excitation. These results indicate the presence of harder ionizing radiation fields at fixed gas-phase enrichment relative to typical z~0 galaxies, consistent with Fe-poor stellar population models that include massive binaries.
\r\n\r\nChapter 4 builds on this analysis to develop a new technique for determining the physical conditions in individual high-z galaxies -- independent of diagnostics tuned to local calibration samples. This method produces self-consistent measurements of the chemical enrichment and excitation conditions in ~150 galaxies at z~2-2.7.
\r\n\r\nTogether, these results provide compelling evidence that the distinct chemical abundance patterns observed in z~2-3 star-forming galaxies result from systematic differences in their star formation histories relative to galaxies with similar stellar masses today. The thesis concludes by considering the importance of accounting for differences in galaxies' past star formation when interpreting spectroscopic observations and briefly discusses opportunities for extending the framework for analyzing high-z galaxies presented here to future studies of star-forming galaxies throughout cosmic time.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:09082017-170618214", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09082017-170618214", "related_url": { "items": [ { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "http://dx.doi.org/10.3847/1538-4357/836/2/164" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Foundation Graduate Research Fellowship" }, { "agency": "National Science Foundation", "grant_number": "AST-0908805" }, { "agency": "National Science Foundation", "grant_number": "AST-1313472" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released to public view 19 March 2018 // \r\nRestricted to Caltech community only until 11 March 2018. // From author: Work contained in thesis is being prepared for publication to a refereed journal.", "deposited_by": "Allison Strom", "deposited_on": "2017-09-18 23:24:47", "doi": "10.7907/Z9N58JJN", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" }, { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162", "role": "member" }, { "email": "bts@irastro.caltech.edu", "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-07-26", "gradofc_approval_date": "2017-09-14", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/92090" } ] } } ], "eprint_status": "archive", "userid": 11340, "dir": "disk0/00/01/10/44", "datestamp": "2018-06-12 01:06:15", "lastmod": "2020-03-10 23:04:12", "status_changed": "2018-06-12 01:06:15", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "murchikova@gmail.com", "id": "Murchikova-Elena-M", "name": { "family": "Murchikova", "given": "Elena M." }, "orcid": "0000-0001-8986-5403", "show_email": "NO" } ] }, "title": "Astrophysical Applications of Quantum Mechanics", "ispublished": "unpub", "full_text_status": "public", "keywords": "astrophysics, quantum mechanics, recombination lines, black holes, Sagittarius A*, neutrino transport, chiral fluids", "abstract": "From an outside point of view, astrophysics and quantum mechanics as subclasses of the physical sciences could not be further from each other. Yet these two sides of nature are deeply intertwined. The influence of quantum mechanics on astrophysics and astrophysics on quantum mechanics has been profound: spectral lines as diagnostics, radiative transport, the interiors of celestial bodies, neutrino oscillations, constraints on neutrino mass and graviton mass. In this work, I discuss several applications of quantum mechanics in astrophysics: (1) I examine the use of submm recombination lines of H, He and He+ to probe the extreme ultraviolet luminosity of starbursts and Active Galactic Nuclei. (2) I use the hydrogen recombination line H30\u03b1 to study the accretion zone of the Milky Way's Galactic Center black hole. I discuss detection of an accretion disk of radius <0.008 pc, consisting of ~104 K gas the disk properties, and its importance in the context of accretion on the black hole. (3) I carry out an extensive study and comparison of M1 closure schemes for neutrino radiation transport, using the protoneutron star interior as a background. (4) I study first-order hydrodynamics of a chiral fluid on a vortex background, and in an external magnetic field, as the precursor for a study of neutron star interiors. I show that there are two previously undiscovered modes describing heat waves propagating along the vortex and magnetic field.\r\n", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:06082018-000259902", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06082018-000259902", "related_url": { "items": [ { "description": "Adapted for ch. 2", "type": "arxiv", "url": "https://arxiv.org/abs/1310.0026" }, { "description": "Adapted for ch. 4", "type": "arxiv", "url": "https://arxiv.org/abs/1701.07027" }, { "description": "Adapted for ch. 5", "type": "arxiv", "url": "https://arxiv.org/abs/1609.00024" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Groce Fellowship" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Elena Murchikova", "deposited_on": "2018-06-12 01:06:15", "doi": "10.7907/PEBS-ZJ88", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "chair" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "member" }, { "email": "jfuller@caltech.edu", "id": "Fuller-James", "name": { "family": "Fuller", "given": "James" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-29", "gradofc_approval_date": "2018-06-11", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2018", "author_list": "Murchikova, Elena M." }, { "id": "/id/eprint/11056", "eprint_id": 11056, "rev_number": 38, "documents": [ { "id": "/id/document/92281", "doc_id": 92281, "rev_number": 3, "files": [ { "id": "/id/file/260259", "fileid": 260259, "datasetid": "document", "objectid": 92281, "filename": "cornell-brett-6-month-embargo-request.pdf", "mime_type": "application/pdf", "hash": "02c8c3325550ffabefedc3f07048d8b0", "hash_type": "MD5", "filesize": 77824, "mtime": "2018-06-11 16:10:00", "url": "/11056/7/cornell-brett-6-month-embargo-request.pdf" } ], "eprint_id": 11056, "pos": 7, "placement": 7, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Author Request 2018-05-26", "language": "en", "security": "internal", "license": "other", "main": "cornell-brett-6-month-embargo-request.pdf", "media_duration": 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of physics is far from complete. The \"ordinary matter\", such as electrons, protons, photons and neutrons, that constitutes the bulk of all human physical experiences is actually only a minority (about 16%) of the total mass of the universe. The remaining 84% is very poorly understood, but has profound effects on the dynamics and evolution of our universe. Because it does not interact with light, and is not observable in telescopes on earth, this extra mass is usually referred to as \"dark matter\". Although the dark matter is poorly understood, Weakly Interacting Massive Particles (WIMPs) are a well-motivated candidate that can be directly detected via a non-gravitational interaction with normal matter, potentially allowing for direct terrestrial detection and characterization of this dark matter. This dissertation is focused on this direct WIMP detection and will be broken into two main parts.
\r\n\r\nThe first part focuses on the blinded analysis of roughly three years of data collected from March 2012 to November 2015 by the SuperCDMS Soudan experiment. SuperCDMS Soudan consists of an array of 15, 0.6-kg, cryogenic, Ge iZIP particle detectors situated in a decommissioned iron mine in remote northern Minnesota. This analysis is optimized to be sensitive to theoretical WIMP masses above 10 GeV/c2. This result set the strongest limits for WIMP--germanium-nucleus interactions for WIMP masses greater than 12 Gev/c2.
\r\n\r\nThe second part focuses on the development new kind of particle detector in the style of a SuperCDMS iZIP, designed to simplify fabrication and readout, improve phonon-based position reconstruction, and help to scale to larger target arrays. These detectors replace the TES-based phonon sensors of the iZIP with Microwave Kinetic Inductance Detectors (MKIDs).
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:06082018-171453167", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06082018-171453167", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Brett Cornell", "deposited_on": "2018-06-12 22:22:19", "doi": "10.7907/M297-J716", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "chair" }, { "email": "smaria@caltech.edu", "id": "Spiropulu-M", "name": { "family": "Spiropulu", "given": "Maria" }, "orcid": "0000-0001-8172-7081", "role": "member" }, { "email": "clifford.cheung@caltech.edu", "id": "Cheung-Clifford-W", "name": { "family": "Cheung", "given": "Clifford W." }, "orcid": "0000-0002-9983-9425", "role": "member" }, { "email": "schwabkeith@protonmail.com", "id": "Schwab-K-C", "name": { "family": "Schwab", "given": "Keith C." }, "orcid": "0000-0001-8216-4815", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-30", "gradofc_approval_date": "2018-06-12", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"/id/document/91759" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/91759" } ] } } ], "eprint_status": "archive", "userid": 11540, "dir": "disk0/00/01/10/16", "datestamp": "2018-06-08 00:37:37", "lastmod": "2020-03-10 19:23:34", "status_changed": "2018-06-08 00:37:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ryan.m.monroe@gmail.com", "id": "Monroe-Ryan-McKay", "name": { "family": "Monroe", "given": "Ryan McKay" }, "orcid": "0000-0002-0026-4546", "show_email": "NO" } ] }, "title": "Gigahertz Bandwidth and Nanosecond Timescales: New Frontiers in Radio Astronomy Through Peak Performance Signal Processing", "ispublished": "unpub", "full_text_status": "public", "keywords": "Radio astronomy, radio frequency interference, FPGA, DSP, cosmic ray, self trigger", "abstract": "Abstract In the past decade, there has been a revolution in radio-astronomy signal processing. High bandwidth receivers coupled with fast ADCs have enabled the collection of tremendous instantaneous bandwidth, but streaming computational resources are struggling to catch up and serve these new capabilities. As a consequence, there is a need for novel signal processing algorithms capable of maximizing these resources. This thesis responds to the demand by presenting FPGA implementations of a Polyphase Filter Bank which are an order of magnitude more efficient than previous algorithms while exhibiting similar noise performance. These algorithms are showcased together alongside a broadband RF front-end in Starburst: a 5 GHz instantaneous bandwidth two-element interferometer, the first broadband digital sideband separating astronomical interferometer.\u00a0 Starburst technology has been applied to three instruments to date.
\r\n\r\nAbstract Wielding tremendous computational power and precisely calibrated hardware, low frequency radio telescope arrays have potential greatly exceeding their current applications.\u00a0 This thesis presents new modes for low frequency radio-telescopes, dramatically extending their original capabilities.\u00a0 A microsecond-scale time/frequency mode empowered the Owens Valley Long Wavelength Array to inspect not just the radio sky by enabling the testing of novel imaging techniques and detecting overhead beacon satellites, but also the terrestrial neighborhood, allowing for the characterization and mitigation of nearby sources of radio frequency interference (RFI).\u00a0 This characterization led to insights prompting a nanosecond-scale observing mode to be developed, opening new avenues in high energy astrophysics, specifically related to the radio frequency detection of ultra-high energy cosmic rays and neutrinos.
\r\n\r\nAbstract Measurement of the flux spectrum, composition, and origin of the highest energy cosmic ray events is a lofty goal in high energy astrophysics. One of the most powerful new windows has been the detection of associated extensive air showers at radio frequencies. However, all current ground-based systems must trigger off an expensive and insensitive external source such as particle detectors - making detection of the rare, high energy events uneconomical.\u00a0 Attempts to make a direct detection in radio-only data have been unsuccessful despite numerous efforts. The problem is even more severe in the case of radio detection of ultra-high energy neutrino events, which cannot rely on in-situ particle detectors as a triggering mechanism. This thesis combines the aforementioned nanosecond-scale observing mode with real-time, on-FPGA RFI mitigation and sophisticated offline post-processing.\u00a0 The resulting system has produced the first successful ground based detection of cosmic rays using only radio instruments. Design and measurements of cosmic ray detections are discussed, as well as recommendations for future cosmic ray experiments.\u00a0 The presented future designs allow for another order of magnitude improvement in both sensitivity and output data-rate, paving the way for the economical ground-based detection of the highest energy neutrinos.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:06042018-004220017", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06042018-004220017", "related_url": { "items": [ { "description": "Article adapted for Ch. 2.", "type": "doi", "url": "https://doi.org/10.1142/S2251171716410026" } ] }, "projects": { "items": [ "Owens Valley Long Wavelength Array", "Starburst" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1654815" }, { "agency": "NSF", "grant_number": "AST-1311098" }, { "agency": "Scialog Research Corporation", "grant_number": "23781" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Ryan Monroe", "deposited_on": "2018-06-08 00:37:37", "doi": "10.7907/25DP-J474", "alt_title": { "items": [ "New Frontiers in Radio Astronomy Through Peak Performance Signal Processing" ] }, "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "role": "chair" }, { "email": "ldaddario@caltech.edu", "id": "D'Addario-L-R", "name": { "family": "D'Addario", "given": "Larry R." }, "role": "member" }, { "email": "hassibi@caltech.edu", "id": "Hassibi-B", "name": { "family": "Hassibi", "given": "Babak" }, "role": "member" }, { "email": "charles.elachi@caltech.edu", "id": "Elachi-C", "name": { "family": "Elachi", "given": "Charles" }, "role": "member" }, { "email": "sweinreb@caltech.edu", "id": "Weinreb-S", "name": { "family": "Weinreb", "given": "Sander" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-07", "gradofc_approval_date": "2018-06-07", "thesis_awards": "Milton and Francis Clauser Doctoral Prize, 2018.", "review_status": "approved", "option_major": { "items": [ "eleceng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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11512, "dir": "disk0/00/01/07/46", "datestamp": "2018-03-13 17:10:14", "lastmod": "2022-12-02 19:48:58", "status_changed": "2018-03-13 17:10:14", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ianyuwong666@gmail.com", "id": "Wong-Ian-Yu", "name": { "family": "Wong", "given": "Ian Yu" }, "orcid": "0000-0001-9665-8429", "show_email": "YES" } ] }, "title": "Probing the Trojan-Hilda-KBO Connection: An Empirical Test of Dynamical Instability Models of Solar System Evolution", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science; Asteroids; Solar System", "abstract": "In recent decades, the paradigm of solar system formation has undergone radical change. Many current models posit that a significant reorganization of the outer Solar System occurred after the end of planet formation. Specifically, it is hypothesized that Jupiter and Saturn crossed a mutual mean motion resonance, leading to a chaotic expansion of the ice giants' orbits that disrupted the large population of planetesimals situated further out. While the majority of these bodies were ejected from the Solar System, a fraction of them were retained as the present-day Kuiper Belt, while others were scattered inward and captured into resonances with Jupiter to become the Trojans and Hildas. These dynamical instability models invariably predict that the Trojans, Hildas, and Kuiper Belt objects (KBOs) were sourced from the same primordial body of outer solar system planetesimals. Therefore, a comparative exploration of these minor body populations serves as one of the definitive observational tests of our present understanding of solar system evolution. Over the past four-and-a-half years, I have carried out a diverse series of systematic studies aimed at synthesizing a detailed picture of Trojan, Hildas, and KBOs. By combining novel analyses of archival data with new photometric surveys, I have derived the first debiased color distributions of Trojans and KBOs and expanded our knowledge of their respective size distributions. In addition, I have explored the peculiar color bimodality attested in the all three asteroid populations, which indicates the presence of two sub-populations. Utilizing the full body of observations, I have formulated the first self-consistent hypothesis outlining the formation, composition, and dynamical/chemical evolution of the primordial outer solar system planetesimals, with special attention given to explaining the color bimodality, size distribution shapes, and collisional families. My results lay the groundwork for future studies with next-generation instruments and ultimately, the Trojan flyby mission Lucy.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:03012018-170927159", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03012018-170927159", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-6256/148/6/112" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-6256/150/6/174" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "http://dx.doi.org/10.3847/0004-6256/152/4/90" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "http://dx.doi.org/10.3847/1538-3881/153/2/69" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "http://dx.doi.org/10.3847/1538-3881/aa60c3" }, { "description": "Article adapted for Chapter 7.", "type": "doi", "url": "http://dx.doi.org/10.3847/1538-3881/aa8406" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Ian Wong", "deposited_on": "2018-03-13 17:10:14", "doi": "10.7907/Z9B856BX", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "hknutso2@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "chair" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "member" }, { "email": "kbatygin@gps.caltech.edu", "id": "Batygin-K", "name": { "family": "Batygin", "given": "Konstantin" }, "orcid": "0000-0002-7094-7908", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "orcid": "0000-0002-2745-3240", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-02-20", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "abhilashmishra87@gmail.com", "id": "Mishra-Abhilash", "name": { "family": "Mishra", "given": "Abhilash" }, "orcid": "0000-0002-4424-4096", "show_email": "YES" } ] }, "title": "The Low-Frequency Frontier: Cosmology with Future 21cm Experiments", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology; Cosmic background radiation; Radio astronomy; Inflation.", "abstract": "This thesis presents theoretical and observational investigations in two areas of cosmology: the detection of inflationary gravitational waves using the circular polarization of the redshifted 21cm line from neutral hydrogen during the Dark Ages, and the study of galactic foregrounds at low-frequencies using the Owens Valley Radio Observatory Long Wavelength Array (OVRO LWA).
\r\n\r\nIn the theoretical part of this thesis, we propose a new method to measure the tensorto-scalar ratio r using the circular polarization of the 21 cm radiation from the Dark Ages. In Chapter II we discuss the basic principles of inflationary physics, which is now accepted as a standard paradigm for the generation of perturbations in the early universe. Along with density (scalar) perturbations, inflation also produces gravitational wave (tensor) modes. In Chapter IV we outline a novel, albeit futuristic method to detect inflationary gravitational waves. Our method relies on the splitting of the F = 1 hyperfine level of neutral hydrogen due to the quadrupole moment of the\r\nCMB during the Dark Ages. We show that unlike the Zeeman effect, where MF = ±1 have opposite energy shifts, the CMB quadrupole shifts MF = ±1 together relative to MF = 0. This splitting leads to a small circular polarization of the emitted 21cm photon, which is in principle observable. Further, we forecast the sensitivity of future radio experiments to measure the CMB quadrupole during the era of first cosmic light (z ~ 20). The tomographic measurement of 21 cm circular polarization allows us to construct a 3D remote quadrupole field. Measuring the B-mode component of this remote quadrupole field can be used to put bounds on the tensor-to-scalar ratio r. We make Fisher forecasts for a future Fast Fourier Transform Telescope (FFTT), consisting of an array of dipole antennas in a compact grid configuration, as a function of array size and observation time. The forecasts are dependent on the evolution of the Lyman-\u03b1 flux in the pre-reionization era, that remains observationally unconstrained. Finally, we calculate the typical order of magnitudes for circular polarization foregrounds and comment on their mitigation strategies. We conclude that detection of primordial gravitational waves with 21 cm observations is in principle possible, so long as the primordial magnetic field amplitude is small, but would require a very futuristic experiment with corresponding advances in calibration and foreground suppression techniques.
\r\n\r\nIn the observational part of this thesis, we investigate the cross-correlation between low-frequency radio maps from the Owens Valley Radio Observatory Long Wave-length Array (OVRO LWA) and tracers of the ISM: dust, H\u03b1, and HI. Our goal is to search for any anomalous radiative processes at low frequencies (20 \u2212 80 MHz). In Chapter III we discuss the basic principles of 21cm cosmology and provide an overview of current and planned 21cm experiments. Broadband foreground sources pose the greatest challenge to 21cm tomography and need to be characterized carefully before the technique becomes a sensitive probe of the dark ages and the epoch\r\nof reionization. The foregrounds are expected to be predominantly galactic and approximately four orders of magnitude larger than the cosmological signal. In Chapter V, we investigate the nature of the diffuse Galactic radio emission in the 20 \u2212 80MHz frequency range using data from the OVRO-LWA. We cross-correlate LWA maps with tracers of ISM (dust, H\u03b1, HI) from a number of surveys , to investigate galactic foregrounds relevant to detection of 21cm signal from the Dark Ages. We describe a formalism to compute the cross-power spectra between LWA maps and ISM tracers. Our results are consistent with no correlation between tracers of the gas and dust in the ISM at high Galactic latitudes (b > 55\u00b0) and low-frequency maps from the LWA, at scales \u2113 ~ 10 \u2212 600 at a 99.9% confidence level.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:09112017-150629661", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09112017-150629661", "related_url": { "items": [ { "description": "Article adapted for Ch. 4", "type": "arxiv", "url": "https://arxiv.org/abs/1707.03514" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Simons Foundation" }, { "agency": "Department of Energy " } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Abhilash Mishra", "deposited_on": "2018-04-09 23:26:42", "doi": "10.7907/Z9W37TJ2", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "hirata.10@osu.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "olivier.dore@caltech.edu", "id": "Dor\u00e9-Olivier-P", "name": { "family": "Dor\u00e9", "given": "Olivier P." }, "orcid": "0000-0001-7432-2932", "role": "member" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" }, { "email": "hirata.10@osu.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-07-21", "gradofc_approval_date": "2018-04-09", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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This dissertation focuses on integrating macroscopic and microscopic scales of measurement with regard to spectroscopy and magnetization. In the first chapter high resolution orbital spectroscopy (~18 m/px) and imagery (~30 cm/px) are used to identify potential sources for some of the sedimentary rocks investigated by the Curiosity rover and expand the accessible stratigraphy. While we find mineralogies in common outside and inside the crater as well as transport mechanisms, we conclude that additional sedimentary sources and/or modification after transport are required to explain chemical differences and that strata point to multiple episodes of a lake in Gale crater. In the third chapter we conducted a laboratory photometric study on candidate calibration target materials for the Mars-2020 rover. We characterized these target materials for proper calibration and monitoring of the Mastcam-Z instrument to enable mineral identification through reflectance spectroscopy. The fourth and fifth chapters focus on the microscopic magnetizations found within Martian meteorite ALH84001. Chapter four reports on paleomagnetic experiments conducted on isolated carbonate crystals which contain magnetite previously reported to be biogenic. We compare paleomagnetic test results which distinguish between biogenic and abiogenic origin hypotheses and find that the magnetization within the carbonates is most consistent with a shock processes. In chapter five we analyzed the distribution of dipoles within slices of ALH84001 and determined that they lie in a girdle distribution which could be interpreted as resulting from a true polar wander event on Mars. Looking at kilometer scale observations outside of Gale enlightened observations made along the rover transverse path. A high resolution laboratory analysis of calibration materials will enable future multispectral mineralogical explorations. Microscopic analyses of magnetization inform ancient surface processes on Mars and hint at large-scale global change. In each of these chapters our results were only made possible or greatly enhanced by the combination of data sources and scales.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:05242018-144308725", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05242018-144308725", "related_url": { "items": [ { "description": "Adapted for Chapter 2.", "type": "doi", "url": "http://dx.doi.org/10.1002/2016JE005163" }, { "description": "Adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1117/1.OE.58.2.027108" }, { "description": "Supporting Data Set", "type": "doi", "url": "http://dx.doi.org/10.22002/D1.1154" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "NNX15AQ95H" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Jennifer Buz", "deposited_on": "2018-05-30 18:33:34", "doi": "10.7907/Z6EH-M526", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "co-advisor" }, { "email": "kirschvink@caltech.edu", "id": "Kirschvink-J-L", "name": { "family": "Kirschvink", "given": "Joseph L." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "mpl@gps.caltech.edu", "id": "Lamb-M-P", "name": { "family": "Lamb", "given": "Michael P." }, "role": "chair" }, { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "member" }, { "email": "kirschvink@caltech.edu", "id": "Kirschvink-J-L", "name": { "family": "Kirschvink", "given": "Joseph L." }, "role": "member" }, { "email": "wfischer@caltech.edu", "id": "Fischer-W-W", "name": { "family": "Fischer", "given": "Woodward W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-04-20", "gradofc_approval_date": "2018-05-30", "review_status": "approved", "option_major": { "items": [ "geol" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/91271" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/91271" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/91271" } ] } } ], "eprint_status": "archive", "userid": 11550, "dir": "disk0/00/01/09/68", "datestamp": "2018-06-01 20:56:23", "lastmod": "2022-12-02 19:43:43", "status_changed": "2018-06-01 20:56:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "martalbryan@gmail.com", "id": "Bryan-Marta-Levesque", "name": { "family": "Bryan", "given": "Marta Levesque" }, "orcid": "0000-0002-6076-5967", "show_email": "NO" } ] }, "title": "Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Extrasolar planets, radial velocity technique, high-resolution spectroscopy, high-contrast imaging, statistical techniques", "abstract": "Over the past two decades, thousands of planets with an extraordinary diversity of properties have been discovered orbiting nearby stars. Many of these exoplanetary systems challenge our narrative for how planets form and evolve, motivating the search for observational clues to the underlying mechanisms that led to this diversity. In this quest, gas giant analogs to our own Jupiter and Saturn immediately stand out as the most visible relics of the planet formation process. They are products of their birth environment, with properties such as atmospheric and interior compositions, masses, and formation locations sculpted by protoplanetary disk and host star properties. They also actively shape their surroundings; early in their lifetimes, gas giants can alter the structure of the gas disk from which additional planetary bodies may coalesce and affect the transport of rocky and icy materials to the inner disk. After the gas has dissipated these same behemoths can push smaller planets around, causing them to migrate or even ejecting them from the system. Thus to explain the observed diversity of exoplanet systems, we must first understand how gas giant planets form and evolve. This thesis presents four studies that harness multiple observational techniques to explore this question of how gas giant planets outside our solar system form and evolve. ", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:05302018-060732719", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302018-060732719", "related_url": { "items": [ { "description": "Article adapted for ch. 2", "type": "doi", "url": "https://doi.org/10.3847/0004-637X/821/2/89" }, { "description": "Article adapted for ch. 3", "type": "doi", "url": "https://doi.org/10.3847/0004-637X/827/2/100" }, { "description": "Article adapted for ch. 4", "type": "doi", "url": "https://doi.org/10.1038/s41550-017-0325-8" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Marta Bryan", "deposited_on": "2018-06-01 20:56:23", "doi": "10.7907/XPMN-WQ35", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "hknutso2@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "chair" }, { "email": "kbatygin@gps.caltech.edu", "id": "Batygin-K", "name": { "family": "Batygin", "given": "Konstantin" }, "orcid": "0000-0002-7094-7908", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "hknutso2@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-01", "gradofc_approval_date": "2018-06-01", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2018", "author_list": "Bryan, Marta Levesque" }, { "id": "/id/eprint/10881", "eprint_id": 10881, "rev_number": 33, "documents": [ { "id": "/id/document/88639", "doc_id": 88639, "rev_number": 5, "files": [ { "id": "/id/file/251473", "fileid": 251473, "datasetid": "document", "objectid": 88639, "filename": "Guszejnov_thesis.pdf", "mime_type": "application/pdf", "hash": "28c6a7cfde0cba6d08deb2d0dd7d8aa3", "hash_type": "MD5", "filesize": 5939250, "mtime": "2018-05-14 23:05:03", "url": "/10881/1/Guszejnov_thesis.pdf" } ], "eprint_id": 10881, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis", "language": "en", "security": "public", "license": "other", "main": "Guszejnov_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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"type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/88639" } ] } } ], "eprint_status": "archive", "userid": 11601, "dir": "disk0/00/01/08/81", "datestamp": "2018-05-21 22:43:47", "lastmod": "2023-05-30 22:21:39", "status_changed": "2018-05-21 22:43:47", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "guszejnov.david@gmail.com", "id": "Guszejnov-D\u00e1vid", "name": { "family": "Guszejnov", "given": "D\u00e1vid" }, "orcid": "0000-0001-5541-3150", "show_email": "YES" } ] }, "title": "On the Origin of Scales and Scaling Laws in Star Formation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astrophysics; star formation; turbulence; IMF", "abstract": "Stars are the fundamental objects of astrophysics and their formation is a key process that influences the evolution of galaxies and planets, and the development of life. Understanding how stars form is crucial even for seemingly unconnected fields of astronomy, as the interpretation of observed starlight from galaxies (even as a background) and other unresolved sources relies on our understanding of star formation. There is no comprehensive theory of star formation, despite intense effort on both the theoretical and observational sides, due to the complicated, non-linear physics involved (e.g., magnetohydrodynamics, gravity, radiation) and the enormous dynamic range of the problem. My goal has been to identify the role different physical processes (e.g., turbulence, feedback) play in star formation.
\r\n\r\nUsing the semi-analytical framework that I developed, I found that a large number of star formation models are inherently sensitive to the initial conditions of the progenitor clouds (e.g., temperature). This led to another study where I predicted the expected variation of the initial mass function (IMF) of stars in a Milky-Way-like galaxy for different star formation models. I showed that IMF models where the peak is either set by turbulent properties or cooling physics (using an effective equation of state) are unable to reproduce the universal IMF of the Milky Way. I also utilized my semi-analytical tools to predict higher-order statistics of star formation: stellar correlation, multiplicity and the companion mass distribution for binaries. I showed that due to observational biases all explored models could roughly reproduce the observed multiplicity and companion mass distributions. This means that observations are currently unable to differentiate between most models.
\r\n\r\nWhile working on these projects I found that several scaling relations (e.g., the slopes of IMF, stellar correlation function and gas column density distribution) are insensitive to our choice of physical model; they are universal. Inspired by this I developed an analytic model that I used to show that scale-free structure formation inherently leads to these scaling relations. This provides a deep physical reason why the mass functions and correlation functions of very different systems (e.g., stars, protostellar cores, star clusters, Dark matter halos) follow roughly the same power-law relations.
\r\n\r\nMy previous findings with my semi-analytical models indicated that isothermal collapse would lead to an infinite fragmentation cascade, i.e. there is no inherent low-mass cut-off. Part of the literature supports these findings and claims that additional physics is needed to imprint a mass scale into the problem, but there are theoretical models and simulations that claim that such a cut-off exists. Using GIZMO, a fully adaptive, meshless MHD code, I have carried out a convergence study and have shown that the isothermal fragmentation cascade continues to ever smaller scales without limit.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:05142018-155029272", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05142018-155029272", "related_url": { "items": [ { "description": "Paper based on Chapter 2.", "type": "doi", "url": "https://doi.org/10.1093/mnras/stv872" }, { "description": "Paper based on Chapter 3.", "type": "doi", "url": "https://doi.org/10.1093/mnras/stw619" }, { "description": "Paper based on Chapter 4.", "type": "doi", "url": "https://doi.org/10.1093/mnras/stw315" }, { "description": "Paper based on Chapter 5.", "type": "doi", "url": "https://doi.org/10.1093/mnras/stx725" }, { "description": "Paper based on Chapter 6.", "type": "doi", "url": "https://doi.org/10.1093/mnras/stx2067" }, { "description": "Paper based on Chapter 7.", "type": "doi", "url": "https://doi.org/10.1093/mnras/sty920" }, { "description": "Paper based on Chapter 8.", "type": "arxiv", "url": "https://arxiv.org/abs/1804.08574" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "David Guszejnov", "deposited_on": "2018-05-21 22:43:47", "doi": "10.7907/WZ2G-R643", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "nzs@caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "dkeres@physics.ucsd.edu", "id": "Keres-Dusan", "name": { "family": "Keres", "given": "Dusan" }, "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-04-30", "gradofc_approval_date": "2018-05-21", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2018", "author_list": "Guszejnov, D\u00e1vid" }, { "id": "/id/eprint/10929", "eprint_id": 10929, "rev_number": 40, "documents": [ { "id": "/id/document/89461", "doc_id": 89461, "rev_number": 7, "files": [ { "id": "/id/file/253511", "fileid": 253511, "datasetid": "document", "objectid": 89461, "filename": "ma_xiangcheng_2018.pdf", "mime_type": "application/pdf", "hash": "2af1f9f46108a27b24ce985bc7ab260e", "hash_type": "MD5", "filesize": 14718465, "mtime": "2018-05-24 00:50:33", "url": "/10929/1/ma_xiangcheng_2018.pdf" } ], "eprint_id": 10929, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "ma_xiangcheng_2018.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/89461" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/89461" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/89461" } ] } } ], "eprint_status": "archive", "userid": 10116, "dir": "disk0/00/01/09/29", "datestamp": "2018-05-25 16:43:56", "lastmod": "2020-03-10 20:21:36", "status_changed": "2018-05-25 16:43:56", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "xiangchma@gmail.com", "id": "Ma-Xiangcheng", "name": { "family": "Ma", "given": "Xiangcheng" }, "orcid": "0000-0001-8091-2349", "show_email": "NO" } ] }, "title": "Understanding Galaxy Formation and Evolution with Realistic Simulations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Galaxies: formation; galaxies: evolution; galaxies: high-redshift; abundances; cosmology", "abstract": "Understanding the formation and evolution of galaxies from the Big Bang to the present day is one of the most important questions in modern astronomy. The tremendous amount of observational data accumulated in the past decade that probe various properties of galaxies across cosmic time demand a more detailed theoretical understanding of galaxy formation and evolution.
\r\n\r\nIn this thesis, I will investigate several open question in this field using state-of-the-art cosmological hydrodynamic zoom-in simulations of galaxy formation from the Feedback in Realistic Environments (FIRE) suite. These high-resolution simulations (10-104M\u2299, 0.1-10pc) include realistic models of the multi-phase ISM, star formation, and stellar feedback and explicitly capture gas cooling down to 10 K, star formation in dense clumps in giant molecular clouds, and feedback coupling on the smallest resolved scales. These simulations are powerful tools for studying the key physics governing galaxy formation and evolution and understanding the detailed observations of galaxy properties.
\r\n\r\nThe first half of this thesis presents three studies on galactic chemical evolution. Chapter 2 focuses on the origin and evolution of the galaxy mass-metallicity relation (MZR), one of the fundamental properties of galaxies. I will show that the FIRE simulations broadly agree with the observed galaxy MZR from z = 0-3. The slope of the MZR is mainly driven by the metal retention fraction in low-mass galaxies, while the amount of redshift evolution of the MZR is mostly determined by the star formation histories of galaxies. Chapter 3 attempts to understanding the diversity of gas-phase metallicity gradients found in intermediate-redshift (z ~ 0.6-3) galaxies. I will show that the metallicity gradient in a galaxy varies on small timescales driven by bursty star formation and feedback cycle at early times, naturally resulting in the observed diversity of metallicity gradients in z ~ 2 galaxies. The metallicity gradient only reflects the instantaneous dynamics of a galaxy. Chapter 4 will study the structure, stellar age and metallicity gradients, and formation history of Milky Way (MW)-like disk galaxies. At high redshift, star formation happens in a chaotic, bursty mode, which eventually forms a nearly spherical structure by z = 0. Since z \u227e 1, a stable gas disk emerged and stars formed in that disk thereafter. The thickness of the gas disk decreases with time due to lowering gas fraction. Stars formed earlier in this disk are kinematically heated to a thicker, flaring disk. Such a formation history leads to the age and stellar metallicity gradients consistent with what observed in the MW disk.
\r\n\r\nThe second half of this thesis focuses on galaxy formation in the first billion years of the Universe, known as the reionization era. Chapters 5 and 6 study the escape fraction of ionizing photons from galaxies at z \u2265 5, which is an important, yet poorly constrained parameter for understanding the reionization history. Most ionizing photons are emitted by the youngest stellar populations in the galaxy, which are usually embedded in their 'birth clouds'. Stellar feedback is required to clear these clouds in a few Myr before ionizing photons are allowed escape. In the meanwhile, the ionizing photon budget decreases rapidly as the most massive stars start to die. The competition of timescales between feedback and stellar evolution is thus the most important physics determines fesc. I will show that canonical single-star stellar population models such as STARBURST99 generally yield a fesc far below what is required for cosmic reionization. Binary models, in contrast, produce more ionizing photons at late times than single-star models and thus lead to a much higher fesc. Chapter 7 presents a new suite of high-resolution cosmological zoom-in simulations of z \u2265 5 galaxies that contains thousands of halos at any time in all zoom-in regions. I will present the stellar mass-halo mass relation, SFR-Mhalo relation, stellar mass-magnitude relation, stellar mass functions, and multi-band luminosity functions at z = 5-12. These prediction agree well with current observational constraints and can be further tested by future observations with the James Webb Space Telescope. Using these new simulations, Chapter 8 studies the morphology and size evolution of galaxies at z \u2265 5. I will show that the rest-frame UV light from z \u2265 5 galaxies is usually dominated by one or several star-forming clumps that are intrinsically bright and small. Current observations with moderate surface brightness limits tend to only pick up the intrinsically small galaxies or individual clumps but miss the diffuse light in the galaxies. Such a selection effect is likely to result in the extremely small sizes claimed for the faint galaxies in the Hubble Frontier Fields.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:05232018-173148982", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05232018-173148982", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "http://dx.doi.org/10.1093/mnras/stv2659" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "http://dx.doi.org/10.1093/mnras/stx273" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "http://dx.doi.org/10.1093/mnras/stx034" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "http://dx.doi.org/10.1093/mnras/stv1679" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "http://dx.doi.org/10.1093/mnras/stw941" }, { "description": "Article adapted for Chapter 7.", "type": "doi", "url": "http://dx.doi.org/10.1093/mnras/sty1024" }, { "description": "Article adapted for Chapter 8.", "type": "doi", "url": "http://dx.doi.org/10.1093/mnras/sty684" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Xiangcheng Ma", "deposited_on": "2018-05-25 16:43:56", "doi": "10.7907/MX2D-6P63", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "chair" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "member" }, { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "role": "member" }, { "email": "eliot@berkeley.edu", "id": "Quataert-Eliot", "name": { "family": "Quataert", "given": "Eliot" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-04-27", "gradofc_approval_date": "2018-05-24", "thesis_awards": "John Stager Stemple Memorial Prize in Physics, 2018.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2018", "author_list": "Ma, Xiangcheng" }, { "id": "/id/eprint/10953", "eprint_id": 10953, "rev_number": 51, "documents": [ { "id": "/id/document/92574", "doc_id": 92574, "rev_number": 7, "files": [ { "id": "/id/file/261106", "fileid": 261106, "datasetid": "document", "objectid": 92574, "filename": "Daven-Quinn-thesis-draft.pdf", "mime_type": "application/pdf", "hash": "7accf66c7d60686118bb551d52ce775c", "hash_type": "MD5", "filesize": 155044090, "mtime": "2018-06-15 03:22:54", "url": "/10953/1/Daven-Quinn-thesis-draft.pdf" } ], "eprint_id": 10953, "pos": 1, "placement": 2, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original final version 6/15/2018", "language": "en", "security": "internal", "license": "other", "main": "Daven-Quinn-thesis-draft.pdf", "media_duration": "0", "media_aspect_ratio": "0", 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Regional mapping techniques are applied to build links between methodologies used to explore rock samples and units \u2014 stratigraphy, structural geology, remote sensing, geochemistry, petrology, and geodynamic modeling. Four research projects are presented: Chapter 2 explores the tectonic context of xenoliths beneath the western margin of North America and illuminates the structural history of the lithospheric underpinnings of the California coast. In Chapter 3, we undertake a structural study of the southern Naukluft Mountains, Namibia, and re-interpret its tectonic context and age. Chapter 4 builds a new method for applying statistical errors to remotely measured planar orientations, and Chapter 5 applies this method to mapping the 3D structure of a globally significant stratigraphy on Mars. We find a long history of interaction with water at the margin of Isidis Basin. Together, these projects demonstrate the application of structural techniques to continental margins on Earth and Mars, and the creation of new techniques to support geological analysis from remotely-sensed data, where structural measurements may be poorly resolved.", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:05282018-115947263", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05282018-115947263", "related_url": { "items": [ { "description": "Thesis Plate 1: Preliminary geologic map of the southern Naukluft Mountains", "type": "doi", "url": "https://doi.org/10.22002/D1.946" }, { "description": "[Interactive] Geologic map of the southern Naukluft Mountains", "type": "doi", "url": "https://doi.org/10.7907/5exk-mr58" }, { "description": "Thesis Plate 2: Stratigraphic columns of the Zebra Nappe, Southern Naukluft Mountains, Namibia", "type": "doi", "url": "https://doi.org/10.22002/D1.947" }, { "description": "Stratigraphic sections of the Zebra Nappe (Dissertation plate 5.2)", "type": "doi", "url": "https:/doi.org/10.7907/9kva-eq78" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "NNX14AO61H" }, { "agency": "Agouron Foundation", "grant_number": "JPG-GIFT-1" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "No thesis embargo request filed. Released to public view 10232018 // Student has indicated that he is interested in sending an updated version with Publications page once articles are published / 6/15/2018 // \r\n", "deposited_by": "Daven Quinn", "deposited_on": "2018-06-19 00:02:30", "doi": "10.7907/9enj-wn23", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "orcid": "0000-0002-2745-3240", "role": "advisor" }, { "email": "grotz@gps.caltech.edu", "id": "Grotzinger-J-P", "name": { "family": "Grotzinger", "given": "John P." }, "orcid": "0000-0001-9324-1257", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "jstock@caltech.edu", "id": "Stock-J-M", "name": { "family": "Stock", "given": "Joann M." }, "orcid": "0000-0003-4816-7865", "role": "chair" }, { "email": "eiler@gps.caltech.edu", "id": "Eiler-J-M", "name": { "family": "Eiler", "given": "John M." }, "orcid": "0000-0001-5768-7593", "role": "member" }, { "email": "asimow@caltech.edu", "id": "Asimow-P-D", "name": { "family": "Asimow", "given": "Paul David" }, "orcid": "0000-0001-6025-8925", "role": "member" }, { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "orcid": "0000-0002-2745-3240", "role": "member" }, { "email": "grotz@gps.caltech.edu", "id": "Grotzinger-J-P", "name": { "family": "Grotzinger", "given": "John P." }, "orcid": "0000-0001-9324-1257", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-02", "gradofc_approval_date": "2018-06-10", "review_status": "approved", "option_major": { "items": [ "geol" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"disk0/00/01/10/14", "datestamp": "2018-06-09 00:04:55", "lastmod": "2021-10-26 17:04:35", "status_changed": "2018-06-09 00:04:55", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "howard.h.hui@gmail.com", "id": "Hui-Howard", "name": { "family": "Hui", "given": "Howard" }, "orcid": "0000-0001-5812-1903", "show_email": "YES" } ] }, "title": "Measuring the Polarization of the Cosmic Microwave Background with BICEP3", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmic Microwave Background; cosmology: observations; gravitational waves; inflation; instrumentation: polarimeters; telescopes", "abstract": "Inflation, a period of accelerated expansion in the early Universe, is postulated to answer the horizon, flatness and monopole problems in the standard model of the Universe. This inflationary scenario generically predicts the existence of primordial gravitational waves, which would leave an unique B-mode polarization pattern in the Cosmic Microwave Background. Detection of the primordial B modes at degree angular scales would be a direct evidence for inflation; and the amplitude, parametrized by the tensor-to-scalar ratio r, would allow us to probe the energy scale at 10-35 second after the Big Bang.
\r\n\r\nThe Bicep/Keck Array experiment is a series of telescopes located at the Amundsen-Scott South Pole Station designed to measure the CMB polarization at degree angular scales. The latest result in Bicep/Keck Array, using data collected up to 2015, and combined with other external data, set upper limits on r < 0.06 at 95% confidence. Bicep3 is the latest addition in the experiment, deployed to South Pole in 2015, and started science observation in 2016. It is a 520 mm aperture, compact two-lens refracting telescope at 95 GHz. With 2500 detectors, it achieved instantaneous sensitivity of 9.1μK√s and 7.3μK√s for 2016 and 2017, respectively. After two year of observations, Bicep3 is estimated to reach a map depth of 3.8μK-arcmin. This is the most sensitive polarization measurement at 95 GHz to date.
\r\n\r\nThis dissertation provides an overview of the Bicep3 instrument design. In particular, the performance of the sub-Kelvin focal plane structure, antenna-coupled transition edge sensor and time domain multiplexing SQUID readout system. We discuss various calibration methods used to probe instrument sensitivity and systematics. Finally, we review the analysis pipeline, and some preliminary results from Bicep3.
\r\n", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:06042018-002455152", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06042018-002455152", "related_url": { "items": [ { "description": "BICEP2 and Keck Array operational overview and status of observations", "type": "arxiv", "url": "https://arxiv.org/abs/1208.0638" }, { "description": "Antenna-coupled TES bolometers for the Keck Array, Spider, and Polar-1", "type": "arxiv", "url": "https://arxiv.org/abs/1208.1247" }, { "description": "Keck array and BICEP3: spectral characterization of 5000+ detectors", "type": "ads", "url": "http://adsabs.harvard.edu/abs/2014SPIE.9153E..3BK" }, { "description": "BICEP3: a 95 GHz refracting telescope for degree-scale CMB polarization", "type": "arxiv", "url": "https://arxiv.org/abs/1407.5928" }, { "description": "Initial Performance of Bicep3: A Degree Angular Scale 95 GHz Band Polarimeter", "type": "ads", "url": "http://adsabs.harvard.edu/abs/2016JLTP..184..765W" }, { "description": "BICEP3 focal plane design and detector performance", "type": "arxiv", "url": "https://arxiv.org/abs/1607.06861" }, { "description": "Optical Characterization of the BICEP3 CMB Polarimeter at the South Pole", "type": "arxiv", "url": "https://arxiv.org/abs/1607.04567" }, { "description": "BICEP3 performance overview and planned Keck Array upgrade", "type": "arxiv", "url": "https://arxiv.org/abs/1607.04668" }, { "description": "Antenna-coupled TES bolometers used in BICEP2, Keck array, and SPIDER", "type": "arxiv", "url": "https://arxiv.org/abs/1502.00619" }, { "description": "A Joint Analysis of BICEP2/Keck Array and Planck Data", "type": "arxiv", "url": "https://arxiv.org/abs/1502.00612" }, { "description": "BICEP2/Keck Array IV: Optical Characterization and Performance of the BICEP2 and Keck Array Experiments", "type": "arxiv", "url": "https://arxiv.org/abs/1502.00596" }, { "description": "BICEP2 / Keck Array V: Measurements of B-mode Polarization at Degree Angular Scales and 150 GHz by the Keck Array", "type": "arxiv", "url": "https://arxiv.org/abs/1502.00643" }, { "description": "BICEP2 / Keck Array VI: Improved Constraints On Cosmology and Foregrounds When Adding 95 GHz Data From Keck Array", "type": "arxiv", "url": "https://arxiv.org/abs/1510.09217" }, { "description": "BICEP2 / Keck Array VII: Matrix based E/B Separation applied to BICEP2 and the Keck Array", "type": "arxiv", "url": "https://arxiv.org/abs/1603.05976" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Howard Hui", "deposited_on": "2018-06-09 00:04:55", "doi": "10.7907/G8ET-FD62", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "chair" }, { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "member" }, { "email": "odore@caltech.edu", "id": "Dor\u00e9-Olivier-P", "name": { "family": "Dor\u00e9", "given": "Olivier P." }, "orcid": "0000-0001-7432-2932", "role": "member" }, { "email": "jfuller@caltech.edu", "id": "Fuller-James", "name": { "family": "Fuller", "given": "James" }, "orcid": "0000-0002-4544-0750", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-25", "gradofc_approval_date": "2018-06-08", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/92340" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/92340" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/92340" } ] } } ], "eprint_status": "archive", "userid": 11293, "dir": "disk0/00/01/10/28", "datestamp": "2018-06-08 23:54:36", "lastmod": "2023-11-08 00:16:42", "status_changed": "2018-06-08 23:54:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "pbcarro@gmail.com", "id": "Carroll-Paul-Brandon", "name": { "family": "Carroll", "given": "Paul Brandon" }, "orcid": "0000-0002-3191-5401", "show_email": "NO" } ] }, "title": "Laboratory and Astronomical Rotational Spectroscopy", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astrochemistry, Spectroscopy, Rotational Spectroscopy", "abstract": "Rotational spectroscopy is a capable technique with a rich history in a variety of chemical physics applications that is undergoing a renaissance thanks to new approaches and powerful new experimental capabilities. This thesis demonstrates that flexibility by examining multiple uses of rotational spectroscopy from instrument development, analytical chemistry, fundamental chemical physics, and astrochemistry.
\r\n\r\nIn chapter 2 we discuss the development of two novel coherent microwave spectrometers. These low cost instruments have only recently become feasible thanks to the burgeoning development of highly flexible digital electronics. The first instrument is designed for undergraduate teaching labs and can be used to demonstrate many new concepts of coherent spectroscopy that are used in modern spectroscopy. It is a rotational spectrometer and can, therefore, also be used for a variety of basic spectroscopy experiments. The second instrument uses the stability and consistency of waveguides and broadband microwave instruments to measure the rotational spectrum and abundance of isotopologues to high accuracy.
\r\n\r\nChapter 3 describes the measurement of the rotational spectrum of the cyclopentanol--water dimer. Using microwave spectroscopy, the spectrum is measured and assigned, and the structure of the dimer is determined. The cyclopentanol--water dimer shows a structure dominated by both strong hydrogen bonding and multiple weaker hydrogen bonds from the hydrocarbon ring. The monomer spectrum is measured, though unassigned due to the strong perturbation from the motion of the ring. Dimerization with water is shown to suppress this motion. This system is shown to be an excellent example of the effect of weak hydrogen bonding on the secondary structure and dynamics of molecular systems.
\r\n\r\nChapter 4 moves to astronomical observations of rotational transitions with the detection of a new species: propylene oxide. Measuring the inventory, abundance, and distribution of molecular species provides tests of our understanding of interstellar chemistry. Propylene oxide is an important addition to this inventory because it is the first chiral species detected beyond our solar system. Chiral species play an enormously important role in biology on Earth, and it is believed that interstellar chemistry may contribute to the early inventory of prebiotic species on newly formed planets. The detection of propylene oxide is discussed in the context of the origin and distribution of chiral molecules in the universe.
\r\n\r\nChapter 5 discusses recent data from the Atacama Large Millimeter/Submillimeter Array. The data maps the distribution of CH3CN isotopologues at incredibly high spatial resolution toward the Orion KL region. The measurement of isotopic ratios in CH3CN is used to inform our understanding the formation mechanisms of cyanides in star forming regions. More broadly, the maps are used to show the extreme spatial heterogeneity of the region, with numerous dense clumps roughly the size of a solar system, each with their own unique chemical and physical structure that reflects their distinct evolutionary histories.
\r\n\r\nFinally, chapter 6 discusses the non-detection of trans ethylmethyl ether. Ethylmethyl ether is one of the largest molecules claimed to be detected in the interstellar medium. Due to its size, it is believed to be produced on grain surfaces as a secondary or tertiary product from dissociation of ice constituents. Given its complexity, its abundance may be an important metric of the accuracy of chemical models of ice chemistry. The study claiming its detection reported an unusually high abundance of the species toward W51 e1/e2. Follow up observations and analysis showed that the original detection was mistaken, likely caused by interference from other features.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:06062018-120951718", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06062018-120951718", "related_url": { "items": [ { "description": "Adapted into Appendix.", "type": "doi", "url": "http://doi.org/10.1063/1.4818137" }, { "description": "Adapted into Chapter IV.", "type": "doi", "url": "http://doi.org/10.1126/science.aae0328" }, { "description": "Adapted into Chapter VI.", "type": "doi", "url": "http://doi.org/10.1088/0004-637X/799/1/15" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Final version received 06/11/2018.", "deposited_by": "Paul Carroll", "deposited_on": "2018-06-08 23:54:36", "doi": "10.7907/8Y1M-6C76", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jlbchamp@caltech.edu", "id": "Beauchamp-J-L", "name": { "family": "Beauchamp", "given": "Jesse L." }, "orcid": "0000-0001-8839-4822", "role": "chair" }, { "email": "weitekamp@caltech.edu", "id": "Weitekamp-D-P", "name": { "family": "Weitekamp", "given": "Daniel P." }, "orcid": "0000-0003-0079-8000", "role": "member" }, { "email": "dadougherty@caltech.edu", "id": "Dougherty-D-A", "name": { "family": "Dougherty", "given": "Dennis A." }, "orcid": "0000-0003-1464-2461", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-09-21", "gradofc_approval_date": "2018-06-08", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/91331" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/91331" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/91331" } ] } } ], "eprint_status": "archive", "userid": 11577, "dir": "disk0/00/01/08/38", "datestamp": "2018-06-01 23:55:50", "lastmod": "2021-10-26 17:06:40", "status_changed": "2018-06-01 23:55:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "alicialanz@gmail.com", "id": "Lanz-Alicia-Elaine", "name": { "family": "Lanz", "given": "Alicia Elaine" }, "orcid": "0000-0003-2565-1558", "show_email": "NO" } ] }, "title": "Studying the Extragalactic Background Light with the Second Cosmic Infrared Background ExpeRiment, CIBER-2", "ispublished": "unpub", "full_text_status": "public", "keywords": "dark ages, reionization, first stars \u2013 diffuse radiation \u2013 infrared: diffuse background \u2013 instrumentation:\r\nspectrographs \u2013 space vehicles", "abstract": "Fluctuations in the extragalactic background light trace emission from the entire history of galaxy formation, including emission from early luminous sources prior to the reionization of the universe. The formation of the first luminous objects represents an important transition in the evolution of the universe from its smooth initial state to the clumpy, highly ordered state observable today. However, these objects are faint and diffuse and not well studied; direct observations of their emission are needed to constrain current numerical simulations of the nonlinear evolution of the early universe. A number of recent near-infrared measurements show excess spatial power at large angular scales inconsistent with models of z < 5 emission from galaxies. These measurements have been interpreted as arising from either redshifted emission of early luminous objects, such as stellar and quasar emission from the epoch of reionization, or the combined intra-halo light from stars thrown out of more recent galaxies during merging activity at lower redshifts. Though astrophysically distinct, both interpretations arise from faint, low surface brightness source populations that are difficult to detect except by statistical approaches using careful observations with suitable instruments. The key to determining the source of these background anisotropies will be wide-field imaging measurements spanning multiple bands from the optical to the near-infrared.
\r\n\r\nThe Cosmic Infrared Background ExpeRiment 2 (CIBER-2) will measure spatial anisotropies in the extragalactic infrared background caused by cosmological structure using six broad spectral bands. The experiment uses three 2048 x 2048 Hawaii-2RG near-infrared arrays in three cameras coupled to a single 28.5 cm telescope housed in a reusable sounding rocket-borne payload. A small portion of each array will also be combined with a linear-variable filter to make absolute measurements of the spectrum of the extragalactic background with high spatial resolution for deep subtraction of Galactic starlight. The large field of view and multiple spectral bands make CIBER-2 unique in its sensitivity to fluctuations predicted by models of lower limits on the luminosity of the first stars and galaxies and in its ability to distinguish between primordial and foreground anisotropies. This work encompasses the scientific motivation for CIBER-2 and describes details of the instrument design and verification prior to flight.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:04272018-205538217", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04272018-205538217", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Alicia Lanz", "deposited_on": "2018-06-01 23:55:50", "doi": "10.7907/CN9Y-MB61", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "advisor" }, { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "chair" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" }, { "email": "Olivier.P.Dore@jpl.nasa.gov", "id": "Dor\u00e9-Olivier-P", "name": { "family": "Dor\u00e9", "given": "Olivier P." }, "orcid": "0000-0001-7432-2932", "role": "member" }, { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-05-08", "gradofc_approval_date": "2018-06-01", "thesis_awards": "Graduate Dean's Award, 2018.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2018", "author_list": "Lanz, Alicia Elaine" }, { "id": "/id/eprint/10430", "eprint_id": 10430, "rev_number": 33, "documents": [ { "id": "/id/document/83252", "doc_id": 83252, "rev_number": 5, "files": [ { "id": "/id/file/235259", "fileid": 235259, "datasetid": "document", "objectid": 83252, "filename": "piskorz_danielle_2017.pdf", "mime_type": "application/pdf", "hash": "ec509d987fdf16bb56c23c80577e5551", "hash_type": "MD5", "filesize": 8088768, "mtime": "2017-10-01 17:05:56", "url": "/10430/1/piskorz_danielle_2017.pdf" } ], "eprint_id": 10430, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "piskorz_danielle_2017.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/83424" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/83424" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/83424" } ] } } ], "eprint_status": "archive", "userid": 11349, "dir": "disk0/00/01/04/30", "datestamp": "2017-10-13 15:49:46", "lastmod": "2023-11-08 00:16:42", "status_changed": "2017-10-13 15:49:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "dpiskorz@gmail.com", "id": "Piskorz-Danielle-F", "name": { "family": "Piskorz", "given": "Danielle F." }, "orcid": "0000-0003-4451-2342", "show_email": "NO" } ] }, "title": "Exploring Exoplanets' Spectroscopic Secrets: Clues on the Migration and Formation of Hot Jupiters", "ispublished": "unpub", "full_text_status": "public", "keywords": "exoplanets; hot Jupiters; giant planets; binary star; observational techniques", "abstract": "Before the mid-90's, scientists' theories for planet formation were finely-tuned to explain the existence of our own Solar System. These theories were thrown into disarray when astronomers began to discover exoplanets, or planets in other solar systems. Forced to reconcile theory with observation, astronomers and planetary scientists have worked together for the past twenty years to solve the puzzles created by these thousands of exoplanets. One particularly intriguing group of newly-discovered planets were the hot Jupiters, planets the size of our Jupiter orbiting their host star every few days. This thesis details two observational campaigns that attempt to illuminate the origin and composition of hot Jupiters. Each project is powered by the NIRSPEC (Near-Infrared SPECtrometer) instrument located at Mauna Kea in Hawaii. The first project aims to determine the stellar multiplicity rate of hot Jupiter host stars. Such a metric can inform the migration histories of these planets. The second project treats a hot Jupiter and its host star as a spectroscopic binary. This treatment reveals the orbital elements and atmospheric composition of the hot Jupiter. The spectroscopic methods described in this thesis are small steps in the study of hot Jupiters and ultimately potentially habitable exoplanets.", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:09122017-074006746", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09122017-074006746", "related_url": { "items": [ { "description": "Chapter 2, published in the Astrophysical Journal", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/814/2/148" }, { "description": "Part of chapter 3, all of chapter 4, published in the Astrophysical Journal", "type": "doi", "url": "https://doi.org/10.3847/0004-637X/832/2/131" }, { "description": "Chapter 5, published in the Astronomical Journal", "type": "doi", "url": "https://doi.org/10.3847/1538-3881/aa7dd8" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released to public view 05/07/2018 //\r\nRestricted to Caltech community only until 6 April 2017. // From author: Chapter 6 has been submitted to The Astronomical Journal, but has not yet been published.", "deposited_by": "Danielle Piskorz", "deposited_on": "2017-10-13 15:49:46", "doi": "10.7907/Z9222RZX", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "co-advisor" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-09-05", "gradofc_approval_date": "2017-10-12", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2018", "author_list": "Piskorz, Danielle F." }, { "id": "/id/eprint/10777", "eprint_id": 10777, "rev_number": 38, "documents": [ { "id": "/id/document/87276", "doc_id": 87276, "rev_number": 4, "files": [ { "id": "/id/file/247658", "fileid": 247658, "datasetid": "document", "objectid": 87276, "filename": "Spalding_Christopher_2018.pdf", "mime_type": "application/pdf", "hash": "084f82b27cb4db4b4114eb66c977a9c0", "hash_type": "MD5", "filesize": 7604191, "mtime": "2018-03-21 17:33:44", "url": "/10777/1/Spalding_Christopher_2018.pdf" } ], "eprint_id": 10777, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Spalding_Christopher_2018.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": 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"/id/document/87276" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/87276" } ] } } ], "eprint_status": "archive", "userid": 11529, "dir": "disk0/00/01/07/77", "datestamp": "2018-04-10 16:59:25", "lastmod": "2022-12-02 19:48:12", "status_changed": "2018-04-10 16:59:25", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "christopherspalding@hotmail.co.uk", "id": "Spalding-Christopher", "name": { "family": "Spalding", "given": "Christopher" }, "orcid": "0000-0001-9052-3400", "show_email": "NO" } ] }, "title": "The Primordial Origin and Dynamical Sculpting of Close-In Planetary System Architectures", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science; Astrophysics; Planet Formation", "abstract": "For centuries, planet formation theories were tuned to reproduce the remarkable coplanarity of our Solar System. Specifically, the eight planetary orbital planes exhibit mutual inclinations limited to ~1\u22122 degrees. Furthermore, the misalignment between the Sun's spin axis and the orbital planes of the planets \u2013 the 'spin-orbit misalignment'\u2013 is only about 6 degrees. However, observational characterization of close-in extrasolar planetary systems has revealed an abundance of spin-orbit misalignments ranging all the way from 0 to 180 degrees (Winn et al. 2010). Particularly among the hot Jupiters (giant planets with orbital periods shorter than ~1 week), spin-orbit misalignments are more prevalent in systems hosted by stars with effective temperatures exceeding about 6200 K. Previous work has suggested that these misalignments arose from violent dynamical interactions that excited planets onto inclined and eccentric orbits, with subsequent tidal circularization generating the observed population (Albrecht et al. 2012). This hypothesis has had great difficulty explaining misaligned multi-planet systems, and misaligned orbits of planets that are too distant from their host stars for tidal circularization to act over a sufficiently short timescale. A new mechanism is required.
\r\n\r\nIn chapters II-VI, I present a theoretical framework referred to as \"disk-torquing,\" whereby spin-orbit misalignments arise through the tilting of protoplanetary disks themselves (Batygin 2012, Spalding and Batygin 2014, 2015). In this picture, gravitational torques from a companion star lead to the precession of the protoplanetary disk. When the disk is young and massive, gravitational star-disk coupling quenches misalignments between the stellar spin axis and disk plane. However, as the disk dissipates, a secular resonance is encountered that impulsively excites large stellar obliquities, ranging between 0 and 180 degrees, in accordance with the observations. In addition, I computed the magnetic torques between the star and disk, finding that a dipole field strength of ~1 kGauss is sufficiently strong to realign the star and disk within typical disk lifetimes (~3 million years). Magnetic fields of this magnitude are observed to persist throughout the disk-hosting stage only for stars less massive than ~1.2 solar masses (Gregory et al. 2012), corresponding to a main sequence effective temperature of 6200 K, i.e., coincident with the observed break between aligned and misaligned hot Jupiters. Cumulatively, the disk-torquing framework exhibits qualitative consistency with the observed dependence of spin- orbit misalignments upon stellar mass, leaving the theory ripe for a statistical comparison to observations within future work.
\r\n\r\nThe final three chapters change focus from spin-orbit misalignments toward the excitation of mutual inclinations between planetary orbits \u2013 orbit-orbit misalignments. Evaluation of the relative numbers of single to multi-transiting planetary systems within the Kepler space telescope\u2019s dataset has revealed a dichotomy whereby there exist two populations of planetary system \u2013 one with low orbit-orbit inclination, and a second that either possesses a single planet, or possesses multiple planets with large mutual inclinations, leaving only one detectable via transit (Johansen et al. 2012, Ballard and Johnson 2016). In separate but related observational work, it has become apparent that transiting hot Jupiters often appear without co-transiting, close-in planetary companions, wheres warm Jupiters often do (Steffen et al. 2012, Huang et al. 2016). I showed that both of these observations can naturally arise owing to secular perturbations from the host star (Spalding and Batygin 2016, 2017). Specifically, young stars rotate fast, becoming oblate. If the star\u2019s spin axis is misaligned with respect to the orbits of a multi-planet system, its quadrupole moment can disrupt the coplanarity of the system. Indeed, the stellar perturbations are often sufficient to completely destabilize the system (Chapter VI). In addition to constituting an entirely new mechanism of planetary instability, the origin of the required spin-orbit misalignment relates directly back to the discussion above \u2013 spin-orbit misalignments may drive the seemingly unrelated Kepler dichotomy.
\r\n\r\nFinally, I tied in the observation that hot Jupiters appear lonely by demonstrating that stellar contraction can give rise to a secular resonance that tilts exterior companions of hot Jupiters, taking them out of transit. Crucially, this resonance is encountered at an earlier time in systems hosting warm Jupiters, precisely owing to their slightly increased orbital distance. I found that the demarcation between a system undergoing secular tilting, and one where the disk quenches the tilting, coincides well with the relatively arbitrary dividing line between hot and warm Jupiters, usually set at orbital periods of about a week.
\r\n\r\nIn summary, I showed that spin-orbit misalignments and orbit-orbit misalignments, measured across a range of planetary size classes, can arise primordially owing to interactions with the host star and binary companions. The importance of the central star had most likely been missed in the previous literature owing to our solar system\u2019s peculiarly wide inner edge at ~0.4 AU, as opposed to the more typical ~0.1 AU within a galactic setting. In reality, through the wider lens of our galactic planetary census, a true understanding of planet formation demands a look at star-planet interactions wholly unknown from centuries of solar system exploration.
", "date": "2018", "date_type": "degree", "id_number": "CaltechTHESIS:03202018-115359218", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03202018-115359218", "related_url": { "items": [ { "description": "Article adapted for Chapter II.", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/790/1/42" }, { "description": "Article adapted for Chapter III.", "type": "doi", "url": "https://doi.org/10.1088/2041-8205/797/2/L29" }, { "description": "Article adapted for Chapter IV.", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/811/2/82" }, { "description": "Article adapted for Chapter V.", "type": "doi", "url": "https://doi.org/10.3847/0004-637X/830/1/5" }, { "description": "Article adapted for Chapter VI.", "type": "arxiv", "url": "https://arxiv.org/abs/1803.01182" }, { "description": "Article adapted for Chapter VII.", "type": "doi", "url": "https://doi.org/10.3847/1538-3881/aa8174" } ] }, "referencetext": { "items": [ "Adams, Fred C (2010). \u201cThe birth environment of the Solar System\u201d. 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In: Astronomy & Astrophysics 550, A99." ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Christopher Spalding", "deposited_on": "2018-04-10 16:59:25", "doi": "10.7907/Z9RB72TQ", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kbatygin@gps.caltech.edu", "id": "Batygin-K", "name": { "family": "Batygin", "given": "Konstantin" }, "orcid": "0000-0002-7094-7908", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "djs@caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "chair" }, { "email": "hknutso2@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "member" }, { "email": "wfischer@caltech.edu", "id": "Fischer-W-W", "name": { "family": "Fischer", "given": "Woodward W." }, "orcid": "0000-0002-8836-3054", "role": "member" }, { "email": "kbatygin@gps.caltech.edu", "id": "Batygin-K", "name": { "family": "Batygin", "given": "Konstantin" }, "orcid": "0000-0002-7094-7908", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-02-13", "gradofc_approval_date": "2018-04-09", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"full_text_status": "public", "keywords": "supermassive black holes; active galactic nuclei (AGN); X-ray spectroscopy; spectral analysis", "abstract": "Despite the long history of studies of active galactic nuclei (AGN), details of the structure of the accretion flow onto supermassive black holes are far from clear. Work presented in this thesis is directed at unveiling properties of AGN structure through broadband X-ray spectroscopy, with particular emphasis on the hard X-ray band (photon energies above 10 keV). With its unprecedented sensitivity in this energy band, the NuSTAR telescope provides the key observational diagnostics of the properties of the AGN X-ray source, the corona, and the surrounding gas in the accretion disk, the broad-line region, and the torus.
\r\n\r\nThe first study presented in this thesis focuses on measurements of the optical depth and the temperature of the plasma in the corona of an obscured AGN. Fitting theoretical spectral models for coronal emission to the NuSTAR data constrained these two basic physical parameters under the assumption of either spherical or disk-like geometry for the corona.
\r\n\r\n\r\nThe remainder of the thesis is dedicated to studies of the anisotropic obscuring structure broadly referred to as the torus. One of them is a case study of three heavily obscured AGN with spectra dominated by the X-ray light scattered and reprocessed in the torus, where it is possible to constrain one of the basic torus properties -- its globally averaged column density. The following study presents the calculation of a new spectral model for reprocessing of the intrinsic X-ray continuum within the torus. Its added flexibility compared to previously available models allows for both the average column density of the torus and its covering factor to be constrained from broadband X-ray spectra of a wide variety of AGN.
\r\n\r\n\r\nThe final part of the thesis in based on a large survey of the local obscured AGN population performed with NuSTAR. Spectral modeling of more than a hundred individual AGN, including both old and new spectral models, is presented. From analyses of the X-ray data for a large and representative AGN sample, for the first time, it is found that their tori preferentially have high covering factors and average column densities close to unity optical depth for Compton scattering.
\r\n", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:06052017-232351957", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06052017-232351957", "related_url": { "items": [ { "description": "Published paper adopted for Ch. 2", "type": "doi", "url": "http://iopscience.iop.org/article/10.1088/0004-637X/800/1/62/meta" }, { "description": "Published paper adopted for Ch. 3", "type": "doi", "url": "http://iopscience.iop.org/article/10.1088/0004-637X/794/2/111/meta" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Fulbright Science & Technology Award" }, { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "NNX14AQ07H" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "suggestions": "Released to public view 19 March 2018 // Restricted to Caltech community only until 6 December 2017.", "deposited_by": "Mislav Balokovic", "deposited_on": "2017-06-07 17:34:01", "doi": "10.7907/Z9WM1BG8", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "chair" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-05-25", "gradofc_approval_date": "2017-06-06", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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atmospheres; scattering; techniques: spectroscopic", "abstract": "This thesis presents theoretical investigations in three areas of astrophysics, all related to radiative processes and interactions between stellar radiation and gaseous media in the Universe, ranging from the intergalactic and interstellar medium to planetary atmospheres.
\r\n\r\nPart I of the thesis consists of two independent investigations in which we study the effects of stellar feedback in high-redshift environments. The topic of Chapter 2 is the intergalactic medium (IGM) in the epoch just after the formation of the first stars in the Universe, but before the cosmic reionization was completed. This epoch is of great interest for the ongoing and future experiments aimed at observing the neutral IGM via the redshifted 21 cm line of hydrogen. We study the effects of resonant scattering of Lyman-\u03b1 photons produced by early stars on the structure of temperature fluctuations in the IGM. In Chapter 3, we use cosmological hydrodynamic simulations of galaxy evolution to study the effects of stellar feedback on the clumpy structure of star-forming galaxies at z ~ 2. Observations of high-redshift galaxies show that their morphology is often dominated by a few giant clumps of intense star formation, but the nature and the importance of these clumps for the evolution of their host galaxies are uncertain. We present a detailed analysis of the properties of giant clumps in a high-redshift simulated galaxy from the FIRE project.
\r\n\r\nPart II of the thesis is devoted to the effects of Raman scattering of stellar radiation in the atmospheres of extrasolar planets. Spectral signatures of Raman scattering imprinted in the geometric albedo spectrum of a gaseous planet carry information about the properties of the planet's atmosphere---its composition, temperature, and the radiation-penetration depth. In Chapter 5, we present the results of radiative transfer calculations including the treatment of Raman scattering for different types of planetary atmospheres and analyze the feasibility of detecting the spectral signatures of Raman scattering in nearby exoplanets. The structure and the intensity of Raman spectral features depends on both the atmospheric properties and the shape of the stellar spectrum irradiating the atmosphere. In Chapter 6, we analyze the diversity of Raman features in the geometric albedo spectra of planets hosted by different types of stars.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:05312017-154839851", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05312017-154839851", "related_url": { "items": [ { "description": "Article adapted for Ch. 2.", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/779/2/146" }, { "description": "Article adapted for Ch. 3.", "type": "doi", "url": "http://dx.doi.org/10.1093/mnras/stw2754" }, { "description": "Article adapted for Ch. 5.", "type": "doi", "url": "http://dx.doi.org/10.3847/0004-637X/832/1/30" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Fulbright Science & Technology Award" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "suggestions": "Files temporarily withheld until Jun 9, 2017 - released to public view 6/9/2017", "deposited_by": "Antonija Oklopcic", "deposited_on": "2017-06-02 21:56:33", "doi": "10.7907/Z9GM85CS", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "hirata.10@osu.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "member" }, { "email": "hirata.10@osu.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-05-09", "gradofc_approval_date": "2017-06-02", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"abstract": "In this thesis, I develop a new suite of tools to address two questions in exoplanet science: how common are Earth-mass planets in the habitable zones of Solar-type stars, and can we detect signs of life on other worlds?
\r\n\r\nAnswering the first question requires a method for detecting Earth-Sun analogs. Currently, the radial velocity (RV) method of exoplanet detection is one of the most successful tools for probing inner planetary systems. However, degeneracy between a spectrometer's wavelength calibration and the astrophysical RV shift has limited the sensitivity of today's instruments. In my thesis, I address a method for breaking this degeneracy: by combining a traditional spectrometer design with a dynamic interferometer, a fringe pattern is generated at the image plane that is highly sensitive to changes in the radial velocity of the target star. I augmented previous theoretical studies of the method, creating an end-to-end simulation to 1) introduce and recover wavelength calibration errors, and 2) investigate the effects of interferometer position errors on the RV precision. My simulation showed that using this kind of interferometric system, a 5-m class telescope could detect an Earth-Sun analog.
\r\n\r\nAddressing the occurrence rate of Earth twins also requires an understanding of planet formation in multiple star systems, which encompass half of all Solar-type stars. Gravitational interactions between binary components separated by 10-100 astronomical units are predicted to truncate the outer edges of their respective disks, possibly reducing the disks' lifetimes. Consequently, the pool of material and the amount of time available for planet formation may be smaller than in single star systems. The stars' rotational periods provide a fossil record of these events: star-disk magnetic interactions initially prevent a contracting pre-main sequence star from spinning up, and hence a star with a shorter-lived disk is expected to be spinning more quickly when it reaches the zero age main sequence. In order to conduct a large-scale multiplicity survey to investigate the relationship between stellar rotation and binary system properties (e.g. their separations and mass ratios), I contributed to the commissioning of Robo-AO, a robotic laser guide star adaptive optics system, at the Kitt Peak 2.1-m. After the instrument's installation, I wrote a data pipeline to optimize the system's sensitivity to close stellar companions via reference star differential imaging. I then characterized Robo-AO's performance during its first year of operations. Finally, I used Robo-AO to search for binaries among the 759 stars in the Pleiades with rotational periods measured using the photometric data of the re-purposed Kepler telescope, K2.
\r\n\r\nDetecting signs of life on other worlds will require detailed characterization of rocky exoplanet atmospheres. Polarimetry has long been proposed as a means of probing these atmospheres, but current instruments lack the sensitivity to detect the starlight reflected and polarized by such small, close-in planets. However, the latest generation of high contrast imaging instruments (e.g. GPI and SPHERE) may be able to detect the polarization of thermal emission by young gas giants due to scattering by aerosols in their atmospheres. Observational constraints on the details of clouds physics imposed by polarized emission will improve our understanding of the planets' compositions, and hence their formation histories. For the case of the brown dwarf HD19467 B orbiting a nearby Sun-like star, I demonstrated that the Gemini Planet Imager can detect linear polarizations on the order predicted for these cloudy exoplanets. My current pilot programs can produce the first detections of polarized exoplanet emission, while also building expertise for reflected starlight polarimetry with future observatories.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:05302017-105911246", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302017-105911246", "related_url": { "items": [ { "description": "Previously published materials in Chapter II.", "type": "doi", "url": "https://doi.org/10.1086/683796" }, { "description": "Previously published materials in Chapter III.", "type": "doi", "url": "https://doi.org/10.3847/0004-637X/820/2/111" }, { "description": "Previously published materials in Chapter V.", "type": "arxiv", "url": "https://arxiv.org/abs/1703.08867" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Files temporarily withheld until Jun 7, 2017 - released to public view 6/7/2017", "deposited_by": "Rebecca Jensen-Clem", "deposited_on": "2017-05-31 21:45:09", "doi": "10.7907/Z96971M9", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "enk@astro.caltech.edu", "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "Evan N." }, "orcid": "0000-0001-6196-5162", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-05-18", "gradofc_approval_date": "2017-05-31", "thesis_awards": "Everhart Distinguished Graduate Student Lecturer Award, 2017.", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/72917" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/72917" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/72917" } ] } } ], "eprint_status": "archive", "userid": 10546, "dir": "disk0/00/00/99/01", "datestamp": "2016-08-22 22:49:40", "lastmod": "2020-03-11 18:42:17", "status_changed": "2016-08-22 22:49:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "lumos.leee@gmail.com", "id": "Li-Cheng", "name": { "family": "Li", "given": "Cheng" }, "orcid": "0000-0002-8280-3119", "show_email": "YES" } ] }, "title": "Convection in Planetary Atmospheres: Titan's Haze, Saturn's Storm and Jupiter's Water", "ispublished": "unpub", "full_text_status": "public", "keywords": "Convection; Jupiter; Juno; Photochemistry; Titan; Eddy diffusion", "abstract": "Atmospheric convection is a profound topic. Numerous books have been written on the consequences of convection. Yet, the picture of convection is still far from complete because of its high nonlinearity, multi-scale coupling and complex interactions with other systems. The theme of my dissertation is to investigate three aspects of atmospheric convection on three different planets. This dissertation is multi-disciplinary and includes scientific topics like photochemistry, dynamics and radiation, and methodologies like information retrieval, theoretical calculation and dynamic modeling.
\r\n\r\nChapter 1 and 2 study Titan. It focuses on how to infer the strength of convection from the vertical distribution of chemical species. In a photochemical model, convection is parameterized as eddy diffusion and the strength of convection is proportional to eddy diffusivity. We developed an inversion method to retrieve the vertical profile of eddy diffusivity directly from the Cassini observations and found out a stable layer in the atmosphere which may give rise to the detached haze layer on Titan. In addition, new observation from Cassini/CIRS limb sounding came a few month later. C3H6 was detected for the first time in the stratosphere. Our new photochemical model with the updated eddy diffusion profile successfully explained the observed vertical distribution of C3H6. Chapter 2 explains the modeling result and does a systematic study on all C3-hydrocarbons.
\r\n\r\nChapter 3 studies Saturn. It investigates the role of convection on regulating Saturn\u2019s giant storms. Six giant storms, called Great White Spots, have erupted on Saturn since 1876 at intervals of about 30 years. The most recent one occurred on Dec. 5th, 2010 at planetographic latitude 37.7\u00b0N. It produced intense lightning, created enormous cloud disturbances and wrapped around the planet in 6 months. We proposed the water-loading mechanism to explain the periodicity. Moist convection is suppressed for decades due to the larger molecular weight of water in a hydrogen-helium atmosphere. We show that this mechanism requires the deep water vapor mixing ratio to be greater than 1.0%, which implies Saturn\u2019s O/H to be at least 10 times the solar value.
\r\n\r\nChapter 4 studies Jupiter. It proposes an inversion strategy for the upcoming Juno microwave observation based on the modeling results and the theoretical arguments developed in Chapter 3. We extend the Juno/MWR\u2019s functionality by retrieving both the deep water mixing ratio and a few dynamic parameters representing subcloud meteorology. This proposition will contribute substantially to achieving the Juno/MWR objectives and shed light on the functioning of convection on planets with deep atmospheres.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:08172016-211741364", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08172016-211741364", "related_url": { "items": [ { "description": "Article adapted for chapter 1", "type": "doi", "url": "http://dx.doi.org/10.1016/j.pss.2013.10.009" }, { "description": "Article adapted for chapter 2", "type": "doi", "url": "http://dx.doi.org/10.1088/2041-8205/803/2/L19" }, { "description": "Article adapted for chapter 3", "type": "doi", "url": "http://dx.doi.org/10.1038/ngeo2405" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released to public view 19 March 2018 // \r\nRestricted to Caltech community only until 30 September 2017.", "deposited_by": "Cheng Li", "deposited_on": "2016-08-22 22:49:40", "doi": "10.7907/Z9R78C58", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "chair" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "role": "member" }, { "email": "bordoni@gps.caltech.edu", "id": "Bordoni-S", "name": { "family": "Bordoni", "given": "Simona" }, "role": "member" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-05-23", "gradofc_approval_date": "2016-08-22", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "envreng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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discovered outside of our solar system were very different from the solar system planets. These discoveries raised new challenges to planet formation models, which were designed to explain the origin of the solar system planets. One particularly intriguing population, the \"hot Jupiters\" were some of the first planets discovered. These gas giant planets have masses similar to Jupiter and Saturn, however, they were found on orbits 100 times closer to their star than Jupiter is to the sun. Proposed formation scenarios involve models that argue for formation at presently observed locations, but these are challenged by the lack of planet-building materials so close to the host star. Other models assume these planets form at more moderate locations, perhaps in a manner similar to Jupiter and Saturn, followed by inward migration via some other mechanism. These models are challenged by the lack of a known migration mechanism.
\r\n\r\nThis dissertation compiles three studies conducted over the past five years to investigate the formation and migration histories of gas giant exoplanets. After the discovery of the first hot Jupiter, additional discoveries revealed some population characteristics that could provide evidence for certain formation or migration scenarios. A large fraction of hot Jupiters were found to have eccentric orbits and/or misaligned orbits relative to the star's spin axis. These properties suggest that a gravitational interaction with an additional massive object may have played a role in the dynamical history of these hot Jupiters. Studies of stellar multiplicity for nearby, sun-like stars have also revealed that multi-stellar systems are common.
\r\n\r\nThe studies presented in this dissertation investigate whether stellar companions to giant planet systems influence the planets. In the first and second study, we conduct a survey for stellar companions around stars that host hot Jupiters detected by the transiting method. The first study examines whether stars hosting misaligned planets are more likely to host a companion star. We found no such correlation, suggesting that stellar companions do not play a dominant role in causing planetary misalignment. In the second study, we look at the population of stellar companions as a whole to quantify the fraction of hot Jupiters that might have migrated due to stellar interactions. We find that less than 20% of hot Jupiters might have experienced this migration scenario. However, we do find that hot Jupiters are three times more likely to be in a wide multi-stellar system compared to nearby stars that do not host hot Jupiters, suggesting some other connection between the companion star and the giant planet.
\r\n\r\nIn the third study, we search for stellar companions around stars that host giant planets over a wide range of separations, from the close-in hot Jupiters to giant planets as far away as Jupiter is to our sun. These planets were found via the radial velocity method. We compare the giant planets' orbital properties for single- and multi-stellar systems to determine whether planets in multi-stellar systems show some evidence for star-planet interactions. With the current dataset, we find no evidence to support the hypothesis that planets in multi-stellar systems have a different set of orbital properties.
\r\n\r\nFinally, we present preliminary results of an ongoing survey to understand giant planet formation on the other extreme end. Instead of hot Jupiters on close-in orbits, this survey seeks to explain the origin of the very distant giant planetary mass objects found by direct imaging surveys. These objects are often found on separations that are ten to one hundred times farther away than Neptune is to our sun. Due to their distance and size, it's not certain if these objects are some of the biggest planets in existence or if they are the smallest stars. This new survey will search for planets to serve as the link between known giant exoplanets and these unknown directly imaged objects.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:05262017-234026021", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05262017-234026021", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/800/2/138" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "http://dx.doi.org/10.3847/0004-637X/827/1/8" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "http://dx.doi.org/10.3847/1538-3881/aa6cac" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Natural Science and Engineering Research Council of Canada" }, { "agency": "NASA Earth and Space Sciences Fellowship", "grant_number": "NNX15AR12H" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Files temporarily withheld until Jun 12, 2017 - released to public view 6/12/2017", "deposited_by": "Henry Ngo", "deposited_on": "2017-06-05 21:39:45", "doi": "10.7907/Z9KD1VZW", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "chair" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "member" }, { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "member" }, { "email": "kbatygin@gps.caltech.edu", "id": "Batygin-K", "name": { "family": "Batygin", "given": "Konstantin" }, "orcid": "0000-0002-7094-7908", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-05-19", "gradofc_approval_date": "2017-06-05", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"/id/document/77903" } ] } } ], "eprint_status": "archive", "userid": 4404, "dir": "disk0/00/01/01/73", "datestamp": "2017-05-23 23:18:00", "lastmod": "2020-03-10 23:49:43", "status_changed": "2017-05-23 23:18:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "slogander@gmail.com", "id": "Lap\u00f4tre-Mathieu-Gaetan-Andre", "name": { "family": "Lap\u00f4tre", "given": "Mathieu Gaetan Andre" }, "orcid": "0000-0001-9941-1552", "show_email": "NO" } ] }, "title": "Sedimentary Processes on Earth and Mars: Canyon Erosion, Sand-Ripple Formation, and Mineral Composition", "ispublished": "unpub", "full_text_status": "public", "keywords": "canyons; ripples; sand; mineral composition; Mars; fluvial geomorphology; eolian geomorphology; spectroscopy", "abstract": "Over the past few decades, orbiters, landers, and rovers have significantly expanded our understanding of Mars\u2019 hydrology and climate; however, significant knowledge gaps stand in the way of our quest for martian life. In particular, the global drying of the planet remains one of the grandest unsolved mysteries in planetary science. To help unravel this puzzle, we develop new quantitative theories for sedimentary processes with implications for both Earth and Mars. This thesis revolves around three main sedimentary processes \u2013 erosion, deposition, and sediment transport. First, we focus on the erosion of bedrock canyons by water on Earth and Mars. After showing that groundwater seepage erosion is only efficient at carving canyons in restricted conditions, we develop a new hydraulic theory for flow focusing upstream of horseshoe-shaped waterfalls and combine it with waterfall-erosion mechanics to constrain the discharge, duration, and volume of canyon-carving floods on Earth and Mars. We show that martian Hesperian floods were large but short-lived. Second, we investigate fluid and sediment controls on the equilibrium size of bedforms. We develop a comprehensive scaling relation to predict the size of ripples forming in various sedimentary environments, including martian brines and methane flows on Titan, and show that the scaling relation predicts the size of large wind ripples forming under a thin martian atmosphere. This new theory, combined with observations of large-ripple cross-strata in wind-blown sandstones of the Burns formation at Victoria crater, suggests that Mars had a thin atmosphere around the Noachian-Hesperian boundary. Finally, we use orbiter-based inferences of the mineralogy of sands of the Bagnold dunes of Gale crater to disentangle the magnitude of wind sorting and local sediment sources. We develop a new probabilistic framework to invert for surface mineralogy, groundtruth our predictions with compositional datasets provided by the Curiosity rover, and discuss the implications of our findings for mineral sorting by martian winds and paleoenvironmental interpretations of martian wind-blown sandstones. Collectively, these results provide new mechanistic and quantitative constraints on the past hydrology and climate of Mars that are key to assess Mars\u2019 astrobiological potential through space and time.", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:05152017-105730412", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05152017-105730412", "related_url": { "items": [ { "description": "Article adapted for ch. 3 (Journal of Geophysical Research: Earth Surface)", "type": "doi", "url": "http://dx.doi.org/10.1002/2014JF003412" }, { "description": "Article adapted for ch. 4 (Journal of Geophysical Research: Planets)", "type": "doi", "url": "http://dx.doi.org/10.1002/2016JE005061" }, { "description": "Article adapted for ch. 5 (Science)", "type": "doi", "url": "http://dx.doi.org/10.1126/science.aaf3206" }, { "description": "Article adapted for ch. 6 (Geology)", "type": "doi", "url": "http://dx.doi.org/10.1130/G38598.1" }, { "description": "Article adapted for ch. 7 (Journal of Geophysical Research: Planets)", "type": "doi", "url": "http://dx.doi.org/10.1002/2016JE005248" }, { "description": "Article adapted for ch. 8 (Journal of Geophysical Research: Planets)", "type": "doi", "url": "http://dx.doi.org/10.1002/2016JE005133" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "12-PLANET12F-0071" }, { "agency": "NSF", "grant_number": "EAR-1147381" }, { "agency": "NASA", "grant_number": "NNX13AM83G" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released to public view 2020-02-07 // Embargo extended to April 5, 2018 // Chapter 2 is under consideration for Nature Geoscience, and we would thus like to keep the whole thesis and all supplementary files under embargo until publication of Chapter 2. I am filling out the \"Thesis Exception Form\", with a release date around November 15 2017. There is a chance I will need further extension at that time.\r\n\r\n// Embargo request approved by committee 7/5/2017.", "deposited_by": "Mathieu Lapotre", "deposited_on": "2017-05-23 23:18:00", "doi": "10.7907/Z9RF5S2T", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mpl@gps.caltech.edu", "id": "Lamb-M-P", "name": { "family": "Lamb", "given": "Michael P." }, "role": "advisor" }, { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "chair" }, { "email": "mpl@gps.caltech.edu", "id": "Lamb-M-P", "name": { "family": "Lamb", "given": "Michael P." }, "role": "member" }, { "email": "grotz@gps.caltech.edu", "id": "Grotzinger-J-P", "name": { "family": "Grotzinger", "given": "John P." }, "role": "member" }, { "email": "farley@gps.caltech.edu", "id": "Farley-K-A", "name": { "family": "Farley", "given": "Kenneth A." }, "role": "member" }, { "email": "matthew.p.golombek@jpl.nasa.gov", "id": "Golombek-M-P", "name": { "family": "Golombek", "given": "Matthew P." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-05-08", "gradofc_approval_date": "2017-05-23", "review_status": "approved", "option_major": { "items": [ "geol" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2017", "author_list": "Lap\u00f4tre, Mathieu Gaetan Andre" }, { "id": "/id/eprint/10047", "eprint_id": 10047, "rev_number": 41, "documents": [ { "id": "/id/document/76201", "doc_id": 76201, "rev_number": 2, "files": [ { "id": "/id/file/215661", "fileid": 215661, "datasetid": "document", "objectid": 76201, "filename": "kher_aditya_2017.pdf", "mime_type": "application/pdf", "hash": "ab7902c4e8108247828a9e73d36630a0", "hash_type": "MD5", "filesize": 5237971, "mtime": "2017-02-10 00:58:00", "url": "/10047/8/kher_aditya_2017.pdf" } ], "eprint_id": 10047, "pos": 8, "placement": 8, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "kher_aditya_2017.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"/id/document/134306", "doc_id": 134306, "rev_number": 1, "files": [ { "id": "/id/file/379751", "fileid": 379751, "datasetid": "document", "objectid": 134306, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "9a2882d378a75321bcbe842cdee99497", "hash_type": "MD5", "filesize": 30049, "mtime": "2021-06-24 21:22:03", "url": "/10047/15/indexcodes.txt" } ], "eprint_id": 10047, "pos": 15, "placement": 15, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/76201" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/76201" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/76201" } ] } } ], "eprint_status": "archive", "userid": 11051, "dir": "disk0/00/01/00/47", "datestamp": "2017-02-08 17:27:47", "lastmod": "2020-03-10 23:25:54", "status_changed": "2017-02-13 20:10:21", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "aditya.kher@zoho.com", "id": "Kher-Aditya-Shreyas", "name": { "family": "Kher", "given": "Aditya Shreyas" }, "orcid": "0000-0002-5994-428X", "show_email": "NO" } ] }, "title": "Superconducting Nonlinear Kinetic Inductance Devices", "ispublished": "unpub", "full_text_status": "public", "keywords": "Superconducting devices; kinetic inductance; nonlinear; current sensor; magnetometer; amplifier; transition-edge sensors", "abstract": "We describe a novel class of devices based on the nonlinearity of the kinetic inductance of a superconducting thin film. By placing a current-dependent inductance in a microwave resonator, small currents can be measured through their effect on the resonator\u2019s frequency. By using a high-resistivity material for the film and nanowires as kinetic inductors, we can achieve a large coefficient of nonlinearity to improve device sensitivity. We demonstrate a current sensitivity of 8 pA/√Hz, making this device useful for transition-edge sensor (TES) readout and other cutting-edge applications. An advantage of these devices is their natural ability to be multiplexed in the frequency domain, enabling large detector arrays for TES-based instruments. A traveling-wave version of the device, consisting of a thin-film microwave transmission line, is also sensitive to small currents as they change the phase length of the line due to their effect on its inductance. We demonstrate a current sensitivity of 5 pA/√Hz for this version of the device, making it also suitable for TES readout as well as other current-detection applications. It has the advantage of multi-gigahertz bandwidth and greater dynamic range, offering a different approach to the resonator version of the device. Finally, we also demonstrate a transmission-line resonator version of the device that combines some of the advantages of the nanowire resonator and the traveling-wave device. This version of the device has high dynamic range but can also be easily multiplexed in the frequency domain.
\r\n\r\nA lumped-element resonator similar to the first device can be placed in a loop configuration to make it sensitive to magnetic fields. We demonstrate an example of such a device whose sensitivity could ultimately reach levels similar to those of state-of-the-art DC SQUIDs, making it potentially useful for many magnetometry applications given its ease of multiplexing. Finally, a similar microwave resonator is shown to exhibit parametric gain of up to 29 dB in the presence of a strong pump tone. The noise performance of this parametric amplifier approaches the quantum limit, making it useful for applications in quantum information and metrology.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:02062017-171647432", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:02062017-171647432", "related_url": { "items": [ { "description": "Topics in this paper are discussed in chapters 1-4 of the thesis", "type": "doi", "url": "http://dx.doi.org/10.1007/s10909-015-1364-0" } ] }, "referencetext": { "items": [ "[1] R. A. Alpher and R. Herman. \u201cEvolution of the Universe\u201d. Nature 162.4124,\r\n774\u2013775 (1948).\r\n\r\n[2] G. Gamow. \u201cThe Origin of Elements and the Separation of Galaxies\u201d.\r\nPhysical Review 74.4, 505\u2013506 (1948).\r\n\r\n[3] G. Gamow. \u201cThe Evolution of the Universe\u201d. Nature 162.4122, 680\u2013682\r\n(1948).\r\n\r\n[4] G. F. Smoot. \u201cCMB anisotropy experiments\u201d. Physics Reports 333, 269\u2013308\r\n(2000).\r\n\r\n[5] A. A. 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Physical Review\r\nD 26.8, 1817\u20131839 (1982)." ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Space Technology Research Fellowship", "grant_number": "NNX12AM42H" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Aditya Kher", "deposited_on": "2017-02-08 17:27:47", "doi": "10.7907/Z9JQ0Z1F", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "chair" }, { "email": "schwab@caltech.edu", "id": "Schwab-K-C", "name": { "family": "Schwab", "given": "Keith C." }, "role": "member" }, { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "role": "member" }, { "email": "sweinreb@caltech.edu", "id": "Weinreb-S", "name": { "family": "Weinreb", "given": "Sander" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-08-30", "gradofc_approval_date": "2017-02-10", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"0000-0003-3924-243X", "show_email": "YES" } ] }, "title": "The Search for Stellar Coronal Mass Ejections", "ispublished": "unpub", "full_text_status": "public", "keywords": "stellar flares; radio astronomy; coronal mass ejections; stellar radio bursts; stellar activity; stellar magnetism; planetary habitability", "abstract": "Coronal mass ejections (CMEs) may dramatically impact habitability and atmospheric composition of planets around magnetically active stars, including young solar analogs and many M dwarfs. Theoretical predictions of such effects are limited by the lack of observations of stellar CMEs. This thesis addresses this gap through a search for the spectral and spatial radio signatures of CMEs on active M dwarfs.
\r\n\r\nSolar CMEs produce radio bursts with a distinctive spectral signature, narrow-band plasma emission that drifts to lower frequency as a CME expands outward. To search for analogous events on nearby stars, I worked on system design, software, and commissioning for the Starburst project, a wideband single-baseline radio interferometry backend dedicated to stellar observations. In addition, I led a survey of nearby active M dwarfs with the Karl G. Jansky Very Large Array (VLA), detecting coherent radio bursts in 13 out of 23 epochs, over a total of 58 hours. This survey's ultra-wide bandwidth (0.23-6.0 GHz) dynamic spectroscopy, unprecedented for stellar observations, revealed diverse behavior in the time-frequency plane. Flare star UV Ceti produced complex, luminous events reminiscent of brown dwarf aurorae; AD Leo sustained long-duration, intense, narrow-band \"storms\"; and YZ CMi emitted a burst with substructure with rapid frequency drift, resembling solar Type III bursts, which are attributed to electrons moving at speeds of order 10% of the speed of light.
\r\n\r\nTo search for the spatial signature of CMEs, I led 8.5-GHz observations with the Very Long Baseline Array simultaneous to 24 hours of the VLA survey. This program detected non-thermal continuum emission from the stars in all epochs, as well as continuum flares on AD Leo and coherent bursts on UV Ceti, enabling measurement of the spatial offset between flaring and quiescent emission.
\r\n\r\nThese observations demonstrate the diversity of stellar transients that can be expected in time-domain radio surveys, especially with the advent of large low-frequency radio telescopes. Wide bandwidth radio dynamic spectroscopy, complemented by high-resolution imaging of the radio corona, is a powerful technique for detecting stellar eruptions and characterizing dynamic processes in the stellar corona.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:02022017-141014631", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:02022017-141014631", "related_url": { "items": [ { "description": "Article included as Ch. 2", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/788/2/112" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Foundation Graduate Research Fellowship" }, { "agency": "National Science Foundation", "grant_number": "AST-1311098" }, { "agency": "Troesh family graduate fellowship" }, { "agency": "PEO Scholar Award" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "suggestions": "Restricted to Caltech community only until 3 September 2017. // From author: Three of the thesis chapters are publications in preparation.// Released to public view 09132017", "deposited_by": "Jacqueline Villadsen", "deposited_on": "2017-03-13 22:20:54", "doi": "10.7907/Z9P55KGB", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "tjp@astro.caltech.edu", "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "Timothy J." }, "orcid": "0000-0001-5213-6231", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-12-16", "gradofc_approval_date": "2017-03-03", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/74411" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/74411" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/74411" } ] } } ], "eprint_status": "archive", "userid": 10971, "dir": "disk0/00/00/99/38", "datestamp": "2016-10-14 22:59:01", "lastmod": "2019-10-04 00:14:35", "status_changed": "2016-10-14 22:59:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jspineda119@gmail.com", "id": "Pineda-John-Sebastian", "name": { "family": "Pineda", "given": "John Sebastian" }, "orcid": "0000-0002-4489-0135", "show_email": "NO" } ] }, "title": "Multiwavelength Characterization of the Brown Dwarf Auroral Phenomenon - Establishing the Nature of the Electrodynamic Engine", "ispublished": "unpub", "full_text_status": "public", "keywords": "Brown Dwarfs; Aurorae; Magnetic Activity", "abstract": "Stellar coronal activity has been shown to persist into the low-mass star regime, down to late M-dwarf spectral types. However, there is now an accumulation of evidence suggesting that at the end of the main sequence there is a transition in the nature of the magnetic activity from chromospheric and coronal to planet-like and auroral, from local impulsive heating via flares and MHD wave dissipation to energy dissipation from strong large-scale magnetospheric current systems. In this dissertation, I examine the effects of these processes on the atmospheres of brown dwarfs across multiple different wavebands and investigate the underlying mechanisms powering the electrodynamic engine responsible for auroral emission in brown dwarfs. I conduct observational surveys looking for the emission features of H\u03b1 and H3+ as indicative of auroral systems across the ultracool dwarf regime. I further provide a comprehensive view of brown dwarf magnetic activity and auroral phenomena, detailing the various emission processes, and expectations for auroral brown dwarfs. I also initiate a preliminary analysis of the detailed emission features and discuss the constraints imposed on the electrodynamic engine of these objects. \r\n", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:10122016-095646319", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10122016-095646319", "related_url": { "items": [ { "description": "Article adapted for Appendix A", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/767/1/28" }, { "description": "Article adapted for ch. 3", "type": "doi", "url": "http://dx.doi.org/10.3847/0004-637X/826/1/73" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "John Pineda", "deposited_on": "2016-10-14 22:59:01", "doi": "10.7907/Z90C4SRW", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "chair" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "role": "member" }, { "email": "davy@ipac.caltech.edu", "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-09-14", "gradofc_approval_date": "2016-10-14", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/80313" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/80313" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/80313" } ] } } ], "eprint_status": "archive", "userid": 9713, "dir": "disk0/00/01/01/36", "datestamp": "2017-06-05 23:42:23", "lastmod": "2020-03-10 23:50:02", "status_changed": "2017-06-05 23:42:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "panlu1005@gmail.com", "id": "Pan-Lu", "name": { "family": "Pan", "given": "Lu" }, "orcid": "0000-0002-8151-2125", "show_email": "NO" } ] }, "title": "Insights into the Geologic History of Mars\u2019 Northern Lowlands from Near-Infrared Spectroscopy \r ", "ispublished": "unpub", "full_text_status": "public", "keywords": "Mars, spectroscopy, mineralogy, northern lowlands", "abstract": "Hydrated minerals, identified on Mars using near-infrared spectroscopy data, reveal new insights into the aqueous processes and evolution of climate in the history of Mars. Through investigations of the mineralogical record using near-infrared spectroscopy, this dissertation focuses on the geologic history and aqueous processes in the northern lowlands of Mars in order to assess the existence of a long-lived global ocean, the extent and volume of Noachian-Hesperian volcanic flows filling the northern lowlands, the nature of aqueous activity in the most recent Amazonian age, and the spectral variability of carbonates. The first chapter reports widespread and diverse mafic and hydrated mineralogy of units associated with impact craters across the northern lowlands. In the lowlands-wide survey, no pervasive carbonate or evaporative salts are found in support of a northern ocean, but we identify widespread phyllosilicates inferred to be Noachian basement materials excavated beneath 1-2 km of mafic lava flows. In the second and third chapters, combined analysis of imagery and spectral data is used to investigate local geologic processes related to liquid water in the knobby terrains of Acidalia and in the vicinity of Lyot crater. Phyllosilicates and hydrated silica are detected in the knobby terrains of Acidalia indicative of a declining prevalence of aqueous alteration through time. We also find diverse mineralogy in the vicinity of Lyot, probably formed in a hydrothermal system and later excavated by the Lyot impact. In contrast, we did not identify mineralization related to local channels that are syn- or post-impact. The fourth study analyzes the spectral properties of unshocked and impact-shocked carbonate rocks on Earth and found similar spectral characteristics between Mars carbonate detections and terrestrial carbonates in impact environments. Using near-infrared spectroscopy, we have identified and characterized the mineralogic record of Mars, and found past environments within the northern lowlands of Mars with varying style and intensity of aqueous alteration through time, with implications for the evolution of Mars climate.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:04132017-163326100", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04132017-163326100", "related_url": { "items": [ { "description": "Adapted for Chapter 3.", "type": "doi", "url": "http://dx.doi.org/10.1002/2014GL059423" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Files temporarily withheld until Jun 12, 2017 - released to public view 6/12/2017", "deposited_by": "Lu Pan", "deposited_on": "2017-06-05 23:42:23", "doi": "10.7907/Z94747WX", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "chair" }, { "email": "grr@gps.caltech.edu", "id": "Rossman-G-R", "name": { "family": "Rossman", "given": "George Robert" }, "role": "member" }, { "email": "grotz@gps.caltech.edu", "id": "Grotzinger-J-P", "name": { "family": "Grotzinger", "given": "John P." }, "role": "member" }, { "email": "ehlmann@caltech.edu", "id": "Ehlmann-B-L", "name": { "family": "Ehlmann", "given": "Bethany L." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-05-10", "gradofc_approval_date": "2017-06-05", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2017", "author_list": "Pan, Lu" }, { "id": "/id/eprint/10090", "eprint_id": 10090, "rev_number": 54, "documents": [ { "id": "/id/document/77502", "doc_id": 77502, "rev_number": 7, "files": [ { "id": "/id/file/219753", "fileid": 219753, "datasetid": "document", "objectid": 77502, "filename": "IAF_thesis.pdf", "mime_type": "application/pdf", "hash": "65005cea51462694ab37f5806e209a9b", "hash_type": "MD5", "filesize": 16172825, "mtime": "2017-04-18 00:48:01", "url": "/10090/1/IAF_thesis.pdf" } ], "eprint_id": 10090, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Full thesis", "language": "en", "security": "public", "license": "other", "main": "IAF_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/77562" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/77562" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/77562" } ] } } ], "eprint_status": "archive", "userid": 10994, "dir": "disk0/00/01/00/90", "datestamp": "2017-04-21 15:42:56", "lastmod": "2023-11-08 00:16:42", "status_changed": "2017-04-21 15:42:56", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ifinn505@gmail.com", "id": "Finneran-Ian-Alan", "name": { "family": "Finneran", "given": "Ian Alan" }, "orcid": "0000-0003-2506-4652", "show_email": "YES" } ] }, "title": "Terahertz and Microwave Spectroscopy of Liquids and Hydrogen-Bonded Clusters", "ispublished": "unpub", "full_text_status": "public", "keywords": "Chemical Physics, Molecular Clusters, Liquids, Ultrafast Laser Spectroscopy, Microwave Spectroscopy, Terahertz Spectroscopy, Coherent Two-Dimensional Spectroscopy, Frequency Comb Spectroscopy", "abstract": "The microwave (MW, 0.3-100 GHz) and terahertz (THz, 0.1-10 THz) regions of the electromagnetic spectrum are replete with a rich set of molecular motions, including soft inter- and intramolecular vibrations, torsions, and rotations. At room temperature these motions are well populated, and play an active role in condensed-phase chemistry on Earth. This work details the development of one MW and two THz spectrometers along with their application to the study of liquids and hydrogen-bonded clusters.
\r\n\r\nIn the first section, we cover the design and construction of a chirped pulse Fourier transform microwave (CP-FTMW) spectrometer. The instrument relies on a compact, inexpensive direct digital synthesis board to generate 2 GHz, 1 microsecond chirped pulses that, after amplification, polarize the rotational states of gas-phase molecules in a pulsed supersonic jet. In an initial demonstration, the CP-FTMW instrument is used to collect the 8-18 GHz rotational spectra of the ethanol-water and ethanol-methanol dimers. These data reveal evidence of quantum tunneling, and a complicated interplay between weak and strong hydrogen-bonds in both dimers.
\r\n\r\nNext, we describe the ongoing development of a decade spanning high precision THz frequency comb, using THz time-domain spectroscopy. The instrument is capable of generating ~28000 comb teeth from 0.15-2.4 THz with a fractional precision of 1.8x10-9 and a Doppler-limited accuracy of 6.1x10-8. Further prospects for studies of intermolecular interactions in jet-cooled molecular clusters are also discussed.
\r\n\r\nIn the last section, we move to condensed-phase studies of THz orientational and vibrational motions of liquids. The liquids are excited with one or two intense time-delayed ultrafast THz pulses and probed with a non-resonant 40 fs Raman pulse. Initially, we use this approach to measure the picosecond molecular orientational alignment and decay timescales in several aromatic liquids. By adding a second THz pulse to the experiment and adjusting the delays between the three pulses, we control the orientational alignment of the molecules, and acquire phase-coherent 2D-THz-THz-Raman spectra in the time domain. The 2D responses of liquid CHBr3, CCl4, and CCl2Br2 show off-diagonal peaks from coupling between thermally-populated vibrational modes. In an extended bandwidth measurement, we observe photon-echo signals from liquid CHBr3 and a complicated pattern of dipole forbidden transitions. The molecular origins of the forbidden transitions are still under investigation, but are likely due to nonlinearities in the condensed-phase dipole moment surface. Coherence transfer, vibrational anharmonicity, and intermolecular coupling are also considered in this analysis.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:03082017-151032634", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03082017-151032634", "related_url": { "items": [ { "description": "Article adapted for Ch. 2", "type": "doi", "url": "https://doi.org/10.1063/1.4818137" }, { "description": "Figure adapted for Ch. 2", "type": "doi", "url": "https://doi.org/10.1126/science.aae0328" }, { "description": "Figure adapted for Ch. 3", "type": "doi", "url": "https://doi.org/10.1016/j.jms.2015.02.003" }, { "description": "Article adapted for Ch. 3", "type": "doi", "url": "https://doi.org/10.1039/C5CP03589A" }, { "description": "Article adapted for Ch. 4", "type": "doi", "url": "https://doi.org/10.1039/C6CP03980D" }, { "description": "Article adapted for Ch. 5", "type": "doi", "url": "https://doi.org/10.1103/PhysRevLett.114.163902" }, { "description": "Experimental details for Ch. 5", "type": "doi", "url": "https://doi.org/10.1063/1.4932567" }, { "description": "Figures adapted for Ch. 6", "type": "doi", "url": "https://doi.org/10.1063/1.4938165" }, { "description": "Article adapted for Ch. 7", "type": "doi", "url": "https://doi.org/10.1073/pnas.1605631113" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released to public view 04162018. //\r\nRestricted to Caltech community only until 19 October 2017. // From author: We would like to publish some of the results and do not want our results to be 'scooped' by other groups.", "deposited_by": "Ian Finneran", "deposited_on": "2017-04-21 15:42:56", "doi": "10.7907/Z9348HD4", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jlbchamp@caltech.edu", "id": "Beauchamp-J-L", "name": { "family": "Beauchamp", "given": "Jesse L." }, "orcid": "0000-0001-8839-4822", "role": "chair" }, { "email": "mo@caltech.edu", "id": "Okumura-M", "name": { "family": "Okumura", "given": "Mitchio" }, "orcid": "0000-0001-6874-1137", "role": "member" }, { "email": "tfm@caltech.edu", "id": "Miller-T-F", "name": { "family": "Miller", "given": "Thomas F." }, "orcid": "0000-0002-1882-5380", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-03-01", "gradofc_approval_date": "2017-04-19", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2017", "author_list": "Finneran, Ian Alan" }, { "id": "/id/eprint/9906", "eprint_id": 9906, "rev_number": 30, "documents": [ { "id": "/id/document/73925", "doc_id": 73925, "rev_number": 4, "files": [ { "id": "/id/file/208369", "fileid": 208369, "datasetid": "document", "objectid": 73925, "filename": "thesis.pdf", "mime_type": "application/pdf", "hash": "7d5dd0405806766a3c815fa710f727a9", "hash_type": "MD5", "filesize": 8434177, "mtime": "2016-08-31 03:10:29", "url": "/9906/1/thesis.pdf" } ], "eprint_id": 9906, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete Thesis", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"uri": "/id/document/73925" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/73925" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/73925" } ] } } ], "eprint_status": "archive", "userid": 10952, "dir": "disk0/00/00/99/06", "datestamp": "2016-09-19 21:45:10", "lastmod": "2021-11-05 22:45:51", "status_changed": "2016-09-19 21:45:10", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "benmontet@gmail.com", "id": "Montet-Benjamin-Tyler", "name": { "family": "Montet", "given": "Benjamin Tyler" }, "orcid": "0000-0001-7516-8308", "show_email": "NO" } ] }, "title": "Low-Mass Stars and Their Companions", "ispublished": "unpub", "full_text_status": "public", "keywords": "Low-mass stars; brown dwarfs; exoplanets; statistics of planetary systems", "abstract": "In this thesis, I present seven studies aimed towards better understanding the demographics and physical properties of M dwarfs and their companions. These studies focus in turn on planetary, brown dwarf, and stellar companions to M dwarfs.
\r\n\r\nI begin with an analysis of radial velocity and transit timing analyses of multi-transiting planetary systems, finding that if both signals are measured to sufficiently high precision the stellar and planetary masses can be measured to a high precision, eliminating a need for stellar models which may have systematic errors. I then combine long-term radial velocity monitoring and a direct imaging campaign to measure the occurrence rate of giant planets around M dwarfs. I find that 6.5 +/- 3.0% of M dwarfs host a Jupiter mass or larger planet within 20 AU, with a strong dependence on stellar metallicity.
\r\n\r\nI then present two papers analyzing the LHS 6343 system, which contains a widely separated M dwarf binary (AB). Star A hosts a transiting brown dwarf (LHS 6343 C) with a 12.7 day period. By combining radial velocity data with transit photometry, I am able to measure the mass and radius of the brown dwarf to 2% precision, the most precise measurement of a brown dwarf to date. I then analyze four secondary eclipses of the LHS 6343 AC system as observed by Spitzer in order to measure the luminosity of the brown dwarf in both Spitzer bandpasses. I find the brown dwarf is consistent with theoretical models of an 1100 K T dwarf at an age of 5 Gyr and empirical observations of field T5-6 dwarfs with temperatures of 1070 +/- 130 K. This is the first non-inflated brown dwarf with a measured mass, radius, and multi-band photometry, making it an ideal test of evolutionary models of field brown dwarfs.
\r\n\r\nNext, I present the results of an astrometric and radial velocity campaign to measure the orbit and masses of both stars in the GJ 3305 AB system, an M+M binary comoving with 51 Eridani, a more massive star with a directly imaged planetary companion. I compare the masses of both stars to largely untested theoretical models of young M dwarfs, finding that the models are consistent with the measured mass of star A but slightly overpredict the luminosity of star B.
\r\n\r\nIn the final two science chapters I focus on space-based transit surveys, present and future. First, I present the first catalog of statistically validated planets from the K2 mission, as well as updated stellar and planetary parameters for all systems with candidate planets in the first K2 field. The catalog includes K2-18b, a ``mini-Neptune'' planet that receives a stellar insolation consistent with the level that the Earth receives from the Sun, making it a useful comparison against planets of a similar size that are highly irradiated, such as GJ 1214 b. Finally, I present predictions for the WFIRST mission. While designed largely as a microlensing mission, I find it will be able to detect as many as 30,000 transiting planets towards the galactic bulge, providing information about how planet occurrence changes across the galaxy. These planets will be able to be confirmed largely through direct detection of their secondary eclipses. Moreover, I find that more than 50% of the planets it detects smaller than Neptune will be found around M dwarf hosts.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:08292016-174647631", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08292016-174647631", "related_url": { "items": [ { "description": "Article adapted for ch. 2: \u201cModel-independent Stellar and Planetary Masses from Multi-transiting Exoplanetary Systems\u201d", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/762/2/112" }, { "description": "Article adapted for ch. 3: \u201cThe TRENDS High-contrast Imaging Survey. IV. The Occurrence Rate of Giant Planets around M Dwarfs\u201d", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/781/1/28" }, { "description": "Article adapted for ch. 4: \u201cCharacterizing the Cool KOIs. VII. Refined Physical Properties of the Transiting Brown Dwarf LHS 6343 C\u201d", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/800/2/134" }, { "description": "Article adapted for ch. 5: \u201cBenchmark Transiting Brown Dwarf LHS 6343 C: Spitzer Secondary Eclipse Observations Yield Brightness Temperature and mid-T Spectral Class\u201d", "type": "doi", "url": "http://dx.doi.org/10.3847/2041-8205/822/1/L6" }, { "description": "Article adapted for ch. 6: \u201cDynamical Masses of Young M Dwarfs: Masses and Orbital Parameters of GJ 3305 AB, the Wide Binary Companion to the Imaged Exoplanet Host 51 Eri\u201d", "type": "doi", "url": "http://dx.doi.org/10.1088/2041-8205/813/1/L11" }, { "description": "Article adapted for ch. 7: \u201cStellar and Planetary Properties of K2 Campaign 1 Candidates and Validation of 17 Planets, Including a Planet Receiving Earth-like Insolation\u201d", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/809/1/25" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Montet", "deposited_on": "2016-09-19 21:45:10", "doi": "10.7907/Z9KW5D1R", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jjohnson@cfa.harvard.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ghallinan@caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "chair" }, { "email": "jjohnson@cfa.harvard.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-07-18", "gradofc_approval_date": "2016-09-16", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2017", "author_list": "Montet, Benjamin Tyler" }, { "id": "/id/eprint/10280", "eprint_id": 10280, "rev_number": 54, "documents": [ { "id": "/id/document/80184", "doc_id": 80184, "rev_number": 4, "files": [ { "id": "/id/file/226546", "fileid": 226546, "datasetid": "document", "objectid": 80184, "filename": "schubert2011_permissions.pdf", "mime_type": "application/pdf", "hash": "89375f86fcaca6ab3f016fca897eaf9e", "hash_type": "MD5", "filesize": 438920, "mtime": "2017-06-05 18:16:51", "url": "/10280/1/schubert2011_permissions.pdf" } ], "eprint_id": 10280, "pos": 1, "placement": 3, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Schubert+ 2011", "language": "en", "security": "internal", "license": "other", "main": "schubert2011_permissions.pdf", "media_duration": "0", "media_aspect_ratio": "0", 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/87263" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/87263" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/87263" } ] } } ], "eprint_status": "archive", "userid": 9995, "dir": "disk0/00/01/02/80", "datestamp": "2017-06-07 00:23:33", "lastmod": "2023-05-30 22:23:56", "status_changed": "2017-06-07 00:23:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "melodie.kao@alum.mit.edu", "id": "Kao-Melodie-Minyu", "name": { "family": "Kao", "given": "Melodie Minyu" }, "orcid": "0000-0001-5125-1414", "show_email": "YES" } ] }, "title": "Constraining Substellar Magnetic Dynamos using Brown Dwarf Radio Aurorae", "ispublished": "unpub", "full_text_status": "public", "keywords": "Brown Dwarfs; Aurorae; Magnetic Activity, Dynamos", "abstract": "Brown dwarfs share characteristics with both low-mass stars and gas giant planets, making them useful laboratories for studying physics occurring in objects throughout this low mass and temperature range. Of particular interest in this dissertation is the nature of the engine driving their magnetic fields. Fully convective magnetic dynamos can operate in low mass stars, brown dwarfs, gas giant planets, and even fluid metal cores in small rocky planets. Objects in this wide mass range are capable of hosting strong magnetic fields, which shape much of the evolution of planets and stars: strong fields can protect planetary atmospheres from evaporating, generate optical and infrared emission that masquerade as clouds in the atmospheres of other worlds, and affect planet formation mechanisms. Thus, implications from understanding convective dynamo mechanisms also extend to exoplanet habitability.
\r\n\r\nHow the convective dynamos driving these fields operate remains an important open problem. While we have extensive data to inform models of magnetic dynamo mechanisms in higher mass stars like our Sun, the coolest and lowest-mass objects that probe the substellar-planetary boundary do not possess the internal structures necessary to drive solar-type dynamos. A number of models examining fully convective dynamo mechanisms have been proposed but they remain unconstrained by magnetic field measurements in the lowest end of the substellar mass and temperature space. Detections of highly circularly polarized pulsed radio emission provide our only window into magnetic field measurements for objects in the ultracool brown dwarf regime, but these detections are very rare; until this dissertation, only one attempt out of ~60 had been successful.
\r\n\r\nThe work presented in this dissertation seeks to address this problem and examines radio emission from late L, T, and Y spectral type brown dwarfs spanning ~1-6 times the surface temperature of Earth and explores implications for fully convective magnetic dynamo models.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:06052017-105748197", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06052017-105748197", "related_url": { "items": [ { "description": "Article adapted for Chapter 2, Chapter 3", "type": "doi", "url": "https://doi.org/10.3847/0004-637X/818/1/24" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Radio Astronomy Observatory Grote Reber fellowship" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Split committee decision - continuing embargo until dispute resolved 05072018 //\r\nExtension request submitted 03192018 //\r\nRestricted to Caltech community only until 6 December 2017. //\r\n\r\nFrom author: I am awaiting copyright permissions from 3 authors / publishers. I have uploaded all other copyright permissions in a ZIP file. I included two versions of my thesis: \r\n\r\nkao_Melodie_2017.pdf: (Final thesis version) Version that I would like to use, includes an excerpt from Invisible Cities, by Italo Calvino.\r\n\r\nkao_Melodie_2017_noCalvino.pdf: Alternate version without excerpt from Invisible Cities, in case I do not receive permission to reprint the material. This version has two figure permissions outstanding through the American Astronomical Society, but I am certain to receive permissions for those figures.", "deposited_by": "Melodie Kao", "deposited_on": "2017-06-07 00:23:33", "doi": "10.7907/Z9J964DK", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-05-30", "gradofc_approval_date": "2017-06-06", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2017", "author_list": "Kao, Melodie Minyu" }, { "id": "/id/eprint/10303", "eprint_id": 10303, "rev_number": 33, "documents": [ { "id": "/id/document/80819", "doc_id": 80819, "rev_number": 4, "files": [ { "id": "/id/file/228158", "fileid": 228158, "datasetid": "document", "objectid": 80819, "filename": "Nicole Thesis June.pdf", "mime_type": "application/pdf", "hash": "382673cc500d7631c6fd8c4454ea65ac", "hash_type": "MD5", "filesize": 50265144, "mtime": "2017-06-07 16:23:07", "url": "/10303/1/Nicole Thesis June.pdf" } ], "eprint_id": 10303, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Nicole Thesis June.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/80819" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/80819" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/80819" } ] } } ], "eprint_status": "archive", "userid": 11256, "dir": "disk0/00/01/03/03", "datestamp": "2017-06-07 21:19:32", "lastmod": "2020-03-10 22:56:35", "status_changed": "2017-06-07 21:19:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "sparklingnili@yahoo.com", "id": "Lingner-Nicole-Renate", "name": { "family": "Lingner", "given": "Nicole Renate" }, "show_email": "YES" } ] }, "title": "The Faint Intergalactic-Medium Redshifted Emission Balloon: FIREBall-2 Scientific Camera and Cooling System", "ispublished": "unpub", "full_text_status": "public", "keywords": "detectors; cryogenically cooled detectors; photon counting detectors; UV;", "abstract": "The FIREBall-2 instrument provides a means of investigating both the processes responsible for building cosmic structure and the galaxies that trace it. By studying the inflow and outflow of gaseous hydrogen, we can better explain galaxy formation and evolution. Each individual galaxy lies within a dense gaseous region called the circumgalactic medium (CGM), itself surrounded by the diffuse intergalactic medium (IGM). Thin gaseous filaments connect galaxies to each other in space and time and they can be found at nodes of these filaments at the center of dark matter halos.
\r\n\r\nThis large-scale structure, called the cosmicweb, has been modeled and corroborated with absorption line studies. To understand the structure of the galaxy environment, we need to map the extremely faint emission from the CGM and these filaments.
\r\n\r\nFIREBall-2 is a 1-meter-class, balloon-borne, UV telescope that will be launched from Texas in the fall of 2017. The instrument includes a vacuum tank, which houses an all-reflective, wide-field multislit spectrograph, guide camera, and UV optimized EMCCD sensor. The scientific camera sensor has to be operated near -110\u00b0C and is cooled with a mechanical cryocooler, which also powers a charcoal getter to maintain high vacuum during flight.
\r\n\r\nThe scientific camera includes a Printed Circuit Board (PCB), which I use as a rigid harness that holds the sensor in place. The sensor (CCD201-20 from e2v) is a delta-doped, electron-multiplying charge-coupled device (EMCCD) that has been modified to be used as a 1K x 2K (1024 x 2048 pixels) sensor. The EMCCD has been developed at the Jet Propulsion Laboratory\u2019s Micro Devices Laboratory. I operate this next-generation UV detector (NEXUS) at 10 MHz with read-out electronics from Nu\u0308vu\u0308 Cam\u0113ras. Nu\u0308vu\u0308\u2019s controller for counting photons (CCCP) was chosen to achieve extremely low detector noise by reducing clock induced charge (CIC) and it is attached to the PCB with a SAMTEC EQCD high-speed coaxial cable. To reduce dark current, the other relevant detector noise source, the EMCCD is supported by a gold-plated copper clamp and cooled with a CryoTel MT mechanical cooler (Stirling engine) from Sunpower. The CCD operating temperature is -110\u00b0C, with a required heat lift of about 7 Watts at a 30\u00b0C reject temperature. Two 10-Watt Omega heaters are used to regulate the temperature. The cryocooler will be operated at a constant input cooling power of about 70 Watts, which corresponds to 110-Watts of battery power. The cooler is mounted to the side of the vacuum tank and I have incorporated the Sunpower active vibration cancellation system (AVC) to reduce the vibrational noise. A flexible copper ribbon conducts heat from the bottom of the CCD via the solid copper clamp. The detector is operated in a vacuum of about 10-6 Torr, initially started by a turbo pump, with the pressure then lowered and maintained by activated charcoal adsorption during flight. The flight hardware has been integrated into the flight vacuum tank and is currently undergoing testing.
", "date": "2017", "date_type": "degree", "id_number": "CaltechTHESIS:06062017-165519688", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06062017-165519688", "projects": { "items": [ "FIREBall-2" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Files temporarily withheld until Jun 14, 2017 - released to public view 6/15/2017", "deposited_by": "Nicole Lingner", "deposited_on": "2017-06-07 21:19:32", "doi": "10.7907/Z9QV3JKQ", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "role": "chair" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "role": "member" }, { "email": "seancarroll@gmail.com", "id": "Carroll-S-M", "name": { "family": "Carroll", "given": "Sean M." }, "role": "member" }, { "email": "bale@ssl.berkeley.edu", "id": "Bale-Stuart-D", "name": { "family": "Bale", "given": "Stuart" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2017-04-26", "gradofc_approval_date": "2017-06-07", "thesis_awards": "Kanel Foundation Scholarship", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2017", "author_list": "Lingner, Nicole Renate" }, { "id": "/id/eprint/9238", "eprint_id": 9238, "rev_number": 30, "documents": [ { "id": "/id/document/61802", "doc_id": 61802, "rev_number": 2, "files": [ { "id": "/id/file/173116", "fileid": 173116, "datasetid": "document", "objectid": 61802, "filename": "siegel_seth_2016_thesis.pdf", "mime_type": "application/pdf", "hash": "4862dfbd1f389638deff1e2eb14ee2b4", "hash_type": "MD5", "filesize": 29094572, "mtime": "2015-10-27 21:11:16", "url": "/9238/1/siegel_seth_2016_thesis.pdf" } ], "eprint_id": 9238, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "siegel_seth_2016_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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and millimeter-wave astronomical instrumentation; microwave kinetic inductance detectors", "abstract": "The first part of this thesis combines Bolocam observations of the thermal Sunyaev-Zel\u2019dovich (SZ) effect at 140 GHz with X-ray observations from Chandra, strong lensing data from the Hubble Space Telescope (HST), and weak lensing data from HST and Subaru to constrain parametric models for the distribution of dark and baryonic matter in a sample of six massive, dynamically relaxed galaxy clusters. For five of the six clusters, the full multiwavelength dataset is well described by a relatively simple model that assumes spherical symmetry, hydrostatic equilibrium, and entirely thermal pressure support. The multiwavelength analysis yields considerably better constraints on the total mass and concentration compared to analysis of any one dataset individually. The subsample of five galaxy clusters is used to place an upper limit on the fraction of pressure support in the intracluster medium (ICM) due to nonthermal processes, such as turbulent and bulk flow of the gas. We constrain the nonthermal pressure fraction at r500c to be less than 0.11 at 95% confidence, where r500c refers to radius at which the average enclosed density is 500 times the critical density of the Universe. This is in tension with state-of-the-art hydrodynamical simulations, which predict a nonthermal pressure fraction of approximately 0.25 at r500c for the clusters in this sample.
\r\n\r\nThe second part of this thesis focuses on the characterization of the Multiwavelength Sub/millimeter Inductance Camera (MUSIC), a photometric imaging camera that was commissioned at the Caltech Submillimeter Observatory (CSO) in 2012. MUSIC is designed to have a 14 arcminute, diffraction-limited field of view populated with 576 spatial pixels that are simultaneously sensitive to four bands at 150, 220, 290, and 350 GHz. It is well-suited for studies of dusty star forming galaxies, galaxy clusters via the SZ Effect, and galactic star formation. MUSIC employs a number of novel detector technologies: broadband phased-arrays of slot dipole antennas for beam formation, on-chip lumped element filters for band definition, and Microwave Kinetic Inductance Detectors (MKIDs) for transduction of incoming light to electric signal. MKIDs are superconducting micro-resonators coupled to a feedline. Incoming light breaks apart Cooper pairs in the superconductor, causing a change in the quality factor and frequency of the resonator. This is read out as amplitude and phase modulation of a microwave probe signal centered on the resonant frequency. By tuning each resonator to a slightly different frequency and sending out a superposition of probe signals, hundreds of detectors can be read out on a single feedline. This natural capability for large scale, frequency domain multiplexing combined with relatively simple fabrication makes MKIDs a promising low temperature detector for future kilopixel sub/millimeter instruments. There is also considerable interest in using MKIDs for optical through near-infrared spectrophotometry due to their fast microsecond response time and modest energy resolution. In order to optimize the MKID design to obtain suitable performance for any particular application, it is critical to have a well-understood physical model for the detectors and the sources of noise to which they are susceptible. MUSIC has collected many hours of on-sky data with over 1000 MKIDs. This work studies the performance of the detectors in the context of one such physical model. Chapter 2 describes the theoretical model for the responsivity and noise of MKIDs. Chapter 3 outlines the set of measurements used to calibrate this model for the MUSIC detectors. Chapter 4 presents the resulting estimates of the spectral response, optical efficiency, and on-sky loading. The measured detector response to Uranus is compared to the calibrated model prediction in order to determine how well the model describes the propagation of signal through the full instrument. Chapter 5 examines the noise present in the detector timestreams during recent science observations. Noise due to fluctuations in atmospheric emission dominate at long timescales (less than 0.5 Hz). Fluctuations in the amplitude and phase of the microwave probe signal due to the readout electronics contribute significant 1/f and drift-type noise at shorter timescales. The atmospheric noise is removed by creating a template for the fluctuations in atmospheric emission from weighted averages of the detector timestreams. The electronics noise is removed by using probe signals centered off-resonance to construct templates for the amplitude and phase fluctuations. The algorithms that perform the atmospheric and electronic noise removal are described. After removal, we find good agreement between the observed residual noise and our expectation for intrinsic detector noise over a significant fraction of the signal bandwidth.
", "date": "2016", "date_type": "degree", "id_number": "CaltechTHESIS:10212015-211417853", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10212015-211417853", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "NASA Earth and Space Science Fellowship" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Seth Siegel", "deposited_on": "2015-10-27 21:23:32", "doi": "10.7907/Z9Z31WJ7", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "chair" }, { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "member" }, { "email": "James.Bartlett@jpl.nasa.gov", "id": "Bartlett-J", "name": { "family": "Bartlett", "given": "James" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-07-14", "gradofc_approval_date": "2015-10-27", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2016", "author_list": "Siegel, Seth Robert" }, { "id": "/id/eprint/9719", "eprint_id": 9719, "rev_number": 28, "documents": [ { "id": "/id/document/66439", "doc_id": 66439, "rev_number": 2, "files": [ { "id": "/id/file/185163", "fileid": 185163, "datasetid": "document", "objectid": 66439, "filename": "yi_cao_2016_thesis.pdf", "mime_type": "application/pdf", "hash": "eee1cbbd84691a923ace0f695338f387", "hash_type": "MD5", "filesize": 15900563, "mtime": "2016-05-18 02:36:14", "url": "/9719/1/yi_cao_2016_thesis.pdf" } ], "eprint_id": 9719, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "yi_cao_2016_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/66439" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/66439" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/66439" } ] } } ], "eprint_status": "archive", "userid": 6706, "dir": "disk0/00/00/97/19", "datestamp": "2016-05-19 21:18:57", "lastmod": "2020-01-23 21:46:45", "status_changed": "2016-05-19 21:18:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "smartcaoyi@gmail.com", "id": "Cao-Yi", "name": { "family": "Cao", "given": "Yi" }, "orcid": "0000-0002-8036-8491", "show_email": "NO" } ] }, "title": "Cosmic Explosions: Observations Of Infant Hydrogen-Free Supernovae Towards An Understanding Of Their Parent Systems", "ispublished": "unpub", "full_text_status": "public", "keywords": "methods: observational; surveys; optical; ultraviolet; image processing; extragalactic: stars; supernovae; white dwarfs; massive stars; ", "abstract": "Radiation in the first days of supernova explosions contains rich information about physical properties of the exploding stars. In the past three years, I used the intermediate Palomar Transient Factory to conduct one-day cadence surveys, in order to systematically search for infant supernovae. I show that the one-day cadences in these surveys were strictly controlled, that the realtime image subtraction pipeline managed to deliver transient candidates within ten minutes of images being taken, and that we were able to undertake follow-up observations with a variety of telescopes within hours of transients being discovered. So far iPTF has discovered over a hundred supernovae within a few days of explosions, forty-nine of which were spectroscopically classified within twenty-four hours of discovery.
\r\n\r\nOur observations of infant Type Ia supernovae provide evidence for both the single-degenerate and double-degenerate progenitor channels. On the one hand, a low-velocity Type Ia supernova iPTF14atg revealed a strong ultraviolet pulse within four days of its explosion. I show that the pulse is consistent with the expected emission produced by collision between the supernova ejecta and a companion star, providing direct evidence for the single degenerate channel. By comparing the distinct early-phase light curves of iPTF14atg to an otherwise similar event iPTF14dpk, I show that the viewing angle dependence of the supernova-companion collision signature is probably responsible to the difference of the early light curves. I also show evidence for a dark period between the supernova explosion and the first light of the radioactively-powered light curve. On the other hand, a peculiar Type Ia supernova iPTF13asv revealed strong near-UV emission and absence of iron in the spectra within the first two weeks of explosion, suggesting a stratified ejecta structure with iron group elements confined to the slow-moving part of the ejecta. With its total ejecta mass estimated to exceed the Chandrasekhar limit, I show that the stratification and large mass of the ejecta favor the double-degenerate channel.
\r\n\r\nIn a separate approach, iPTF found the first progenitor system of a Type Ib supernova iPTF13bvn in the pre-explosion HST archival mages. Independently, I used the early-phase optical observations of this supernova to constrain its progenitor radius to be no larger than several solar radii. I also used its early radio detections to derive a mass loss rate of 3e-5 solar mass per year for the progenitor right before the supernova explosion. These constraints on the physical properties of the iPTF13bvn progenitor provide a comprehensive data set to test Type Ib supernova theories. A recent HST revisit to the iPTF13bvn site two years after the supernova explosion has confirmed the progenitor system.
\r\n\r\nMoving forward, the next frontier in this area is to extend these single-object analyses to a large sample of infant supernovae. The upcoming Zwicky Transient Facility with its fast survey speed, which is expected to find one infant supernova every night, is well positioned to carry out this task.
\r\n", "date": "2016", "date_type": "degree", "id_number": "CaltechTHESIS:05142016-213503805", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05142016-213503805", "related_url": { "items": [ { "description": "Article adapted for Chapter 3", "type": "doi", "url": "http://dx.doi.org/10.1038/nature14440" }, { "description": "Article adapted for Chapter 6", "type": "doi", "url": "http://dx.doi.org/10.1088/2041-8205/775/1/L7" }, { "description": "Article adapted for the appendix chapter", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/752/2/133" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Yi Cao", "deposited_on": "2016-05-19 21:18:57", "doi": "10.7907/Z9XD0ZNT", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" }, { "email": "penugent@lbl.gov", "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "penugent@lbl.gov", "id": "Nugent-P-E", "name": { "family": "Nugent", "given": "Peter E." }, "role": "member" }, { "email": "prince@srl.caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-05-03", "gradofc_approval_date": "2016-05-19", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2016", "author_list": "Cao, Yi" }, { "id": "/id/eprint/9777", "eprint_id": 9777, "rev_number": 46, "documents": [ { "id": "/id/document/69056", "doc_id": 69056, "rev_number": 4, "files": [ { "id": "/id/file/189728", "fileid": 189728, "datasetid": "document", "objectid": 69056, "filename": "su_zhan_2016.pdf", "mime_type": "application/pdf", "hash": "8aab5107cd6cc077c5646b3d342943cf", "hash_type": "MD5", "filesize": 13792756, "mtime": "2016-05-31 22:22:23", "url": "/9777/7/su_zhan_2016.pdf" } ], "eprint_id": 9777, "pos": 7, "placement": 7, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "su_zhan_2016.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/69057", 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/69056" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/69056" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/69056" } ] } } ], "eprint_status": "archive", "userid": 10801, "dir": "disk0/00/00/97/77", "datestamp": "2016-06-01 17:17:16", "lastmod": "2020-03-11 18:42:30", "status_changed": "2016-06-01 17:17:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "zhanfluid@gmail.com", "id": "Su-Zhan", "name": { "family": "Su", "given": "Zhan" }, "orcid": "0000-0001-7603-7211", "show_email": "NO" } ] }, "title": "High-Latitude Ocean Convection and Gyre Dynamics", "ispublished": "unpub", "full_text_status": "public", "keywords": "ocean dynamics, ocean turbulence, ocean deep convection, gyre dynamics, ocean heat/freshwater transport, abrupt climate change", "abstract": "High-latitude ocean deep convection substantially contributes to vertical mixing, vertical heat transport, deep-water formation, and sea-ice budget in the World Ocean. However, the extent of this contribution remains poorly constrained. The concept of ocean convective available potential energy (OCAPE) have been developed to improve the understanding and the prediction for these deep convection events. The kinetic energy (KE) budget of deep convection is explored analytically and numerically based on the observations in the Weddell Sea. OCAPE, which is derived from thermobaricity, is identified as a critical KE source to power ocean deep convection. Other significant contributions to the energetics of convection, including diabatic processes related to cabbeling and stratification, are also carefully quantified. An associated theory is developed to predict the maximum depth of convection. This work may provide a useful basis for improving the convection parameterization in ocean models.
\r\n\r\nAs an application of the theory above, basin-scale OCAPE is found to be significantly built up in the North Atlantic at the end of Heinrich Stadial 1 (~17,000 years ago). This OCAPE is ultimately released to power strong ocean deep convection in North Atlantic as simulated by numerical models. This causes a ~2 \u00b0C sea surface warming for the whole basin (~700 km) within a month and exposes a huge heat reservoir to the atmosphere. This may invigorate the Atlantic meridional overturning circulation and provide an important mechanism to explain the abrupt Bolling-Allerod warming.
\r\n\r\nMesoscale turbulence is another crucial process for high-latitude ocean dynamics. From the physical nature of baroclinic instability, the framework of eddy-size- constrained Available Potential Energy (APE) density is developed, which is capable of well-detecting individual eddies and local eddy kinetic energy (EKE) in the World Ocean. This new framework is likely useful in parameterizing mesoscale eddies in ocean GCMs. Mesoscale turbulence are found to be coupled to the wind-driven Ekman pumping in determining the temperature and salinity budgets in subpolar gyres such as the Weddell Gyre. A conceptual model of the evolution of isopycnals has been developed in which the isopycnal responds to a seasonal oscillation in the surface wind stress. The model accurately predicts the observed phases of the temperature and salinity variability in relationship to the surface wind stress. The model, despite its heavy idealization, also accounts for more than 50% of the observed oscillation amplitude, which depends on the strength of the seasonal wind variability and the parameterized eddy diffusivity. These results highlight the importance of mesoscale eddies in modulating the export of AABW in narrow boundary layers around the Antarctic margins.
", "date": "2016", "date_type": "degree", "id_number": "CaltechTHESIS:05262016-174848616", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05262016-174848616", "related_url": { "items": [ { "description": "Article adapted for ch. 1", "type": "doi", "url": "http://dx.doi.org/10.1175/JPO-D-14-0155.1" }, { "description": "Article adapted for ch. 2", "type": "doi", "url": "http://dx.doi.org/10.1175/JPO-D-14-0156.1" }, { "description": "Article adapted for ch. 3", "type": "doi", "url": "http://dx.doi.org/10.1175/JCLI-D-15-0675.1" }, { "description": "Article adapted for ch. 4", "type": "doi", "url": "http://dx.doi.org/10.1175/JPO-D-16-0074.1" }, { "description": "Article adapted for ch. 5", "type": "doi", "url": "http://dx.doi.org/10.1175/JPO-D-13-0263.1" }, { "description": "Information-rich spectral channels for simulated retrievals of partial column-averaged methane", "type": "related", "url": "http://dx.doi.org/10.1002/2015EA000120" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Zhan Su", "deposited_on": "2016-06-01 17:17:16", "doi": "10.7907/Z9H12ZZ3", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" }, { "email": "andrewt@caltech.edu", "id": "Thompson-A-F", "name": { "family": "Thompson", "given": "Andrew F." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "andrewt@caltech.edu", "id": "Thompson-A-F", "name": { "family": "Thompson", "given": "Andrew F." }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "email": "Jess@gps.caltech.edu", "id": "Adkins-J-F", "name": { "family": "Adkins", "given": "Jess F." }, "role": "member" }, { "email": "astewart@atmos.ucla.edu", "id": "Stewart-A-L", "name": { "family": "Stewart", "given": "Andrew L." }, "role": "member" }, { "email": "Dimitris.Menemenlis@jpl.nasa.gov", "id": "Menemenlis-D", "name": { "family": "Menemenlis", "given": "Dimitris" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-05-13", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2016", "author_list": "Su, Zhan" }, { "id": "/id/eprint/9750", "eprint_id": 9750, "rev_number": 27, "documents": [ { "id": "/id/document/68180", "doc_id": 68180, "rev_number": 2, "files": [ { "id": "/id/file/187611", "fileid": 187611, "datasetid": "document", "objectid": 68180, "filename": "jgood_thesis.pdf", "mime_type": "application/pdf", "hash": "06995783e60982058e856b5e577c202b", "hash_type": "MD5", "filesize": 3074066, "mtime": "2016-05-25 21:37:02", "url": "/9750/1/jgood_thesis.pdf" } ], "eprint_id": 9750, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "jgood_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/68181", 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/68180" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/68180" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/68180" } ] } } ], "eprint_status": "archive", "userid": 10856, "dir": "disk0/00/00/97/50", "datestamp": "2016-05-25 23:35:16", "lastmod": "2023-11-08 00:16:42", "status_changed": "2016-05-25 23:35:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jacob.thomas.good@gmail.com", "id": "Good-Jacob-Thomas", "name": { "family": "Good", "given": "Jacob Thomas" }, "show_email": "NO" } ] }, "title": "Design and Applications of a Decade-Spanning Terahertz Frequency Comb Spectrometer: Doppler-limited Rotational Spectroscopy of Methanol and Methanol-OD", "ispublished": "unpub", "full_text_status": "public", "keywords": "molecular spectroscopy; frequency combs; time-domain spectroscopy; methanol; asynchronous optical sampling", "abstract": "This thesis details the design and applications of a terahertz (THz) frequency comb spectrometer. The spectrometer employs two offset locked Ti:Sapphire femtosecond oscillators with repetition rates of approximately 80 MHz, offset locked at 100 Hz to continuously sample a time delay of 12.5 ns at a maximum time delay resolution of 15.6 fs. These oscillators emit continuous pulse trains, allowing the generation of a THz pulse train by the master, or pump, oscillator and the sampling of this THz pulse train by the slave, or probe, oscillator via the electro-optic effect. Collecting a train of 16 consecutive THz pulses and taking the Fourier transform of this pulse train produces a decade-spanning frequency comb, from 0.25 to 2.5 THz, with a comb tooth width of 5 MHz and a comb tooth spacing of ~80 MHz. This frequency comb is suitable for Doppler-limited rotational spectroscopy of small molecules. Here, the data from 68 individual scans at slightly different pump oscillator repetition rates were combined, producing an interleaved THz frequency comb spectrum, with a maximum interval between comb teeth of 1.4 MHz, enabling THz frequency comb spectroscopy.
\r\n\r\nThe accuracy of the THz frequency comb spectrometer was tested, achieving a root mean square error of 92 kHz measuring selected absorption center frequencies of water vapor at 10 mTorr, and a root mean square error of 150 kHz in measurements of a K-stack of acetonitrile. This accuracy is sufficient for fitting of measured transitions to a model Hamiltonian to generate a predicted spectrum for molecules of interest in the fields of astronomy and physical chemistry. As such, the rotational spectra of methanol and methanol-OD were acquired by the spectrometer. Absorptions from 1.3 THz to 2.0 THz were compared to JPL catalog data for methanol and the spectrometer achieved an RMS error of 402 kHz, improving to 303 kHz when excluding low signal-to-noise absorptions. This level of accuracy compares favorably with the ~100 kHz accuracy achieved by JPL frequency multiplier submillimeter spectrometers. Additionally, the relative intensity performance of the THz frequency comb spectrometer is linear across the entire decade-spanning bandwidth, making it the preferred instrument for recovering lineshapes and taking absolute intensity measurements in the THz region. The data acquired by the Terahertz Frequency Comb Spectrometer for methanol-OD is of comparable accuracy to the methanol data and may be used to refine the fit parameters for the predicted spectrum of methanol-OD.
", "date": "2016", "date_type": "degree", "id_number": "CaltechTHESIS:05252016-124438217", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05252016-124438217", "related_url": { "items": [ { "description": "Article adapted for Ch 1,2,4,5, and 6", "type": "doi", "url": "https://doi.org/10.1063/1.4932567" }, { "description": "Article adapted for Ch 5, and 6", "type": "doi", "url": "https://doi.org/10.1103/PhysRevLett.114.163902" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Jacob Good", "deposited_on": "2016-05-25 23:35:16", "doi": "10.7907/Z9MW2F37", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "hbgray@caltech.edu", "id": "Gray-H-B", "name": { "family": "Gray", "given": "Harry B." }, "orcid": "0000-0002-7937-7876", "role": "chair" }, { "email": "mo@caltech.edu", "id": "Okumura-M", "name": { "family": "Okumura", "given": "Mitchio" }, "orcid": "0000-0001-6874-1137", "role": "member" }, { "email": "heath@caltech.edu", "id": "Heath-J-R", "name": { "family": "Heath", "given": "James R." }, "orcid": "0000-0001-5356-4385", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-03-18", "gradofc_approval_date": "2016-05-25", "review_status": "gradoffice", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2016", "author_list": "Good, Jacob Thomas" }, { "id": "/id/eprint/9243", "eprint_id": 9243, "rev_number": 40, "documents": [ { "id": "/id/document/61861", "doc_id": 61861, "rev_number": 3, "files": [ { "id": "/id/file/173251", "fileid": 173251, "datasetid": "document", "objectid": 61861, "filename": "thesis_SirioBelli.pdf", "mime_type": "application/pdf", "hash": "d76e7e68bba74a21468039d4484e92b0", "hash_type": "MD5", "filesize": 15500692, "mtime": "2015-10-29 10:14:58", "url": "/9243/7/thesis_SirioBelli.pdf" } ], "eprint_id": 9243, "pos": 7, "placement": 7, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete Thesis", "language": "en", "security": "public", "license": "other", "main": "thesis_SirioBelli.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/61861" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/61861" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/61861" } ] } } ], "eprint_status": "archive", "userid": 10694, "dir": "disk0/00/00/92/43", "datestamp": "2015-11-09 17:24:06", "lastmod": "2021-11-05 22:46:40", "status_changed": "2015-11-09 17:24:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "sirbelli@gmail.com", "id": "Belli-Sirio", "name": { "family": "Belli", "given": "Sirio" }, "orcid": "0000-0002-5615-6018", "show_email": "NO" } ] }, "title": "Deep Near-Infrared Spectroscopy of High-Redshift Galaxies: the Physical Growth of Passive Systems", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxy evolution; high-redshift galaxies; stellar dynamics; galaxy structure; galaxy metallicity", "abstract": "The assembly history of massive galaxies is one of the most important aspects of galaxy formation and evolution. Although we have a broad idea of what physical processes govern the early phases of galaxy evolution, there are still many open questions. In this thesis I demonstrate the crucial role that spectroscopy can play in a physical understanding of galaxy evolution. I present deep near-infrared spectroscopy for a sample of high-redshift galaxies, from which I derive important physical properties and their evolution with cosmic time. I take advantage of the recent arrival of efficient near-infrared detectors to target the rest-frame optical spectra of z > 1 galaxies, from which many physical quantities can be derived. After illustrating the applications of near-infrared deep spectroscopy with a study of star-forming galaxies, I focus on the evolution of massive quiescent systems.
\r\n\r\nMost of this thesis is based on two samples collected at the W. M. Keck Observatory that represent a significant step forward in the spectroscopic study of z > 1 quiescent galaxies. All previous spectroscopic samples at this redshift were either limited to a few objects, or much shallower in terms of depth. Our first sample is composed of 56 quiescent galaxies at 1 < z < 1.6 collected using the upgraded red arm of the Low Resolution Imaging Spectrometer (LRIS). The second consists of 24 deep spectra of 1.5 < z < 2.5 quiescent objects observed with the Multi-Object Spectrometer For Infra-Red Exploration (MOSFIRE). Together, these spectra span the critical epoch 1 < z < 2.5, where most of the red sequence is formed, and where the sizes of quiescent systems are observed to increase significantly.
\r\n\r\nWe measure stellar velocity dispersions and dynamical masses for the largest number of z > 1 quiescent galaxies to date. By assuming that the velocity dispersion of a massive galaxy does not change throughout its lifetime, as suggested by theoretical studies, we match galaxies in the local universe with their high-redshift progenitors. This allows us to derive the physical growth in mass and size experienced by individual systems, which represents a substantial advance over photometric inferences based on the overall galaxy population. We find a significant physical growth among quiescent galaxies over 0 < z < 2.5 and, by comparing the slope of growth in the mass-size plane dlogRe/dlogM\u2217 with the results of numerical simulations, we can constrain the physical process responsible for the evolution. Our results show that the slope of growth becomes steeper at higher redshifts, yet is broadly consistent with minor mergers being the main process by which individual objects evolve in mass and size.
\r\n\r\nBy fitting stellar population models to the observed spectroscopy and photometry we derive reliable ages and other stellar population properties. We show that the addition of the spectroscopic data helps break the degeneracy between age and dust extinction, and yields significantly more robust results compared to fitting models to the photometry alone. We detect a clear relation between size and age, where larger galaxies are younger. Therefore, over time the average size of the quiescent population will increase because of the contribution of large galaxies recently arrived to the red sequence. This effect, called progenitor bias, is different from the physical size growth discussed above, but represents another contribution to the observed difference between the typical sizes of low- and high-redshift quiescent galaxies. By reconstructing the evolution of the red sequence starting at z \u223c 1.25 and using our stellar population histories to infer the past behavior to z \u223c 2, we demonstrate that progenitor bias accounts for only half of the observed growth of the population. The remaining size evolution must be due to physical growth of individual systems, in agreement with our dynamical study.
\r\n\r\nFinally, we use the stellar population properties to explore the earliest periods which led to the formation of massive quiescent galaxies. We find tentative evidence for two channels of star formation quenching, which suggests the existence of two independent physical mechanisms. We also detect a mass downsizing, where more massive galaxies form at higher redshift, and then evolve passively. By analyzing in depth the star formation history of the brightest object at z > 2 in our sample, we are able to put constraints on the quenching timescale and on the properties of its progenitor.
\r\n\r\nA consistent picture emerges from our analyses: massive galaxies form at very early epochs, are quenched on short timescales, and then evolve passively. The evolution is passive in the sense that no new stars are formed, but significant mass and size growth is achieved by accreting smaller, gas-poor systems. At the same time the population of quiescent galaxies grows in number due to the quenching of larger star-forming galaxies. This picture is in agreement with other observational studies, such as measurements of the merger rate and analyses of galaxy evolution at fixed number density.
", "date": "2016", "date_type": "degree", "id_number": "CaltechTHESIS:10232015-070212778", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10232015-070212778", "related_url": { "items": [ { "description": "Article adapted for Chapter 2", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/772/2/141" }, { "description": "Article adapted for Chapter 3", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/783/2/117" }, { "description": "Article adapted for Chapter 4", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/799/2/206" }, { "description": "Article adapted for part of Chapter 5", "type": "doi", "url": "https://doi.org/10.1088/2041-8205/788/2/L29" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Sirio Belli", "deposited_on": "2015-11-09 17:24:06", "doi": "10.7907/Z9QN64NQ ", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-07-21", "gradofc_approval_date": "2015-11-05", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2016", "author_list": "Belli, Sirio" }, { "id": "/id/eprint/9604", "eprint_id": 9604, "rev_number": 32, "documents": [ { "id": "/id/document/64353", "doc_id": 64353, "rev_number": 2, "files": [ { "id": "/id/file/180087", "fileid": 180087, "datasetid": "document", "objectid": 64353, "filename": "Swarnima-Manohar-thesis-2016.pdf", "mime_type": "application/pdf", "hash": "bdc02cd191e990752b92719159e904aa", "hash_type": "MD5", "filesize": 8264476, "mtime": "2016-03-17 16:48:13", "url": "/9604/1/Swarnima-Manohar-thesis-2016.pdf" } ], "eprint_id": 9604, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Swarnima-Manohar-thesis-2016.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/64353" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/64353" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/64353" } ] } } ], "eprint_status": "archive", "userid": 10775, "dir": "disk0/00/00/96/04", "datestamp": "2016-03-08 18:56:22", "lastmod": "2022-12-02 19:59:31", "status_changed": "2016-03-21 17:35:28", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "swarnim@gmail.com", "id": "Manohar-Swarnima", "name": { "family": "Manohar", "given": "Swarnima" }, "orcid": "0000-0002-3506-566X", "show_email": "YES" } ] }, "title": "Lurking in ULIRGs: Molecular Gas in local Merging Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Galaxies: individual (Arp 220, NGC 6240); Galaxies: Starbursts", "abstract": "Mergers and interacting galaxies are pivotal to the evolution of galaxies in the universe. They are the sites of prodigious star formation and key to understanding the starburst processes: the physical and chemical properties and the dynamics of the molecular gas. ULIRGs or Ultraluminous Infrared Galaxies are a result of many of these mergers. They host extreme starbursts, AGNs, and mergers. They are the perfect laboratory to probe the connection between starbursts, black hole accretion and mergers and to further our understanding of star formation and merging.
\r\n\r\nNGC 6240 and Arp 220 can be considered the founding members of this very active class of objects. They are in different stages of merging and hence are excellent case studies to further our understanding about the merging process. We have imaged the dense star-forming regions of these galaxies at sub-arcsec resolution with CARMA C and B Configurations (2\" and 0.5 - 0.8\"). Multi-band imaging allows excitation analysis of HCN, HCO+, HNC, and CS along with CO transitions to constrain the properties of the gas. Our dataset is unique in that we have observed these lines at similar resolutions and high sensitivity which can be used to derive line ratios of faint high excitation lines.
\r\n\r\nArp 220 has not had confirmed X-ray AGN detections for either nuclei. However, our observations indicate HCN/HNC ratios consistent with the chemistry of X-ray Dominated Regions (XDRs) -- a likely symptom of AGN. We calculated the molecular Hydrogen densities using each of the molecular species and conclude that assuming abundances of HNC and HCO+ similar to those in galactic sources are incorrect in the case of ULIRGs. The physical conditions in the dense molecular gas in ULIRGs alter these abundances. The derived H2 volume densities are ~ 5 x 104 cm-3 in both Arp 220 nuclei and ~ 104 cm-3 in NGC 6240.
", "date": "2016", "date_type": "degree", "id_number": "CaltechTHESIS:03042016-144127692", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03042016-144127692", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Swarnima Manohar", "deposited_on": "2016-03-08 18:56:22", "doi": "10.7907/Z9T72FDK", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "chair" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" }, { "email": "dmawet@astro.caltech.edu", "id": "Mawet-D", "name": { "family": "Mawet", "given": "Dimitri" }, "orcid": "0000-0002-8895-4735", "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-01-12", "gradofc_approval_date": "2016-03-18", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2016", "author_list": "Manohar, Swarnima" }, { "id": "/id/eprint/9741", "eprint_id": 9741, "rev_number": 28, "documents": [ { "id": "/id/document/66885", "doc_id": 66885, "rev_number": 2, "files": [ { "id": "/id/file/186152", "fileid": 186152, "datasetid": "document", "objectid": 66885, "filename": "thesis_mod_to_cit_standards.pdf", "mime_type": "application/pdf", "hash": "3ecbed11b04516b6223bd0d579c46729", "hash_type": "MD5", "filesize": 30777010, "mtime": "2016-05-25 00:07:22", "url": "/9741/1/thesis_mod_to_cit_standards.pdf" } ], "eprint_id": 9741, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis_mod_to_cit_standards.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/66885" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/66885" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/66885" } ] } } ], "eprint_status": "archive", "userid": 10615, "dir": "disk0/00/00/97/41", "datestamp": "2016-05-25 23:31:38", "lastmod": "2021-10-26 17:25:53", "status_changed": "2016-05-25 23:31:38", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mbottom.caltech@gmail.com", "id": "Bottom-Michael", "name": { "family": "Bottom", "given": "Michael" }, "orcid": "0000-0003-1341-5531", "show_email": "NO" } ] }, "title": "Two Roads to Planet Detection", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomical instrumentation, extrasolar planets, high contrast imaging, high resolution spectroscopy", "abstract": "One of the most exciting discoveries in astrophysics of the last last decade is of the sheer diversity of planetary systems. These include \"hot Jupiters\", giant planets so close to their host stars that they orbit once every few days; \"Super-Earths\", planets with sizes intermediate to those of Earth and Neptune, of which no analogs exist in our own solar system; multi-planet systems with planets smaller than Mars to larger than Jupiter; planets orbiting binary stars; free-floating planets flying through the emptiness of space without any star; even planets orbiting pulsars. Despite these remarkable discoveries, the field is still young, and there are many areas about which precious little is known. In particular, we don't know the planets orbiting Sun-like stars nearest to our own solar system, and we know very little about the compositions of extrasolar planets. This thesis provides developments in those directions, through two instrumentation projects.
\r\n\r\nThe first chapter of this thesis concerns detecting planets in the Solar neighborhood using precision stellar radial velocities, also known as the Doppler technique. We present an analysis determining the most efficient way to detect planets considering factors such as spectral type, wavelengths of observation, spectrograph resolution, observing time, and instrumental sensitivity. We show that G and K dwarfs observed at 400-600 nm are the best targets for surveys complete down to a given planet mass and out to a specified orbital period. Overall we find that M dwarfs observed at 700-800 nm are the best targets for habitable-zone planets, particularly when including the effects of systematic noise floors caused by instrumental imperfections. Somewhat surprisingly, we demonstrate that a modestly sized observatory, with a dedicated observing program, is up to the task of discovering such planets.
\r\n\r\nWe present just such an observatory in the second chapter, called the \"MINiature Exoplanet Radial Velocity Array,\" or MINERVA. We describe the design, which uses a novel multi-aperture approach to increase stability and performance through lower system etendue, as well as keeping costs and time to deployment down. We present calculations of the expected planet yield, and data showing the system performance from our testing and development of the system at Caltech's campus. We also present the motivation, design, and performance of a fiber coupling system for the array, critical for efficiently and reliably bringing light from the telescopes to the spectrograph. We finish by presenting the current status of MINERVA, operational at Mt. Hopkins observatory in Arizona.
\r\n\r\nThe second part of this thesis concerns a very different method of planet detection, direct imaging, which involves discovery and characterization of planets by collecting and analyzing their light. Directly analyzing planetary light is the most promising way to study their atmospheres, formation histories, and compositions. Direct imaging is extremely challenging, as it requires a high performance adaptive optics system to unblur the point-spread function of the parent star through the atmosphere, a coronagraph to suppress stellar diffraction, and image post-processing to remove non-common path \"speckle\" aberrations that can overwhelm any planetary companions.
\r\n\r\nTo this end, we present the \"Stellar Double Coronagraph,\" or SDC, a flexible coronagraphic platform for use with the 200\" Hale telescope. It has two focal and pupil planes, allowing for a number of different observing modes, including multiple vortex phase masks in series for improved contrast and inner working angle behind the obscured aperture of the telescope. We present the motivation, design, performance, and data reduction pipeline of the instrument. In the following chapter, we present some early science results, including the first image of a companion to the star delta Andromeda, which had been previously hypothesized but never seen.
\r\n\r\nA further chapter presents a wavefront control code developed for the instrument, using the technique of \"speckle nulling,\" which can remove optical aberrations from the system using the deformable mirror of the adaptive optics system. This code allows for improved contrast and inner working angles, and was written in a modular style so as to be portable to other high contrast imaging platforms. We present its performance on optical, near-infrared, and thermal infrared instruments on the Palomar and Keck telescopes, showing how it can improve contrasts by a factor of a few in less than ten iterations.
\r\n\r\nOne of the large challenges in direct imaging is sensing and correcting the electric field in the focal plane to remove scattered light that can be much brighter than any planets. In the last chapter, we present a new method of focal-plane wavefront sensing, combining a coronagraph with a simple phase-shifting interferometer. We present its design and implementation on the Stellar Double Coronagraph, demonstrating its ability to create regions of high contrast by measuring and correcting for optical aberrations in the focal plane. Finally, we derive how it is possible to use the same hardware to distinguish companions from speckle errors using the principles of optical coherence. We present results observing the brown dwarf HD 49197b, demonstrating the ability to detect it despite it being buried in the speckle noise floor. We believe this is the first detection of a substellar companion using the coherence properties of light.
", "date": "2016", "date_type": "degree", "id_number": "CaltechTHESIS:05242016-123425364", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05242016-123425364", "related_url": { "items": [ { "description": "Previously published material in chapter 2 and 3", "type": "doi", "url": "http://dx.doi.org/10.1086/670174" }, { "description": "Previously published materials in chapter 3", "type": "doi", "url": "http://dx.doi.org/10.1117/1.JATIS.1.2.027002" }, { "description": "Previously published materials in chapter 5", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/809/1/11" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Space Technology Research Fellowship", "grant_number": "NNX13AN42H" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "http://iopscience.iop.org/journal/1538-3873/page/forthcomingArticles: (Accepted 2/12/2016, not yet published) Stellar Double Coronagraph: A Multistage Coronagraphic Platform at Palomar Observatory ", "deposited_by": "Michael Bottom", "deposited_on": "2016-05-25 23:31:38", "doi": "10.7907/Z97P8WC0", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "advisor" }, { "email": "jjohnson@cfa.harvard.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "jjohnson@cfa.harvard.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" }, { "email": "Eugene.Serabyn@jpl.nasa.gov", "id": "Serabyn-E", "name": { "family": "Serabyn", "given": "Eugene" }, "role": "member" }, { "email": "hirata.10@osu.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2016-05-10", "gradofc_approval_date": "2016-05-25", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2016", "author_list": "Bottom, Michael" }, { "id": "/id/eprint/8898", "eprint_id": 8898, "rev_number": 27, "documents": [ { "id": "/id/document/56950", "doc_id": 56950, "rev_number": 4, "files": [ { "id": "/id/file/161881", "fileid": 161881, "datasetid": "document", "objectid": 56950, "filename": "saFN999I9qeezyfjOAIBOSbqqbgW0lXJe8VCTAf7R624ttavA87cha2LoU7i0CUv", "mime_type": "application/pdf", "hash": "4a5722f53e70679e31e3ed131826e9fc", "hash_type": "MD5", "filesize": 72440132, "mtime": "2015-05-29 01:16:01", "url": "/8898/1/saFN999I9qeezyfjOAIBOSbqqbgW0lXJe8VCTAf7R624ttavA87cha2LoU7i0CUv" } ], "eprint_id": 8898, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "saFN999I9qeezyfjOAIBOSbqqbgW0lXJe8VCTAf7R624ttavA87cha2LoU7i0CUv", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" } ], "eprint_status": "archive", "userid": 10573, "dir": "disk0/00/00/88/98", "datestamp": "2015-06-02 15:17:41", "lastmod": "2020-03-10 19:19:04", "status_changed": "2015-06-02 15:17:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "rduan@vip.163.com", "id": "Duan-Ran", "name": { "family": "Duan", "given": "Ran" }, "show_email": "NO" } ] }, "title": "Instrumentation for Kinetic-Inductance-Detector-Based Submillimeter Radio Astronomy", "ispublished": "unpub", "full_text_status": "public", "keywords": "Submillimeter, Radio Astronomy, Instrumentation, Kinetic Inductance Detector", "abstract": "A substantial amount of important scientific information is contained within astronomical data at the submillimeter and far-infrared (FIR) wavelengths, including information regarding dusty galaxies, galaxy clusters, and star-forming regions; however, these wavelengths are among the least-explored\r\nfields in astronomy because of the technological difficulties involved in such research. Over the past 20 years, considerable efforts have been devoted to developing submillimeter- and millimeter-wavelength astronomical instruments and telescopes.
\r\n\r\nThe number of detectors is an important property of such instruments and is the subject of the current study. Future telescopes will require as many as hundreds of thousands of detectors to meet the necessary requirements in terms of the field of view, scan speed, and resolution. A large pixel count is one benefit of the development of multiplexable detectors that use kinetic inductance detector (KID) technology.
\r\n\r\nThis dissertation presents the development of a KID-based instrument including a portion of the millimeter-wave bandpass filters and all aspects of the readout electronics, which together enabled one of the largest detector counts achieved to date in submillimeter-/millimeter-wavelength imaging arrays: a total of 2304 detectors. The work presented in this dissertation has been implemented in the MUltiwavelength Submillimeter Inductance Camera (MUSIC), a new instrument for the Caltech Submillimeter Observatory (CSO).
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:05282015-141343540", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05282015-141343540", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Ran Duan", "deposited_on": "2015-06-02 15:17:41", "doi": "10.7907/Z90P0WXZ", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "chair" }, { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" }, { "email": "sweinreb@caltech.edu", "id": "Weinreb-S", "name": { "family": "Weinreb", "given": "Sander" }, "role": "member" }, { "email": "rutledge@caltech.edu", "id": "Rutledge-D-B", "name": { "family": "Rutledge", "given": "David B." }, "role": "member" }, { "email": "hajimiri@caltech.edu", "id": "Hajimiri-A", "name": { "family": "Hajimiri", "given": "Ali" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-06-21", "gradofc_approval_date": "2015-06-01", "review_status": "approved", "option_major": { "items": [ "eleceng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2015", "author_list": "Duan, Ran" }, { "id": "/id/eprint/8958", "eprint_id": 8958, "rev_number": 25, "documents": [ { "id": "/id/document/58289", "doc_id": 58289, "rev_number": 2, "files": [ { "id": "/id/file/164471", "fileid": 164471, "datasetid": "document", "objectid": 58289, "filename": "teply_grant_2015_thesis.pdf", "mime_type": "application/pdf", "hash": "2be4557ec0197cc762136ffb18eaed07", "hash_type": "MD5", "filesize": 15369733, "mtime": "2015-06-02 22:30:19", "url": "/8958/1/teply_grant_2015_thesis.pdf" } ], "eprint_id": 8958, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "teply_grant_2015_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/58289" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/58289" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/58289" } ] } } ], "eprint_status": "archive", "userid": 10589, "dir": "disk0/00/00/89/58", "datestamp": "2015-06-04 22:56:23", "lastmod": "2021-10-26 17:13:27", "status_changed": "2015-06-04 22:56:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "grant.teply@gmail.com", "id": "Teply-Grant-Paul", "name": { "family": "Teply", "given": "Grant Paul" }, "show_email": "NO" } ] }, "title": "Measurement of the Polarization of the Cosmic Microwave Background with the BICEP2 and Keck Array Telescopes", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; instrumentation: polarimeters; telescopes", "abstract": "Precision polarimetry of the cosmic microwave background (CMB) has become a mainstay of observational cosmology. The \u039bCDM model predicts a polarization of the CMB at the level of a few \u03bcK, with a characteristic E-mode pattern. On small angular scales, a B-mode pattern arises from the gravitational lensing of E-mode power by the large scale structure of the universe. Inflationary gravitational waves (IGW) may be a source of B-mode power on large angular scales, and their relative contribution to primordial fluctuations is parameterized by a tensor-to-scalar ratio r. BICEP2 and Keck Array are a pair of CMB polarimeters at the South Pole designed and built for optimal sensitivity to the primordial B-mode peak around multipole l ~ 100. The BICEP2/Keck Array program intends to achieve a sensitivity to r \u2265 0.02. Auxiliary science goals include the study of gravitational lensing of E-mode into B-mode signal at medium angular scales and a high precision survey of Galactic polarization. These goals require low noise and tight control of systematics. We describe the design and calibration of the instrument. We also describe the analysis of the first three years of science data. BICEP2 observes a significant B-mode signal at 150 GHz in excess of the level predicted by the lensed-\u039bCDM model, and Keck Array confirms the excess signal at > 5\u03c3. We combine the maps from the two experiments to produce 150 GHz Q and U maps which have a depth of 57 nK deg (3.4 \u03bcK arcmin) over an effective area of 400 deg2 for an equivalent survey weight of 248000 \u03bcK2. We also show preliminary Keck Array 95 GHz maps. A joint analysis with the Planck collaboration reveals that much of BICEP2/Keck Array's observed 150 GHz signal at low l is more likely a Galactic dust foreground than a measurement of r. Marginalizing over dust and r, lensing B-modes are detected at 7.0\u03c3 significance.", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:06012015-163200704", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06012015-163200704", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Grant Teply", "deposited_on": "2015-06-04 22:56:23", "doi": "10.7907/Z9XP72WM", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "chair" }, { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "member" }, { "email": "smaria@caltech.edu", "id": "Spiropulu-M", "name": { "family": "Spiropulu", "given": "Maria" }, "orcid": "0000-0001-8172-7081", "role": "member" }, { "email": "olivier.dore@caltech.edu", "id": "Dor\u00e9-Olivier-P", "name": { "family": "Dor\u00e9", "given": "Olivier P." }, "orcid": "0000-0001-7432-2932", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-05-08", "gradofc_approval_date": "2015-06-04", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2015", "author_list": "Teply, Grant Paul" }, { "id": "/id/eprint/9002", "eprint_id": 9002, "rev_number": 44, "documents": [ { "id": "/id/document/59385", "doc_id": 59385, "rev_number": 4, "files": [ { "id": "/id/file/166710", "fileid": 166710, "datasetid": "document", "objectid": 59385, "filename": "Jing-Luan-2015-thesis.pdf", "mime_type": "application/pdf", "hash": "74274f7fd1546792cb8e15e255a9fa20", "hash_type": "MD5", "filesize": 1078515, "mtime": "2015-06-08 20:10:27", "url": "/9002/1/Jing-Luan-2015-thesis.pdf" } ], "eprint_id": 9002, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "original appproved version", "language": "en", "security": "internal", "license": "other", "main": "Jing-Luan-2015-thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": 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"eprint_status": "archive", "userid": 855, "dir": "disk0/00/00/90/02", "datestamp": "2015-12-17 19:02:39", "lastmod": "2019-10-04 00:08:55", "status_changed": "2015-12-17 19:02:39", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jingluan2008@gmail.com", "id": "Luan-Jing", "name": { "family": "Luan", "given": "Jing" }, "show_email": "NO" } ] }, "title": "Toward Understanding Astrophysical Phenomena", "ispublished": "unpub", "full_text_status": "public", "keywords": "Fast radio burst, Mean motion resonance, Secular interaction, Rubble piles", "abstract": "Fast radio bursts (FRBs), a novel type of radio pulse, whose physics is not yet understood at all. Only a handful of FRBs had been detected when we started this project. Taking account of the scant observations, we put physical constraints on FRBs. We excluded proposals of a galactic origin for their extraordinarily high dispersion measures (DM), in particular stellar coronas and HII regions. Therefore our work supports an extragalactic origin for FRBs. We show that the resolved scattering tail of FRB 110220 is unlikely to be due to propagation through the intergalactic plasma. Instead the scattering is probably caused by the interstellar medium in the FRB's host galaxy, and indicates that this burst sits in the central region of that galaxy. Pulse durations of order ms constrain source sizes of FRBs implying enormous brightness temperatures and thus coherent emission. Electric fields near FRBs at cosmological distances would be so strong that they could accelerate free electrons from rest to relativistic energies in a single wave period. When we worked on FRBs, it was unclear whether they were genuine astronomical signals as distinct from 'perytons', clearly terrestrial radio bursts, sharing some common properties with FRBs. Recently, in April 2015, astronomers discovered that perytons were emitted by microwave ovens. Radio chirps similar to FRBs were emitted when their doors opened while they were still heating. Evidence for the astronomical nature of FRBs has strengthened since our paper was published. Some bursts have been found to show linear and circular polarizations and Faraday rotation of the linear polarization has also been detected. I hope to resume working on FRBs in the near future. But after we completed our FRB paper, I decided to pause this project because of the lack of observational constraints.
\r\n\r\n\r\nThe pulsar triple system, J0733+1715, has its orbital parameters fitted to high accuracy owing to the precise timing of the central ms pulsar. The two orbits are highly hierarchical, namely Porb,1 << Porb,2, where 1 and 2 label the inner and outer white dwarf (WD) companions respectively. Moreover, their orbital planes almost coincide, providing a unique opportunity to study secular interaction associated purely with eccentricity beyond the solar system. Secular interaction only involves effect averaged over many orbits. Thus each companion can be represented by an elliptical wire with its mass distributed inversely proportional to its local orbital speed. Generally there exists a mutual torque, which vanishes only when their apsidal lines are parallel or anti-parallel. To maintain either mode, the eccentricity ratio, e1/e2, must be of the proper value, so that both apsidal lines precess together. For J0733+1715, e1 << e2 for the parallel mode, while e1 >> e2 for the anti-parallel one. We show that the former precesses ~ 10 times slower than the latter. Currently the system is dominated by the parallel mode. Although only a little anti-parallel mode survives, both eccentricities especially e1 oscillate on ~ 103yr timescale. Detectable changes would occur within ~ 1\\yr. We demonstrate that the anti-parallel mode gets damped ~ 104 times faster than its parallel brother by any dissipative process diminishing e1. If it is the tidal damping in the inner WD, we proceed to estimate its tidal quantity parameter (Q) to be ~ 106, which was poorly constrained by observations. However, tidal damping may also happen during the preceding low-mass X-ray binary (LMXB) phase or hydrogen thermal nuclear flashes. But, in both cases, the inner companion fills its Roche lobe and probably suffers mass/angular momentum loss, which might cause e1 to grow rather than decay.
\r\n\r\n\r\nSeveral pairs of solar system satellites occupy mean motion resonances (MMRs). We divide these into two groups according to their proximity to exact resonance. Proximity is measured by the existence of a separatrix in phase space. MMRs between Io-Europa, Europa-Ganymede and Enceladus-Dione are too distant from exact resonance for a separatrix to appear. A separatrix is present only in the phase spaces of the Mimas-Tethys and Titan-Hyperion MMRs and their resonant arguments are the only ones to exhibit substantial librations. When a separatrix is present, tidal damping of eccentricity or inclination excites overstable librations that can lead to passage through resonance on the damping timescale. However, after investigation, we conclude that the librations in the Mimas-Tethys and Titan-Hyperion MMRs are fossils and do not result from overstability.
\r\n\r\n\r\nRubble piles are common in the solar system. Monolithic elements touch their neighbors in small localized areas. Voids occupy a significant fraction of the volume. In a fluid-free environment, heat cannot conduct through voids; only radiation can transfer energy across them. We model the effective thermal conductivity of a rubble pile and show that it is proportional the square root of the pressure, P, for P\u2264 \u03b53\u03bc where \u03b5 is the material's yield strain and \u03bc its shear modulus. Our model provides an excellent fit to the depth dependence of the thermal conductivity in the top 140 cm of the lunar regolith. It also offers an explanation for the low thermal inertias of rocky asteroids and icy satellites. Lastly, we discuss how rubble piles slow down the cooling of small bodies such as asteroids.
\r\n\r\n\r\nElectromagnetic (EM) follow-up observations of gravitational wave (GW) events will help shed light on the nature of the sources, and more can be learned if the EM follow-ups can start as soon as the GW event becomes observable. In this paper, we propose a computationally efficient time-domain algorithm capable of detecting gravitational waves (GWs) from coalescing binaries of compact objects with nearly zero time delay. In case when the signal is strong enough, our algorithm also has the flexibility to trigger EM observation before the merger. The key to the efficiency of our algorithm arises from the use of chains of so-called Infinite Impulse Response (IIR) filters, which filter time-series data recursively. Computational cost is further reduced by a template interpolation technique that requires filtering to be done only for a much coarser template bank than otherwise required to sufficiently recover optimal signal-to-noise ratio. Towards future detectors with sensitivity extending to lower frequencies, our algorithm's computational cost is shown to increase rather insignificantly compared to the conventional time-domain correlation method. Moreover, at latencies of less than hundreds to thousands of seconds, this method is expected to be computationally more efficient than the straightforward frequency-domain method.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:06052015-153743425", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06052015-153743425", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "suggestions": "Withheld until Sept 6, 2015. Updated version received 12/15/2015. Released 12/17/2015.", "deposited_by": "Jing Luan", "deposited_on": "2015-12-17 19:02:39", "doi": "10.7907/Z97942NB ", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "chair" }, { "email": "cott@tapir.caltech.edu", "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "role": "member" }, { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-05-22", "gradofc_approval_date": "2015-06-09", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2015", "author_list": "Luan, Jing" }, { "id": "/id/eprint/8925", "eprint_id": 8925, "rev_number": 27, "documents": [ { "id": "/id/document/57337", "doc_id": 57337, "rev_number": 2, "files": [ { "id": "/id/file/162769", "fileid": 162769, "datasetid": "document", "objectid": 57337, "filename": "Thesis.pdf", "mime_type": "application/pdf", "hash": "bda01d2286942db13483405f819fabc4", "hash_type": "MD5", "filesize": 20294259, "mtime": "2015-05-30 15:24:23", "url": "/8925/1/Thesis.pdf" } ], "eprint_id": 8925, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/57338", "doc_id": 57338, 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left-over building blocks from its formation. The Palomar Transient Factory (PTF) survey began in 2009 as the latest wide-field sky-survey program to be conducted on the 1.2-meter Samuel Oschin telescope at Palomar Observatory. Though its main science program has been the discovery of high-energy extragalactic sources (such as supernovae), during its first five years PTF has collected nearly five million observations of over half a million unique solar system small bodies. This thesis begins to analyze this vast data set to address key population-level science topics, including: the detection rates of rare main-belt comets and small near-Earth asteroids, the spin and shape properties of asteroids as inferred from their lightcurves, the applicability of this visible light data to the interpretation of ultraviolet asteroid observations, and a comparison of the physical properties of main-belt and Jovian Trojan asteroids. Future sky-surveys would benefit from application of the analytical techniques presented herein, which include novel modeling methods and unique applications of machine-learning classification. The PTF asteroid small-body data produced in the course of this thesis work should remain a fertile source of solar system science and discovery for years to come.", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:05292015-134454898", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05292015-134454898", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Lindsay Cleary", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Adam Waszczak", "deposited_on": "2015-06-10 13:56:42", "doi": "10.7907/Z91G0J73", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "chair" }, { "email": "prince@srl.caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-05-15", "gradofc_approval_date": "2015-06-09", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2015", "author_list": "Waszczak, Adam" }, { "id": "/id/eprint/8949", "eprint_id": 8949, "rev_number": 32, "documents": [ { "id": "/id/document/57417", "doc_id": 57417, "rev_number": 3, "files": [ { "id": "/id/file/162899", "fileid": 162899, "datasetid": "document", "objectid": 57417, "filename": "mallodi_thesis_5.tex", "mime_type": "text/plain", "hash": "40f6a051e559fdab2e72b5a43660d10c", "hash_type": "MD5", "filesize": 205388, "mtime": "2015-06-01 05:50:28", "url": "/8949/7/mallodi_thesis_5.tex" } ], "eprint_id": 8949, "pos": 7, "placement": 7, "mime_type": "text/plain", "format": "application/x-latex", "format_desc": "Thesis Latex", "language": "en", "security": "internal", "license": "other", "main": "mallodi_thesis_5.tex", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/57581" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/57581" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/57581" } ] } } ], "eprint_status": "archive", "userid": 10586, "dir": "disk0/00/00/89/49", "datestamp": "2015-06-02 15:33:34", "lastmod": "2023-11-08 00:16:42", "status_changed": "2015-06-02 15:33:34", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "marco.allodi@gmail.com", "id": "Allodi-Marco-Alberto", "name": { "family": "Allodi", "given": "Marco Alberto" }, "orcid": "0000-0002-3289-1659", "show_email": "NO" } ] }, "title": "On Ultrafast Time-Domain TeraHertz Spectroscopy in the Condensed Phase: Linear Spectroscopic Measurements of Hydrogen-Bond Dynamics of Astrochemical Ice Analogs and Nonlinear TeraHertz Kerr Effect Measurements of Vibrational Quantum Beats", "ispublished": "unpub", "full_text_status": "public", "keywords": "Chemical Physics, Ultrafast Laser Spectroscopy, TeraHertz Spectroscopy, Molecular Spectroscopy, Condensed-Phase Dynamics", "abstract": "Much of the chemistry that affects life on planet Earth occurs in the condensed phase. The TeraHertz\r\n(THz) or far-infrared (far-IR) region of the electromagnetic spectrum (from 0.1 THz to 10 THz,\r\n3 cm-1 to 300 cm-1, or 3000 \u03bcm to 30 \u03bcm) has been shown to provide unique possibilities in the\r\nstudy of condensed-phase processes. The goal of this work is to expand the possibilities available in\r\nthe THz region and undertake new investigations of fundamental interest to chemistry. Since we are\r\nfundamentally interested in condensed-phase processes, this thesis focuses on two areas where THz\r\nspectroscopy can provide new understanding: astrochemistry and solvation science.\r\nTo advance these fields, we had to develop new instrumentation that would enable the experiments\r\nnecessary to answer new questions in either astrochemistry or solvation science. We first\r\ndeveloped a new experimental setup capable of studying astrochemical ice analogs in both the TeraHertz\r\n(THz), or far-Infrared (far-IR), region (0.3 - 7.5 THz; 10 - 250 cm-1) and the mid-IR (400 -\r\n4000 cm-1). The importance of astrochemical ices lies in their key role in the formation of complex\r\norganic molecules, such as amino acids and sugars in space. Thus, the instruments are capable of\r\nperforming variety of spectroscopic studies that can provide especially relevant laboratory data to\r\nsupport astronomical observations from telescopes such as the Herschel Space Telescope, the Stratospheric\r\nObservatory for Infrared Astronomy (SOFIA), and the Atacama Large Millimeter Array\r\n(ALMA). The experimental apparatus uses a THz time-domain spectrometer, with a 1750/875 nm\r\nplasma source and a GaP detector crystal, to cover the bandwidth mentioned above with ~10 GHz\r\n(~0.3 cm-1) resolution.
\r\n\r\nUsing the above instrumentation, experimental spectra of astrochemical ice analogs of water and\r\ncarbon dioxide in pure, mixed, and layered ices were collected at different temperatures under high\r\nvacuum conditions with the goal of investigating the structure of the ice. We tentatively observe a\r\nnew feature in both amorphous solid water and crystalline water at 33 cm-1 (1 THz). In addition,\r\nour studies of mixed and layered ices show how it is possible to identify the location of carbon dioxide\r\nas it segregates within the ice by observing its effect on the THz spectrum of water ice. The THz\r\nspectra of mixed and layered ices are further analyzed by fitting their spectra features to those of\r\npure amorphous solid water and crystalline water ice to quantify the effects of temperature changes\r\non structure. From the results of this work, it appears that THz spectroscopy is potentially well\r\nsuited to study thermal transformations within the ice.
\r\n\r\nTo advance the study of liquids with THz spectroscopy, we developed a new ultrafast nonlinear\r\nTHz spectroscopic technique: heterodyne-detected, ultrafast THz Kerr effect (TKE) spectroscopy.\r\nWe implemented a heterodyne-detection scheme into a TKE spectrometer that uses a stilbazoiumbased\r\nTHz emitter, 4-N,N-dimethylamino-4-N-methyl-stilbazolium 2,4,6-trimethylbenzenesulfonate\r\n(DSTMS), and high numerical aperture optics which generates THz electric field in excess of\r\n300 kV/cm, in the sample. This allows us to report the first measurement of quantum beats at terahertz\r\n(THz) frequencies that result from vibrational coherences initiated by the nonlinear, dipolar\r\ninteraction of a broadband, high-energy, (sub)picosecond THz pulse with the sample. Our instrument\r\nimproves on both the frequency coverage, and sensitivity previously reported; it also ensures\r\na backgroundless measurement of the THz Kerr effect in pure liquids. For liquid diiodomethane, we\r\nobserve a quantum beat at 3.66 THz (122 cm-1), in exact agreement with the fundamental transition\r\nfrequency of the \u03c54 vibration of the molecule. This result provides new insight into dipolar\r\nvs. Raman selection rules at terahertz frequencies.
\r\n\r\nTo conclude we discuss future directions for the nonlinear THz spectroscopy in the Blake lab.\r\nWe report the first results from an experiment using a plasma-based THz source for nonlinear\r\nspectroscopy that has the potential to enable nonlinear THz spectra with a sub-100 fs temporal\r\nresolution, and how the optics involved in the plasma mechanism can enable THz pulse shaping.\r\nFinally, we discuss how a single-shot THz detection scheme could improve the acquisition of THz\r\ndata and how such a scheme could be implemented in the Blake lab. The instruments developed\r\nherein will hopefully remain a part of the groups core competencies and serve as building blocks\r\nfor the next generation of THz instrumentation that pushes the frontiers of both chemistry and the\r\nscientific enterprise as a whole.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:05312015-221615628", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05312015-221615628", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Restricted to Caltech community only until 1 January 2016. Released Jan. 4, 2016.", "deposited_by": "Marco Allodi", "deposited_on": "2015-06-02 15:33:34", "doi": "10.7907/Z97D2S2P", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jlbchamp@caltech.edu", "id": "Beauchamp-J-L", "name": { "family": "Beauchamp", "given": "Jesse L." }, "orcid": "0000-0001-8839-4822", "role": "chair" }, { "email": "hbgray@caltech.edu", "id": "Gray-H-B", "name": { "family": "Gray", "given": "Harry B." }, "orcid": "0000-0002-7937-7876", "role": "member" }, { "email": "tfm@caltech.edu", "id": "Miller-T-F", "name": { "family": "Miller", "given": "Thomas F." }, "orcid": "0000-0002-1882-5380", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-05-26", "gradofc_approval_date": "2015-06-01", "thesis_awards": "The Herbert Newby McCoy Award, 2015", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2015", "author_list": "Allodi, Marco Alberto" }, { "id": "/id/eprint/8644", "eprint_id": 8644, "rev_number": 23, "documents": [ { "id": "/id/document/51708", "doc_id": 51708, "rev_number": 4, "files": [ { "id": "/id/file/149967", "fileid": 149967, "datasetid": "document", "objectid": 51708, "filename": "apj_permission.pdf", "mime_type": "application/pdf", "hash": "a09caf98f5a75e6a0e77da8a7cea9035", "hash_type": "MD5", "filesize": 45367, "mtime": "2014-08-27 19:00:07", "url": "/8644/7/apj_permission.pdf" } ], "eprint_id": 8644, "pos": 7, "placement": 7, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Clarification of Astrophysical Journal license", "language": "en", "security": "internal", "license": "other", "main": "apj_permission.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/51746" } ] } } ], "eprint_status": "archive", "userid": 10350, "dir": "disk0/00/00/86/44", "datestamp": "2014-08-29 18:44:46", "lastmod": "2023-05-30 22:14:46", "status_changed": "2014-08-29 18:44:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kfindeisen@wavecable.com", "id": "Findeisen-Krzysztof", "name": { "family": "Findeisen", "given": "Krzysztof" }, "show_email": "NO" } ] }, "title": "New Insights from Aperiodic Variability of Young Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy; variable stars; pre-main sequence stars; T Tauri stars; statistical methods; time domain astronomy; surveys", "abstract": "Nearly all young stars are variable, with the variability traditionally divided into two classes: periodic variables and aperiodic or \"irregular\" variables. Periodic variables have been studied extensively, typically using periodograms, while aperiodic variables have received much less attention due to a lack of standard statistical tools. However, aperiodic variability can serve as a powerful probe of young star accretion physics and inner circumstellar disk structure. For my dissertation, I analyzed data from a large-scale, long-term survey of the nearby North America Nebula complex, using Palomar Transient Factory photometric time series collected on a nightly or every few night cadence over several years. This survey is the most thorough exploration of variability in a sample of thousands of young stars over time baselines of days to years, revealing a rich array of lightcurve shapes, amplitudes, and timescales.
\r\n\r\nI have constrained the timescale distribution of all young variables, periodic and aperiodic, on timescales from less than a day to ~100 days. I have shown that the distribution of timescales for aperiodic variables peaks at a few days, with relatively few (~15%) sources dominated by variability on tens of days or longer. My constraints on aperiodic timescale distributions are based on two new tools, magnitude- vs. time-difference (\u0394m-\u0394t) plots and peak-finding plots, for describing aperiodic lightcurves; this thesis provides simulations of their performance and presents recommendations on how to apply them to aperiodic signals in other time series data sets. In addition, I have measured the error introduced into colors or SEDs from combining photometry of variable sources taken at different epochs. These are the first quantitative results to be presented on the distributions in amplitude and time scale for young aperiodic variables, particularly those varying on timescales of weeks to months.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:08272014-105550096", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08272014-105550096", "related_url": { "items": [ { "description": "Published article adapted for Chapter 3", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/768/1/93" } ] }, "projects": { "items": [ "Palomar Transient Factory" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Krzysztof Findeisen", "deposited_on": "2014-08-29 18:44:46", "doi": "10.7907/Z93F4MH9", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "chair" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-07-29", "gradofc_approval_date": "2014-08-29", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/51416" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/51416" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/51416" } ] } } ], "eprint_status": "archive", "userid": 10330, "dir": "disk0/00/00/86/26", "datestamp": "2014-08-07 00:04:18", "lastmod": "2019-10-04 00:06:33", "status_changed": "2014-08-07 00:04:18", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "matthew.a.schenker@gmail.com", "id": "Schenker-Matthew-Aaron", "name": { "family": "Schenker", "given": "Matthew Aaron" }, "show_email": "NO" } ] }, "title": "Did Galaxies Reionize the Universe?", "ispublished": "unpub", "full_text_status": "public", "keywords": "Galaxies, cosmology", "abstract": "The epoch of reionization remains one of the last uncharted eras of cosmic history, yet this time is of crucial importance, encompassing the formation of both the first galaxies and the first metals in the universe. In this thesis, I present four related projects that both characterize the abundance and properties of these first galaxies and uses follow-up observations of these galaxies to achieve one of the first observations of the neutral fraction of the intergalactic medium during the heart of the reionization era.
\r\n\r\nFirst, we present the results of a spectroscopic survey using the Keck telescopes targeting 6.3 < z < 8.8 star-forming galaxies. We secured observations of 19 candidates, initially selected by applying the Lyman\r\nbreak technique to infrared imaging data from the Wide Field Camera 3 (WFC3) onboard the Hubble Space Telescope (HST). This survey builds upon earlier work from Stark et al. (2010, 2011), which showed that star-forming galaxies at 3 < z < 6, when the universe was highly ionized, displayed a significant increase in strong Lyman alpha emission with redshift. Our work uses the LRIS and NIRSPEC instruments to search for Lyman alpha emission in candidates at a greater redshift in the observed near-infrared, in order to discern if this evolution continues, or is quenched by an increase in the neutral fraction of the intergalactic medium. Our spectroscopic observations\r\ntypically reach a 5-sigma limiting sensitivity of < 50 AA. Despite expecting to detect Lyman alpha at 5-sigma in 7-8 galaxies based on our Monte Carlo simulations, we only achieve secure detections in two of 19 sources. Combining these results with a similar sample of 7 galaxies from Fontana et al. (2010), we determine that these few detections would only occur in < 1% of simulations if the intrinsic distribution was the same as that at z ~ 6. We consider other explanations for this decline, but find the most convincing explanation to be an increase in the neutral fraction of the intergalactic medium. Using theoretical models, we infer a neutral fraction of X_HI ~ 0.44 at z = 7.
\r\n\r\nSecond, we characterize the abundance of star-forming galaxies at z > 6.5 again using WFC3 onboard the HST. This project conducted a detailed search for candidates both in the Hubble Ultra Deep Field as well as a number of additional wider Hubble Space Telescope surveys to construct luminosity\r\nfunctions at both z ~ 7 and 8, reaching 0.65 and 0.25 mag fainter than any previous surveys, respectively. With this increased depth, we achieve some of the most robust constraints on the Schechter function faint end slopes\r\nat these redshifts, finding very steep values of alpha_{z~7} = -1.87 +/- 0.18 and alpha_{z~8} = -1.94 +/- 0.23. We discuss these results in the context of cosmic reionization, and show that given reasonable assumptions about the ionizing spectra and escape fraction of ionizing photons, only half the photons needed to maintain reionization are provided by currently observable galaxies at z ~ 7-8. We show that an extension of the luminosity function down to M_{UV} = -13.0, coupled with a low level of star-formation out to\r\nhigher redshift, can fit all available constraints on the ionization history of the universe.
\r\n\r\nThird, we investigate the strength of nebular emission in 3 < z < 5 star-forming galaxies. We begin by using the Infrared Array Camera (IRAC) onboard the Spitzer Space Telescope to investigate the strength of \r\nH alpha emission in a sample of 3.8 < z < 5.0 spectroscopically confirmed galaxies. We then conduct near-infrared observations of star-forming galaxies at 3 < z < 3.8 to investigate the strength of the [OIII] 4959/5007 and H beta emission lines from the ground using MOSFIRE. In both cases, we uncover near-ubiquitous strong nebular emission, and find excellent agreement between the fluxes derived using the separate methods. For a subset of 9 objects in our MOSFIRE sample\r\nthat have secure Spitzer IRAC detections, we compare the emission\r\nline flux derived from the excess in the K_s band photometry to that derived from direct spectroscopy and find 7 to agree within a factor of 1.6, with only one catastrophic outlier. Finally, for a different subset for which we also\r\nhave DEIMOS rest-UV spectroscopy, we compare the relative velocities of Lyman alpha and the rest-optical nebular lines which should trace the cites of star-formation. We find a median velocity offset of only \r\nv_{Ly alpha} = 149 km/s, significantly less than the 400 km/s observed for star-forming galaxies with weaker Lyman alpha emission at z = 2-3 (Steidel et al. 2010), and show that this decrease can be explained by a decrease \r\nin the neutral hydrogen column density covering the galaxy. We discuss how this will imply a lower neutral fraction for a given observed extinction of Lyman alpha when its visibility is used to probe the ionization state of the intergalactic medium.
\r\n\r\nFinally, we utilize the recent CANDELS wide-field, infra-red photometry over the GOODS-N and S fields to re-analyze the use of Lyman alpha emission to evaluate the neutrality of the intergalactic medium. With this new data, we derive accurate ultraviolet spectral slopes for a sample of 468 3 < z < 6 star-forming galaxies, already observed in the rest-UV with the Keck spectroscopic survey (Stark et al. 2010). We use a Bayesian fitting method which accurately\r\naccounts for contamination and obscuration by skylines to derive a relationship between the UV-slope of a galaxy and its intrinsic Lyman alpha equivalent width probability distribution. We then apply this data to spectroscopic surveys during the reionization era, including our own, to accurately interpret the drop in observed Lyman alpha emission. From our most recent such MOSFIRE survey, we also present evidence for the most distant galaxy confirmed through emission line spectroscopy at z = 7.62, as well as a first detection of the CIII]1907/1909 doublet at z > 7.
\r\n\r\nWe conclude the thesis by exploring future prospects and summarizing the results of Robertson et al. (2013). This work synthesizes many of the measurements in this thesis, along with external constraints, to create a model of reionization that fits nearly all available constraints.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:08012014-181643065", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08012014-181643065", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "GP", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Matthew Schenker", "deposited_on": "2014-08-07 00:04:18", "doi": "10.7907/Z9736NVR", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-06-18", "gradofc_approval_date": "2014-08-06", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/75411" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/75411" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/75411" } ] } } ], "eprint_status": "archive", "userid": 10574, "dir": "disk0/00/00/88/97", "datestamp": "2015-06-04 22:53:23", "lastmod": "2021-10-26 18:23:16", "status_changed": "2015-06-04 22:53:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "casey.handmer@gmail.com", "id": "Handmer-Casey-John", "name": { "family": "Handmer", "given": "Casey John" }, "show_email": "YES" } ] }, "title": "Gauge Invariant Spectral Cauchy Characteristic Extraction of Gravitational Waves in Computational General Relativity\r \r \r ", "ispublished": "unpub", "full_text_status": "public", "keywords": "Gravitational waves, Numerical methods, General relativity, Black holes", "abstract": "We present a complete system for Spectral Cauchy characteristic extraction (Spectral CCE). Implemented in C++ within the Spectral Einstein Code (SpEC), the method employs numerous innovative algorithms to efficiently calculate the Bondi strain, news, and flux.
\r\n\r\nSpectral CCE was envisioned to ensure physically accurate gravitational wave-forms computed for the Laser Interferometer Gravitational wave Observatory (LIGO) and similar experiments, while working toward a template bank with more than a thousand waveforms to span the binary black hole (BBH) problem\u2019s seven-dimensional parameter space.
\r\n\r\nThe Bondi strain, news, and flux are physical quantities central to efforts to understand and detect astrophysical gravitational wave sources within the Simulations of eXtreme Spacetime (SXS) collaboration, with the ultimate aim of providing the first strong field probe of the Einstein field equation.
\r\n\r\nIn a series of included papers, we demonstrate stability, convergence, and gauge invariance. We also demonstrate agreement between Spectral CCE and the legacy Pitt null code, while achieving a factor of 200 improvement in computational efficiency.
\r\n\r\nSpectral CCE represents a significant computational advance. It is the foundation upon which further capability will be built, specifically enabling the complete calculation of junk-free, gauge-free, and physically valid waveform data on the fly within SpEC.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:05282015-131606315", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05282015-131606315", "related_url": { "items": [ { "description": "Article related to ch. 3", "type": "arxiv", "url": "http://arxiv.org/abs/1406.7029" }, { "description": "Article related to ch. 3", "type": "doi", "url": "http://dx.doi.org/10.1088/0264-9381/32/2/025008" }, { "description": "Article related to ch. 4", "type": "arxiv", "url": "http://arxiv.org/abs/1502.06987" }, { "description": "Article related to ch. 4", "type": "doi", "url": "http://dx.doi.org/10.1088/0264-9381/32/23/235018" }, { "description": "Article related to ch. 5", "type": "arxiv", "url": "https://arxiv.org/abs/1605.04332" }, { "description": "Article related to ch. 5", "url": "http://dx.doi.org/10.1088/0264-9381/33/22/225007" }, { "description": "Paper on optimizing high speed transport networks using genetic algorithms", "type": "doc", "url": "https://arxiv.org/abs/1503.01524" }, { "description": "Paper on hazards to Earth orbiting satellites from captured asteroid disruption in distant Lunar retrograde orbits", "type": "doc", "url": "http://arxiv.org/abs/1505.03800" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Lindsay Cleary", "local_group": { "items": [ "TAPIR", "Astronomy Department", "LIGO" ] }, "deposited_by": "Casey Handmer", "deposited_on": "2015-06-04 22:53:23", "doi": "10.7907/Z9NP22DZ", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "advisor" }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "chair" }, { "email": "bszilagyi69@gmail.com", "id": "Szilagyi-B", "name": { "family": "Szilagyi", "given": "Bela" }, "role": "member" }, { "email": "scheel@caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "member" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "rbpatter@caltech.edu", "id": "Patterson-R-B", "name": { "family": "Patterson", "given": "Ryan B." }, "orcid": "0000-0002-5787-9517", "role": "member" }, { "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-05-14", "gradofc_approval_date": "2015-06-04", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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active binary; caltech nrao stripe 82 survey; Galactic; extragalactic; star; galaxy; ", "abstract": "While synoptic surveys in the optical and at high energies have revealed a rich discovery phase space of slow transients, a similar yield is still awaited in the radio. Majority of the past blind surveys, carried out with radio interferometers, have suffered from a low yield of slow transients, ambiguous transient classifications, and contamination by false positives. The newly-refurbished Karl G. Jansky Array (Jansky VLA) offers wider bandwidths for accurate RFI excision as well as substantially-improved sensitivity and survey speed compared with the old VLA. The Jansky VLA thus eliminates the pitfalls of interferometric transient search by facilitating sensitive, wide-field, and near-real-time radio surveys and enabling a systematic exploration of the dynamic radio sky. This thesis aims at carrying out blind Jansky VLA surveys for characterizing the radio variable and transient sources at frequencies of a few GHz and on timescales between days and years. Through joint radio and optical surveys, the thesis addresses outstanding questions pertaining to the rates of slow radio transients (e.g. radio supernovae, tidal disruption events, binary neutron star mergers, stellar flares, etc.), the false-positive foreground relevant for the radio and optical counterpart searches of gravitational wave sources, and the beaming factor of gamma-ray bursts. The need for rapid processing of the Jansky VLA data and near-real-time radio transient search has enabled the development of state-of-the-art software infrastructure. This thesis has successfully demonstrated the Jansky VLA as a powerful transient search instrument, and it serves as a pathfinder for the transient surveys planned for the SKA-mid pathfinder facilities, viz. ASKAP, MeerKAT, and WSRT/Apertif.", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:03222015-185636984", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03222015-185636984", "related_url": { "items": [ { "description": "Article adapted for Ch. 2", "type": "doi", "url": "https://doi.org/10.1038/nature10366" }, { "description": "Article adapted for Ch. 2", "type": "arxiv", "url": "https://doi.org/10.48550/arXiv.1106.3568" }, { "description": "Article adapted for Ch. 3", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/768/2/165" }, { "description": "Article adapted for Ch. 3", "type": "arxiv", "url": "https://doi.org/10.48550/arXiv.1303.6282" }, { "description": "Article adapted for Appendix A", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/771/2/110" }, { "description": "Article adapted for Appendix A", "type": "arxiv", "url": "https://doi.org/10.48550/arXiv.1306.0598" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Radio Astronomy Observatory Grote Reber fellowship" } ] }, "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Kunal Mooley", "deposited_on": "2015-05-06 20:31:45", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "co-advisor" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "co-advisor" }, { "email": "dfrail@aoc.nrao.edu", "id": "Frail-D-A", "name": { "family": "Frail", "given": "Dale A." }, "role": "co-advisor" }, { "email": "smyers@aoc.nrao.esu", "id": "Myers-Steven-Theodore", "name": { "family": "Myers", "given": "Steven T." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "chair" }, { "email": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "orcid": "0000-0001-8638-0320", "role": "member" }, { "email": "smyers@aoc.nrao.edu", "id": "Myers-Steven-Theodore", "name": { "family": "Myers", "given": "Steven T." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-02-25", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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environments. There are an equally diverse number of methods by which we can study and characterize atmospheric composition. In order to better understand the fundamental chemistry and physical processes underlying all planetary atmospheres, my research of the past four years has focused on two distinct topics. First, I focused on the data analysis and spectral retrieval of observations obtained by the Ultraviolet Imaging Spectrograph (UVIS) instrument onboard the Cassini spacecraft while in orbit around Saturn. These observations consisted of stellar occultation measurements of Titan's upper atmosphere, probing the chemical composition in the region 300 to 1500 km above Titan's surface. I examined the relative abundances of Titan's two most prevalent chemical species, nitrogen and methane. I also focused on the aerosols that are formed through chemistry involving these two major species, and determined the vertical profiles of aerosol particles as a function of time and latitude. Moving beyond our own solar system, my second topic of investigation involved analysis of infra-red light curves from the Spitzer space telescope, obtained as it measured the light from stars hosting planets of their own. I focused on both transit and eclipse modeling during Spitzer data reduction and analysis. In my initial work, I utilized the data to search for transits of planets a few Earth masses in size. In more recent research, I analyzed secondary eclipses of three exoplanets and constrained the range of possible temperatures and compositions of their atmospheres.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:08312014-134619300", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08312014-134619300", "related_url": { "items": [ { "description": "Article adapted for ch. 3", "type": "doi", "url": "https://doi.org/10.1016/j.pss.2013.08.003" }, { "description": "Article adapted for ch. 5", "type": "doi", "url": "https://doi.org/10.1088/0004-637X/781/2/103" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Joshua Kammer", "deposited_on": "2014-10-03 17:18:46", "doi": "10.7907/Z9GX48HD", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "co-advisor" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "member" }, { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "member" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-09-25", "gradofc_approval_date": "2014-10-01", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/51645" } ] } } ], "eprint_status": "archive", "userid": 10341, "dir": "disk0/00/00/86/36", "datestamp": "2016-09-20 17:09:24", "lastmod": "2023-05-30 22:26:24", "status_changed": "2016-09-20 17:09:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ryan.f.trainor@gmail.com", "id": "Trainor-Ryan-Francis", "name": { "family": "Trainor", "given": "Ryan Francis" }, "show_email": "YES" } ] }, "title": "Faint Galaxies in the Megaparsec-Scale Environments of Hyperluminous QSOs at Redshifts 2 < z < 3", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology; galaxy formation; black holes; quasars; qsos", "abstract": "This thesis presents detailed observational studies of the extended distributions of gas, galaxies, and dark matter around hyperluminous quasars (HLQSOs) at high redshift. Taken together, these works aim to coherently describe the relationships between these massive, accreting black holes and their environments: the nature of the regions that give rise to such massive black holes, the effect of HLQSO radiation on their surrounding galaxies and gas, and the ability of both galaxies and black holes to shed new light on the formation and evolution of the other.
\r\n\r\nChapter 2 focuses on the continuum-color-selected galaxies drawn from the Keck Baryonic Structure Survey (KBSS). The KBSS is a uniquely deep spectroscopic survey of star-forming galaxies in the same volumes of space as 15 HLQSOs at 2.5 <
Chapter 3 describes the first results from a new survey (KBSS-Lyα) conducted for this thesis. The KBSS-Lyα survey uses narrowband imaging to identify Lyα-emitters (LAEs) in the ~Mpc regions around eight of the KBSS HLQSOs. Many of these LAEs show the effect of reprocessed HLQSO radiation in their emission through the process known as Lyα fluorescence. In this chapter, these fluorescent LAEs are used to generate a coarse map of the average HLQSO ionizing emission on Mpc scales, thereby setting the first direct constraints of the lifetime and angular distribution of activity for a population of these uniquely luminous black holes.
\r\n\r\nChapter 4 contains a more detailed description of the KBSS-Lyα survey itself and the detailed properties of the star-forming and fluorescent objects selected therein. Using imaging and spectroscopic data covering rest-frame UV and optical wavelengths, including spectra from the new near-infrared spectrometer MOSFIRE, we characterize this population of nascent galaxies in terms of their kinematics, enrichment, gas properties, and luminosity distribution while comparing and contrasting them with previously-studied populations of continuum-selected galaxies and LAEs far from the effects of HLQSO emission.
\r\n\r\nAt the conclusion of this thesis, I briefly present future directions for the continuation of this research. In Appendix A, I provide background information on the instrumentation used in this thesis, including my own contributions to MOSFIRE.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:08182014-123907723", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08182014-123907723", "referencetext": { "items": [ "\\begin{thebibliography}{159}\r\n\\expandafter\\ifx\\csname natexlab\\endcsname\\relax\\def\\natexlab#1{#1}\\fi\r\n\r\n\\bibitem[{{Adelberger}(2005)}]{ade05b}\r\n{Adelberger}, K.~L. 2005, \\apj, 621, 574\r\n\r\n\\bibitem[{{Adelberger} {et~al.}(2005{\\natexlab{a}}){Adelberger}, {Shapley},\r\n {Steidel}, {Pettini}, {Erb}, \\& {Reddy}}]{ade05d}\r\n{Adelberger}, K.~L., {Shapley}, A.~E., {Steidel}, C.~C., {Pettini}, M., {Erb},\r\n D.~K., \\& {Reddy}, N.~A. 2005{\\natexlab{a}}, \\apj, 629, 636\r\n\r\n\\bibitem[{{Adelberger} \\& {Steidel}(2005{\\natexlab{a}})}]{ade05e}\r\n{Adelberger}, K.~L. \\& {Steidel}, C.~C. 2005{\\natexlab{a}}, \\apj, 630, 50\r\n\r\n\\bibitem[{{Adelberger} \\& {Steidel}(2005{\\natexlab{b}})}]{ade05c}\r\n---. 2005{\\natexlab{b}}, \\apjl, 627, 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"Withheld until 15 August 2016. Released 9/20/2016.", "deposited_by": "Ryan Trainor", "deposited_on": "2016-09-20 17:09:24", "doi": "10.7907/Z90K26JG", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" }, { "email": "jak@obs.carnegiescience.edu", "id": "Kollmeier-J-A", "name": { "family": "Kollmeier", "given": "Juna A." }, "orcid": "0000-0001-9852-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-08-15", "gradofc_approval_date": "2014-08-20", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2015", "author_list": "Trainor, Ryan Francis" }, { "id": "/id/eprint/8598", "eprint_id": 8598, "rev_number": 39, "documents": [ { "id": "/id/document/51444", "doc_id": 51444, "rev_number": 2, "files": [ { "id": "/id/file/149341", "fileid": 149341, "datasetid": "document", "objectid": 51444, "filename": "mcguire_thesis_4.pdf", "mime_type": "application/pdf", "hash": "14fc701d492d7fabf0a4e84154c07b29", "hash_type": "MD5", "filesize": 6150630, "mtime": "2014-08-07 16:38:02", "url": "/8598/1/mcguire_thesis_4.pdf" } ], "eprint_id": 8598, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "mcguire_thesis_4.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"Understanding the origin of life on Earth has long fascinated the minds of the global community, and has been a driving factor in interdisciplinary research for centuries. Beyond the pioneering work of Darwin, perhaps the most widely known study in the last century is that of Miller and Urey, who examined the possibility of the formation of prebiotic chemical precursors on the primordial Earth [1]. More recent studies have shown that amino acids, the chemical building blocks of the biopolymers that comprise life as we know it on Earth, are present in meteoritic samples, and that the molecules extracted from the meteorites display isotopic signatures indicative of an extraterrestrial origin [2]. The most recent major discovery in this area has been the detection of glycine (NH2CH2COOH), the simplest amino acid, in pristine cometary samples returned by the NASA STARDUST mission [3]. Indeed, the open questions left by these discoveries, both in the public and scientific communities, hold such fascination that NASA has designated the understanding of our \"Cosmic Origins\" as a key mission priority.
\r\n\r\nDespite these exciting discoveries, our understanding of the chemical and physical pathways to the formation of prebiotic molecules is woefully incomplete. This is largely because we do not yet fully understand how the interplay between grain-surface and sub-surface ice reactions and the gas-phase affects astrophysical chemical evolution, and our knowledge of chemical inventories in these regions is incomplete. The research presented here aims to directly address both these issues, so that future work to understand the formation of prebiotic molecules has a solid foundation from which to work.
\r\n\r\nFrom an observational standpoint, a dedicated campaign to identify hydroxylamine (NH2OH), potentially a direct precursor to glycine, in the gas-phase was undertaken. No trace of NH2OH was found. These observations motivated a refinement of the chemical models of glycine formation, and have largely ruled out a gas-phase route to the synthesis of the simplest amino acid in the ISM. A molecular mystery in the case of the carrier of a series of transitions was resolved using observational data toward a large number of sources, confirming the identity of this important carbon-chemistry intermediate B11244 as l-C3H+ and identifying it in at least two new environments. Finally, the doubly-nitrogenated molecule carbodiimide HNCNH was identified in the ISM for the first time through maser emission features in the centimeter-wavelength regime.
\r\n\r\nIn the laboratory, a TeraHertz Time-Domain Spectrometer was constructed to obtain the experimental spectra necessary to search for solid-phase species in the ISM in the THz region of the spectrum. These investigations have shown a striking dependence on large-scale, long-range (i.e. lattice) structure of the ices on the spectra they present in the THz. A database of molecular spectra has been started, and both the simplest and most abundant ice species, which have already been identified, as well as a number of more complex species, have been studied. The exquisite sensitivity of the THz spectra to both the structure and thermal history of these ices may lead to better probes of complex chemical and dynamical evolution in interstellar environments.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:07232014-152145064", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:07232014-152145064", "referencetext": { "items": [ "[1] S. L. Miller and H. C. Urey, \u201cOrganic Compound Synthesis on the Primitive Earth,\u201d Science, 130, 245\u2013251 (1959).\r\n[2] O. Botta and J. L. Bada, \u201cExtraterrestrial organic compounds in meteorites,\u201d Surveys in Geophysics, 23, 411\u2013467 (2002).\r\n[3] J. E. Elsila, D. P. Glavin, and J. P. Dworkin, \u201cCometary glycine detected in samples returned by Stardust,\u201d Meteoritics & Planetary Science, 44, 1323\u20131330 (2009).\r\n[4] R. L. Pulliam, B. A. McGuire, and A. J. Remijan, \u201cA search for hydroxylamine (NH2OH) toward select astronomical sources,\u201d The Astrophysical Journal, 751, 1 (2012).\r\n[5] V. Blagojevic, S. Petrie, and D. K. 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Emprechtinger et al., \u201cBroadband analysis techniques for Herschel/HIFI spectral surveys of chemically rich star-forming regions,\u201d Journal of Molecular Spectroscopy, 280, 150\u2013154 (2012)." ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "GP", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Brett McGuire", "deposited_on": "2014-08-08 22:09:18", "doi": "10.7907/Z9B27S79", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "hbgray@caltech.edu", "id": "Gray-H-B", "name": { "family": "Gray", "given": "Harry B." }, "orcid": "0000-0002-7937-7876", "role": "chair" }, { "email": "mo@caltech.edu", "id": "Okumura-M", "name": { "family": "Okumura", "given": "Mitchio" }, "orcid": "0000-0001-6874-1137", "role": "member" }, { "email": "ram@caltech.edu", "id": "Marcus-R-A", "name": { "family": "Marcus", "given": "Rudolph A." }, "orcid": "0000-0001-6547-1469", "role": "member" }, { "email": "aremijan@nrao.edu", "id": "Remijan-A-J", "name": { "family": "Remijan", "given": "Anthony J." }, "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-05-21", "gradofc_approval_date": "2014-08-08", "thesis_awards": "Everhart Distinguished Graduate Student Lecture Series, 2014", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/53372" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/53372" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/53372" } ] } } ], "eprint_status": "archive", "userid": 10446, "dir": "disk0/00/00/87/39", "datestamp": "2014-12-12 22:33:33", "lastmod": "2021-10-26 18:25:45", "status_changed": "2014-12-12 22:33:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "doc.aronnax@gmail.com", "id": "Singer-Leo-Pound", "name": { "family": "Singer", "given": "Leo Pound" }, "orcid": "0000-0001-9898-5597", "show_email": "NO" } ] }, "title": "The Needle in the 100 deg\u00b2 Haystack: The Hunt for Binary Neutron Star Mergers with LIGO and Palomar Transient Factory", "ispublished": "unpub", "full_text_status": "public", "keywords": "Laser Interferometer Gravitational-Wave Observatory; LIGO; PTF; gravitational waves; compact binary coalescence; CBC; binary neutron star mergers; BNS; gamma-ray bursts; GRB; signal processing; Bayesian inference; parameter estimation; optical transients; optical counterparts; multimessenger", "abstract": "The Advanced LIGO and Virgo experiments are poised to detect gravitational waves (GWs) directly for the first time this decade. The ultimate prize will be joint observation of a compact binary merger in both gravitational and electromagnetic channels. However, GW sky locations that are uncertain by hundreds of square degrees will pose a challenge. I describe a real-time detection pipeline and a rapid Bayesian parameter estimation code that will make it possible to search promptly for optical counterparts in Advanced LIGO. Having analyzed a comprehensive population of simulated GW sources, we describe the sky localization accuracy that the GW detector network will achieve as each detector comes online and progresses toward design sensitivity. Next, in preparation for the optical search with the intermediate Palomar Transient Factory (iPTF), we have developed a unique capability to detect optical afterglows of gamma-ray bursts (GRBs) detected by the Fermi Gamma-ray Burst Monitor (GBM). Its comparable error regions offer a close parallel to the Advanced LIGO problem, but Fermi's unique access to MeV-GeV photons and its near all-sky coverage may allow us to look at optical afterglows in a relatively unexplored part of the GRB parameter space. We present the discovery and broadband follow-up observations (X-ray, UV, optical, millimeter, and radio) of eight GBM-IPTF afterglows. Two of the bursts (GRB 130702A / iPTF13bxl and GRB 140606B / iPTF14bfu) are at low redshift (z=0.145 and z = 0.384, respectively), are sub-luminous with respect to \"standard\" cosmological bursts, and have spectroscopically confirmed broad-line type Ic supernovae. These two bursts are possibly consistent with mildly relativistic shocks breaking out from the progenitor envelopes rather than the standard mechanism of internal shocks within an ultra-relativistic jet. On a technical level, the GBM--IPTF effort is a prototype for locating and observing optical counterparts of GW events in Advanced LIGO with the Zwicky Transient Facility.", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:12102014-223122387", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:12102014-223122387", "related_url": { "items": [ { "description": "Refereed publication corresponding to Chapter 3", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/748/2/136" }, { "description": "Refereed publication corresponding to Chapter 5", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/795/2/105" }, { "description": "Refereed publication corresponding to Chapter 6", "type": "doi", "url": "http://dx.doi.org/10.1088/2041-8205/776/2/L34" }, { "description": "Online supplemental data corresponding to Appendix D", "type": "doc", "url": "http://ligo.org/scientists/first2years/" } ] }, "projects": { "items": [ "LIGO", "Virgo", "Palomar Transient Factory", "Zwicky Transient Facility" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "John and Ursula Kanel Foundation Charitable Scholarship" }, { "agency": "NSF", "grant_number": "PHY-0107417" }, { "agency": "Swift Guest Investigator Program Cycle 9", "grant_number": "NNX14AC24G" }, { "agency": "Swift Guest Investigator Program Cycle 10", "grant_number": "NNX14AI99G" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "other_numbering_system": { "items": [ { "id": "P1400223-v10", "name": "LIGO" } ] }, "local_group": { "items": [ "LIGO", "Palomar Transient Factory", "Astronomy Department" ] }, "deposited_by": "Leo Singer", "deposited_on": "2014-12-12 22:33:33", "doi": "10.7907/Z9ZP442V", "alt_title": { "items": [ "The Needle in the hundred square degree Haystack: The Hunt for Binary Neutron Star Mergers with LIGO and Palomar Transient Factory" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ajw@ligo.caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "advisor" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "ajw@ligo.caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "cott@tapir.caltech.edu", "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055", "role": "member" }, { "email": "reitze@ligo.caltech.edu", "id": "Reitze-D-H", "name": { "family": "Reitze", "given": "David H." }, "orcid": "0000-0002-5756-1111", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-11-24", "gradofc_approval_date": "2014-12-12", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2015", "author_list": "Singer, Leo Pound" }, { "id": "/id/eprint/8883", "eprint_id": 8883, "rev_number": 35, "documents": [ { "id": "/id/document/56500", "doc_id": 56500, "rev_number": 3, "files": [ { "id": "/id/file/160689", "fileid": 160689, "datasetid": "document", "objectid": 56500, "filename": "main.pdf", "mime_type": "application/pdf", "hash": "130f3c7b3e801ee214ba474f73f46a4e", "hash_type": "MD5", "filesize": 3935814, "mtime": "2015-05-23 01:18:24", "url": "/8883/1/main.pdf" } ], "eprint_id": 8883, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete thesis", "language": "en", "security": "public", "license": "other", "main": "main.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"uri": "/id/document/56500" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/56500" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/56500" } ] } } ], "eprint_status": "archive", "userid": 7038, "dir": "disk0/00/00/88/83", "datestamp": "2015-06-04 22:54:56", "lastmod": "2023-11-08 00:16:42", "status_changed": "2015-06-04 22:54:56", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "zhangkebnu@gmail.com", "id": "Zhang-Ke", "name": { "family": "Zhang", "given": "Ke" }, "orcid": "0000-0002-0661-7517", "show_email": "NO" } ] }, "title": "Volatiles in Protoplanetary Disks", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astrochemistry, protoplanetary disks, planetary systems", "abstract": "Planets are assembled from the gas, dust, and ice in the accretion disks that encircle young stars. Ices of chemical compounds with low condensation temperatures (<200 K), the so-called volatiles, dominate the solid mass reservoir from which planetesimals are formed and are thus available to build the protoplanetary cores of gas/ice giant planets. It has long been thought that the regions near the condensation fronts of volatiles are preferential birth sites of planets. Moreover, the main volatiles in disks are also the main C-and O-containing species in (exo)planetary atmospheres. Understanding the distribution of volatiles in disks and their role in planet-formation processes is therefore of great interest.
\r\n\r\nThis thesis addresses two fundamental questions concerning the nature of volatiles in planet-forming disks: (1) how are volatiles distributed throughout a disk, and (2) how can we use volatiles to probe planet-forming processes in disks? We tackle the first question in two complementary ways. We have developed a novel super-resolution method to constrain the radial distribution of volatiles throughout a disk by combining multi-wavelength spectra. Thanks to the ordered velocity and temperature profiles in disks, we find that detailed constraints can be derived even with spatially and spectrally unresolved data -- provided a wide range of energy levels are sampled. We also employ high-spatial resolution interferometric images at (sub)mm frequencies using the Atacama Large Millimeter Array (ALMA) to directly measure the radial distribution of volatiles.
\r\n\r\nFor the second question, we combine volatile gas emission measurements with those of the dust continuum emission or extinction to understand dust growth mechanisms in disks and disk instabilities at planet-forming distances from the central star. Our observations and models support the idea that the water vapor can be concentrated in regions near its condensation front at certain evolutionary stages in the lifetime of protoplanetary disks, and that fast pebble growth is likely to occur near the condensation fronts of various volatile species.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:05222015-173941425", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05222015-173941425", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Lindsay Cleary", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Ke Zhang", "deposited_on": "2015-06-04 22:54:56", "doi": "10.7907/Z9VQ30MD", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-05-15", "gradofc_approval_date": "2015-06-04", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/56900" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/56900" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/56900" } ] } } ], "eprint_status": "archive", "userid": 2892, "dir": "disk0/00/00/88/96", "datestamp": "2015-05-28 23:57:39", "lastmod": "2020-03-10 19:19:29", "status_changed": "2015-05-28 23:57:39", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jcg051987@gmail.com", "id": "Ji-Chenguang", "name": { "family": "Ji", "given": "Chenguang" }, "show_email": "YES" } ] }, "title": "Design of Antenna-Coupled Lumped-Element Titanium Nitride KIDs for LongWavelength Multi-Band Continuum Imaging", "ispublished": "unpub", "full_text_status": "public", "keywords": "sensors, low-temperature detectors, bolometers, submillimeter-wave and millimeter-wave receivers and detectors, kinetic inductance detectors, radio telescopes and instrumentation", "abstract": "Many applications in cosmology and astrophysics at millimeter wavelengths including CMB polarization, studies of galaxy clusters using the Sunyaev-Zeldovich effect (SZE), and studies of star formation at high redshift and in our local universe and our galaxy, require large-format arrays of millimeter-wave detectors. Feedhorn and phased-array antenna architectures for receiving mm-wave light present numerous advantages for control of systematics, for simultaneous coverage of both polarizations and/or multiple spectral bands, and for preserving the coherent nature of the incoming light. This enables the application of many traditional \"RF\" structures such as hybrids, switches,\r\nand lumped-element or microstrip band-defining filters.
\r\n\r\nSimultaneously, kinetic inductance detectors (KIDs) using high-resistivity materials like titanium nitride are an attractive sensor option for large-format arrays because they are highly multiplexable and because they can have sensitivities reaching the condition of background-limited detection. A\r\nKID is a LC resonator. Its inductance includes the geometric inductance and kinetic inductance of the inductor in the superconducting phase. A photon absorbed by the superconductor breaks a Cooper pair into normal-state electrons and perturbs its kinetic inductance, rendering it a detector\r\nof light. The responsivity of KID is given by the fractional frequency shift of the LC resonator per unit optical power.
\r\n\r\nHowever, coupling these types of optical reception elements to KIDs is a challenge because of the impedance mismatch between the microstrip transmission line exiting these architectures and the high resistivity of titanium nitride. Mitigating direct absorption of light through free space coupling to the inductor of KID is another challenge. We present a detailed titanium nitride KID\r\ndesign that addresses these challenges. The KID inductor is capacitively coupled to the microstrip in such a way as to form a lossy termination without creating an impedance mismatch. A parallel plate capacitor design mitigates direct absorption, uses hydrogenated amorphous silicon, and yields acceptable noise. We show that the optimized design can yield expected sensitivities very close to\r\nthe fundamental limit for a long wavelength imager (LWCam) that covers six spectral bands from 90 to 400 GHz for SZE studies.
\r\n\r\nExcess phase (frequency) noise has been observed in KID and is very likely caused by two-level systems (TLS) in dielectric materials. The TLS hypothesis is supported by the measured dependence of the noise on resonator internal power and temperature. However, there is still a lack of a unified microscopic theory which can quantitatively model the properties of the TLS noise. In this thesis we\r\nderive the noise power spectral density due to the coupling of TLS with phonon bath based on an existing model and compare the theoretical predictions about power and temperature dependences with experimental data. We discuss the limitation of such a model and propose the direction for future study.
", "date": "2015", "date_type": "degree", "id_number": "CaltechTHESIS:05282015-121920930", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05282015-121920930", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Lindsay Cleary", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Restricted to Caltech community only until 12 June 2016. Released 6/14/2016.", "deposited_by": "Chenguang Ji", "deposited_on": "2015-05-28 23:57:39", "doi": "10.7907/Z9W66HQ7", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "chair" }, { "email": "wag@wag.caltech.edu", "id": "Goddard-W-A-III", "name": { "family": "Goddard", "given": "William A., III" }, "role": "member" }, { "email": "wlj@caltech.edu", "id": "Johnson-W-L", "name": { "family": "Johnson", "given": "William L." }, "role": "member" }, { "email": "rutledge@caltech.edu", "id": "Rutledge-D-B", "name": { "family": "Rutledge", "given": "David B." }, "role": "member" }, { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2015-05-18", "gradofc_approval_date": "2015-05-28", "review_status": "approved", "option_major": { "items": [ "matsci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2015", "author_list": "Ji, Chenguang" }, { "id": "/id/eprint/7904", "eprint_id": 7904, "rev_number": 37, "documents": [ { "id": "/id/document/42137", "doc_id": 42137, "rev_number": 2, "files": [ { "id": "/id/file/126738", "fileid": 126738, "datasetid": "document", "objectid": 42137, "filename": "zhang_fan_2014_thesis.pdf", "mime_type": "application/pdf", "hash": "0b841d19070b950bbd2c57ab3d5eb026", "hash_type": "MD5", "filesize": 23829729, "mtime": "2013-06-20 23:15:11", "url": "/7904/1/zhang_fan_2014_thesis.pdf" } ], "eprint_id": 7904, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "zhang_fan_2014_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/42137" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/42137" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/42137" } ] } } ], "eprint_status": "archive", "userid": 9955, "dir": "disk0/00/00/79/04", "datestamp": "2013-07-29 17:48:54", "lastmod": "2021-10-26 18:31:11", "status_changed": "2013-07-29 17:48:54", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "fanzfanzh25@gmail.com", "id": "Zhang-Fan", "name": { "family": "Zhang", "given": "Fan" }, "show_email": "YES" } ] }, "title": "Tools for the Study of Dynamical Spacetimes", "ispublished": "unpub", "full_text_status": "public", "keywords": "bifurcation of mode spectrum, quasi-normal modes, quasi-Kinnersley tetrad, tendex and vortex, gauge invariance", "abstract": "This thesis covers a range of topics in numerical and analytical relativity, centered around introducing tools and methodologies for the study of dynamical spacetimes. The scope of the studies is limited to classical (as opposed to quantum) vacuum spacetimes described by Einstein's general theory of relativity. The numerical works presented here are carried out within the Spectral Einstein Code (SpEC) infrastructure, while analytical calculations extensively utilize Wolfram's Mathematica program.
\r\n\r\nWe begin by examining highly dynamical spacetimes such as binary black hole mergers, which can be investigated using numerical simulations. However, there are difficulties in interpreting the output of such simulations. One difficulty stems from the lack of a canonical coordinate system (henceforth referred to as gauge freedom) and tetrad, against which quantities such as Newman-Penrose Psi_4 (usually interpreted as the gravitational wave part of curvature) should be measured. We tackle this problem in Chapter 2 by introducing a set of geometrically motivated coordinates that are independent of the simulation gauge choice, as well as a quasi-Kinnersley tetrad, also invariant under gauge changes in addition to being optimally suited to the task of gravitational wave extraction.
\r\n\r\nAnother difficulty arises from the need to condense the overwhelming amount of data generated by the numerical simulations. In order to extract physical information in a succinct and transparent manner, one may define a version of gravitational field lines and field strength using spatial projections of the Weyl curvature tensor. Introduction, investigation and utilization of these quantities will constitute the main content in Chapters 3 through 6.
\r\n\r\nFor the last two chapters, we turn to the analytical study of a simpler dynamical spacetime, namely a perturbed Kerr black hole. We will introduce in Chapter 7 a new analytical approximation to the quasi-normal mode (QNM) frequencies, and relate various properties of these modes to wave packets traveling on unstable photon orbits around the black hole. In Chapter 8, we study a bifurcation in the QNM spectrum as the spin of the black hole a approaches extremality.
\r\n", "date": "2014", "date_type": "degree", "id_number": "CaltechTHESIS:06192013-175010723", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06192013-175010723", "related_url": { "items": [ { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.86.084020" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.84.124014" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.84.044037" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.86.084049" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.86.104028" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.86.104006" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.87.041502" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0653653" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "NSF", "grant_number": "PHY-1005655" }, { "agency": "NSF", "grant_number": "PHY-0960291" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "Brinson Foundation" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Fan Zhang", "deposited_on": "2013-07-29 17:48:54", "doi": "10.7907/Z9WD3XHF", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "advisor" }, { "email": "yanbei.chen@gmail.com", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei.chen@gmail.com", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "chair" }, { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "member" }, { "email": "bela@caltech.edu", "id": "Szilagyi-B", "name": { "family": "Szilagyi", "given": "Bela" }, "role": "member" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-06-17", "gradofc_approval_date": "2013-07-25", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2014", "author_list": "Zhang, Fan" }, { "id": "/id/eprint/8197", "eprint_id": 8197, "rev_number": 32, "documents": [ { "id": "/id/document/47335", "doc_id": 47335, "rev_number": 5, "files": [ { "id": "/id/file/138474", "fileid": 138474, "datasetid": "document", "objectid": 47335, "filename": "Holland_thesis_final.pdf", "mime_type": "application/pdf", "hash": "66921b3cce8fa78126f9420e9fa34a34", "hash_type": "MD5", "filesize": 7943636, "mtime": "2014-04-22 20:33:23", "url": "/8197/1/Holland_thesis_final.pdf" } ], "eprint_id": 8197, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Holland_thesis_final.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"/id/document/47335" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/47335" } ] } } ], "eprint_status": "archive", "userid": 10210, "dir": "disk0/00/00/81/97", "datestamp": "2016-09-19 23:43:13", "lastmod": "2023-11-08 00:16:42", "status_changed": "2016-09-19 23:43:13", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "thz@danielbholland.com", "id": "Holland-Daniel-Brian", "name": { "family": "Holland", "given": "Daniel Brian" }, "show_email": "NO" } ] }, "title": "Design, Construction, and Applications of a High-Resolution Terahertz Time-Domain Spectrometer", "ispublished": "unpub", "full_text_status": "public", "keywords": "THz;spectroscopy;water;phonon;ASOPS;thermal conductivity ", "abstract": "This thesis reports on the design, construction, and initial applications of a high-resolution terahertz time-domain ASOPS spectrometer. The instrument employs asynchronous optical sampling (ASOPS) between two Ti:sapphire ultrafast lasers operating at a repetition rate of approximately 80 MHz, and we thus demonstrate a THz frequency resolution approaching the limit of that repetition rate. This is an order of magnitude improvement in resolution over typical THz time-domain spectrometers. The improved resolution is important for our primary effort of collecting THz spectra for far-infrared astronomy. We report on various spectroscopic applications including the THz rotational spectrum of water, where we achieve a mean frequency error, relative to established line centers, of 27.0 MHz. We also demonstrate application of the THz system to the long-duration observation of a coherent magnon mode in a anti-ferromagnetic yttrium iron oxide (YFeO3) crystal. Furthermore, we apply the all-optical virtual delay line of ASOPS to a transient thermoreflectance experiment for quickly measuring the thermal conductivity of semiconductors.", "date": "2014", "date_type": "degree", "id_number": "CaltechTHESIS:04222014-120506633", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04222014-120506633", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Karthy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Withheld until 22 April 2016. Released 9/19/2016", "deposited_by": "Daniel Holland", "deposited_on": "2016-09-19 23:43:13", "doi": "10.7907/Z91J97QR", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "heath@caltech.edu", "id": "Heath-J-R", "name": { "family": "Heath", "given": "James R." }, "orcid": "0000-0001-5356-4385", "role": "chair" }, { "email": "jlbchamp@caltech.edu", "id": "Beauchamp-J-L", "name": { "family": "Beauchamp", "given": "Jesse L." }, "role": "member" }, { "email": "dcrees@caltech.edu", "id": "Rees-D-C", "name": { "family": "Rees", "given": "Douglas C." }, "orcid": "0000-0003-4073-1185", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-04-18", "gradofc_approval_date": "2014-04-22", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2014", "author_list": "Holland, Daniel Brian" }, { "id": "/id/eprint/7966", "eprint_id": 7966, "rev_number": 30, "documents": [ { "id": "/id/document/43331", "doc_id": 43331, "rev_number": 2, "files": [ { "id": "/id/file/129087", "fileid": 129087, "datasetid": "document", "objectid": 43331, "filename": "stevenson_matthew_2014_thesis.pdf", "mime_type": "application/pdf", "hash": "6abe0bd80c285ae7f64a887717b6e98c", "hash_type": "MD5", "filesize": 13045735, "mtime": "2013-09-30 01:29:45", "url": "/7966/1/stevenson_matthew_2014_thesis.pdf" } ], "eprint_id": 7966, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "stevenson_matthew_2014_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/43331" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/43331" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/43331" } ] } } ], "eprint_status": "archive", "userid": 10057, "dir": "disk0/00/00/79/66", "datestamp": "2013-11-20 17:47:01", "lastmod": "2023-05-30 22:27:34", "status_changed": "2013-11-20 17:47:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "matthewalanstevenson@gmail.com", "id": "Stevenson-Matthew-Alan", "name": { "family": "Stevenson", "given": "Matthew Alan" }, "show_email": "NO" } ] }, "title": "Observational and Theoretical Advances in Cosmological Foreground Emission", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology; Cosmological foreground emission; Interstellar dust; Interstellar medium; Wide-area astronomy survey; Radio astronomy instrumentation", "abstract": "Observational and theoretical work towards the separation of foreground emission from the cosmic microwave background is described. The bulk of this work is in the design, construction, and commissioning of the C-Band All-Sky Survey (C-BASS), an experiment to produce a template of the Milky Way Galaxy's polarized synchrotron emission. Theoretical work is the derivation of an analytical approximation to the emission spectrum of spinning dust grains.
\r\n\r\nThe performance of the C-BASS experiment is demonstrated through a preliminary, deep survey of the North Celestial Pole region. A comparison to multiwavelength data is performed, and the thermal and systematic noise properties of the experiment are explored. The systematic noise has been minimized through careful data processing algorithms, implemented both in the experiment's Field Programmable Gate Array (FPGA) based digital backend and in the data analysis pipeline. Detailed descriptions of these algorithms are presented.
\r\n\r\nThe analytical function of spinning dust emission is derived through the application of careful approximations, with each step tested against numerical calculations. This work is intended for use in the parameterized separation of cosmological foreground components and as a framework for interpreting and comparing the variety of anomalous microwave emission observations.
\r\n", "date": "2014", "date_type": "degree", "id_number": "CaltechTHESIS:09292013-182521898", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09292013-182521898", "related_url": { "items": [ { "description": "Journal Article", "type": "related", "url": "http://resolver.caltech.edu/CaltechAUTHORS:20190301-092706950" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Matthew Stevenson", "deposited_on": "2013-11-20 17:47:01", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "chair" }, { "email": "golwala@astro.caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "tjp@astro.caltech.edu", "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "Timothy J." }, "orcid": "0000-0001-5213-6231", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-06-12", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2014", "author_list": "Stevenson, Matthew Alan" }, { "id": "/id/eprint/8389", "eprint_id": 8389, "rev_number": 26, "documents": [ { "id": "/id/document/48365", "doc_id": 48365, "rev_number": 5, "files": [ { "id": "/id/file/141059", "fileid": 141059, "datasetid": "document", "objectid": 48365, "filename": "Yang_Da_2014_Thesis.pdf", "mime_type": "application/pdf", "hash": "b1a8614d07180a6cfdc52c2b5cf588fa", "hash_type": "MD5", "filesize": 17079781, "mtime": "2014-05-23 18:43:02", "url": "/8389/1/Yang_Da_2014_Thesis.pdf" } ], "eprint_id": 8389, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Yang_Da_2014_Thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/129024", "doc_id": 129024, "rev_number": 1, "files": [ { "id": "/id/file/374460", "fileid": 374460, "datasetid": "document", "objectid": 129024, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "324655a4d98c24685644d1b15a7ceaf1", "hash_type": "MD5", "filesize": 19740, "mtime": "2021-06-24 03:25:51", "url": "/8389/8/indexcodes.txt" } ], "eprint_id": 8389, "pos": 8, "placement": 8, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/48365" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/48365" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/48365" } ] } } ], "eprint_status": "archive", "userid": 9729, "dir": "disk0/00/00/83/89", "datestamp": "2014-05-29 21:36:10", "lastmod": "2020-03-11 18:42:47", "status_changed": "2014-05-29 21:36:10", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "yangdapku@gmail.com", "id": "Yang-Da", "name": { "family": "Yang", "given": "Da" }, "show_email": "NO" } ] }, "title": "The Madden-Julian Oscillation: Observation, Modeling, and Theory", "ispublished": "unpub", "full_text_status": "public", "keywords": "The Madden-Julian Oscillation; Atmospheric Convection; Equatorial Waves; Tropical Meteorology", "abstract": "The Madden-Julian Oscillation (MJO) is a pattern of intense rainfall and associated planetary-scale circulations in the tropical atmosphere, with a recurrence interval of 30-90 days. Although the MJO was first discovered 40 years ago, it is still a challenge to simulate the MJO in general circulation models (GCMs), and even with simple models it is difficult to agree on the basic mechanisms. This deficiency is mainly due to our poor understanding of moist convection\u2014deep cumulus clouds and thunderstorms, which occur at scales that are smaller than the resolution elements of the GCMs. Moist convection is the most important mechanism for transporting energy from the ocean to the atmosphere. Success in simulating the MJO will improve our understanding of moist convection and thereby improve weather and climate forecasting.
\r\n\r\nWe address this fundamental subject by analyzing observational datasets, constructing a hierarchy of numerical models, and developing theories. Parameters of the models are taken from observation, and the simulated MJO fits the data without further adjustments. The major findings include: 1) the MJO may be an ensemble of convection events linked together by small-scale high-frequency inertia-gravity waves; 2) the eastward propagation of the MJO is determined by the difference between the eastward and westward phase speeds of the waves; 3) the planetary scale of the MJO is the length over which temperature anomalies can be effectively smoothed by gravity waves; 4) the strength of the MJO increases with the typical strength of convection, which increases in a warming climate; 5) the horizontal scale of the MJO increases with the spatial frequency of convection; and 6) triggered convection, where potential energy accumulates until a threshold is reached, is important in simulating the MJO. Our findings challenge previous paradigms, which consider the MJO as a large-scale mode, and point to ways for improving the climate models.
", "date": "2014", "date_type": "degree", "id_number": "CaltechTHESIS:05232014-112348842", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05232014-112348842", "related_url": { "items": [ { "description": "Article adapted for Ch. 2: Testing the Hypothesis that the MJO is a Mixed Rossby-Gravity Wave Packet ", "type": "pub", "url": "http://dx.doi.org/10.1175/2010JAS3563.1" }, { "description": "Article adapted for Ch. 3: Triggered Convection, Gravity Waves, and the MJO: A Shallow-Water Model", "type": "pub", "url": "http:///dx.doi.org/10.1175/JAS-D-12-0255.1" }, { "description": "Article adapted for Ch. 4: A theory of the MJO horizontal scale", "type": "pub", "url": "http://dx.doi.org/10.1002/2013GL058542" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Restricted to Caltech community only until 2 September 2016. Released 04/28/2016", "deposited_by": "Da Yang", "deposited_on": "2014-05-29 21:36:10", "doi": "10.7907/N1D7-1T85", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "bordoni@gps.caltech.edu", "id": "Bordoni-S", "name": { "family": "Bordoni", "given": "Simona" }, "role": "chair" }, { "email": "andrewt@caltech.edu", "id": "Thompson-A-F", "name": { "family": "Thompson", "given": "Andrew F." }, "role": "member" }, { "email": "duane.waliser@jpl.nasa.gov", "id": "Waliser-D-E", "name": { "family": "Waliser", "given": "Duane E." }, "role": "member" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-05-09", "gradofc_approval_date": "2014-05-28", "review_status": "approved", "option_major": { "items": [ "envreng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2014", "author_list": "Yang, Da" }, { "id": "/id/eprint/8031", "eprint_id": 8031, "rev_number": 42, "documents": [ { "id": "/id/document/43919", "doc_id": 43919, "rev_number": 2, "files": [ { "id": "/id/file/130658", "fileid": 130658, "datasetid": "document", "objectid": 43919, "filename": "Tendulkar_Shriharsh_P_Astrophysics_2013_Aug_26_v3.pdf", "mime_type": "application/pdf", "hash": "fea63f949be74e0f24a9ec0be0ed0844", "hash_type": "MD5", "filesize": 44672205, "mtime": "2013-11-20 19:25:25", "url": "/8031/7/Tendulkar_Shriharsh_P_Astrophysics_2013_Aug_26_v3.pdf" } ], "eprint_id": 8031, "pos": 7, "placement": 7, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete Thesis", "language": "en", "security": "public", "license": "other", "main": "Tendulkar_Shriharsh_P_Astrophysics_2013_Aug_26_v3.pdf", 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"media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/43919" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/43919" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/43919" } ] } } ], "eprint_status": "archive", "userid": 5772, "dir": "disk0/00/00/80/31", "datestamp": "2014-01-27 20:18:27", "lastmod": "2023-05-30 22:28:11", "status_changed": "2014-01-27 20:18:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "shriharsh@gmail.com", "id": "Tendulkar-Shriharsh-Prakash", "name": { "family": "Tendulkar", "given": "Shriharsh Prakash" }, "show_email": "NO" } ] }, "title": "Beyond the Blur: Construction and Characterization of the First Autonomous AO System and an AO Survev of Magnetar Proper Motions", "ispublished": "unpub", "full_text_status": "public", "keywords": "Adaptive Optics; Magnetars; Kinematics; Astrometry; Neutron Stars", "abstract": "Adaptive optics (AO) corrects distortions created by atmospheric turbulence and delivers diffraction-limited images on ground-based telescopes. The vastly improved spatial resolution and sensitivity has been utilized for studying everything from the magnetic fields of sunspots upto the internal dynamics of high-redshift galaxies. This thesis about AO science from small and large telescopes is divided into two parts: Robo-AO and magnetar kinematics.
\r\n\r\nIn the first part, I discuss the construction and performance of the world\u2019s first fully autonomous visible light AO system, Robo-AO, at the Palomar 60-inch telescope. Robo-AO operates extremely efficiently with an overhead < 50s, typically observing about 22 targets every hour. We have performed large AO programs observing a total of over 7,500 targets since May 2012. In the visible band, the images have a Strehl ratio of about 10% and achieve a contrast of upto 6 magnitudes at a separation of 1\u2032\u2032. The full-width at half maximum achieved is 110\u2013130 milli-arcsecond. I describe how Robo-AO is used to constrain the evolutionary models of low-mass pre-main-sequence stars by measuring resolved spectral energy distributions of stellar multiples in the visible band, more than doubling the current sample. I conclude this part with a discussion of possible future improvements to the Robo-AO system.
\r\n\r\nIn the second part, I describe a study of magnetar kinematics using high-resolution near-infrared (NIR) AO imaging from the 10-meter Keck II telescope. Measuring the proper motions of five magnetars with a precision of upto 0.7 milli-arcsecond/yr, we have more than tripled the previously known sample of magnetar proper motions and proved that magnetar kinematics are equivalent to those of radio pulsars. We conclusively showed that SGR 1900+14 and SGR 1806-20 were ejected from the stellar clusters with which they were traditionally associated. The inferred kinematic ages of these two magnetars are 6\u00b11.8 kyr and 650\u00b1300 yr respectively. These ages are a factor of three to four times greater than their respective characteristic ages. The calculated braking index is close to unity as compared to three for the vacuum dipole model and 2.5-2.8 as measured for young pulsars. I conclude this section by describing a search for NIR counterparts of new magnetars and a future promise of polarimetric investigation of a magnetars\u2019 NIR emission mechanism.
", "date": "2014", "date_type": "degree", "id_number": "CaltechTHESIS:11192013-181748112", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:11192013-181748112", "related_url": { "items": [ { "description": "Author's web-page", "type": "author", "url": "http://www.astro.caltech.edu/~spt" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Shriharsh Tendulkar", "deposited_on": "2014-01-27 20:18:27", "doi": "10.7907/7YS5-1P75", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "prince@srl.caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-08-26", "gradofc_approval_date": "2014-01-23", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2014", "author_list": "Tendulkar, Shriharsh Prakash" }, { "id": "/id/eprint/8448", "eprint_id": 8448, "rev_number": 27, "documents": [ { "id": "/id/document/49673", "doc_id": 49673, "rev_number": 2, "files": [ { "id": "/id/file/143787", "fileid": 143787, "datasetid": "document", "objectid": 49673, "filename": "Tucker_PhDthesis.pdf", "mime_type": "application/pdf", "hash": "90300b7bb54778b12a4dadafcfe2fe8f", "hash_type": "MD5", "filesize": 47614875, "mtime": "2014-05-31 00:13:16", "url": "/8448/1/Tucker_PhDthesis.pdf" } ], "eprint_id": 8448, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Tucker_PhDthesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/49673" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/49673" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/49673" } ] } } ], "eprint_status": "archive", "userid": 10269, "dir": "disk0/00/00/84/48", "datestamp": "2014-06-03 18:56:02", "lastmod": "2021-10-26 17:28:08", "status_changed": "2014-06-03 18:56:02", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "beckytucker86@gmail.com", "id": "Tucker-Rebecca-Suzanne", "name": { "family": "Tucker", "given": "Rebecca Suzanne" }, "show_email": "NO" } ] }, "title": "Characterization of Detectors and Instrument Systematics for the SPIDER CMB Polarimeter", "ispublished": "unpub", "full_text_status": "public", "keywords": "CMB, polarization, inflation, bolometer", "abstract": "We know from the CMB and observations of large-scale structure that the universe is extremely flat, homogenous, and isotropic. The current favored mechanism for generating these characteristics is inflation, a theorized period of exponential expansion of the universe that occurred shortly after the Big Bang. Most theories of inflation generically predict a background of stochastic gravitational waves. These gravitational waves should leave their unique imprint on the polarization of the CMB via Thompson scattering. Scalar perturbations of the metric will cause a pattern of polarization with no curl (E-mode). Tensor perturbations (gravitational waves) will cause a unique pattern of polarization on the CMB that includes a curl component (B-mode). A measurement of the ratio of the tensor to scalar perturbations (r) tells us the energy scale of inflation. Recent measurements by the BICEP2 team detect the B-mode spectrum with a tensor-to-scalar ratio of r = 0.2 (+0.05, \u22120.07). An independent confirmation of this result is the next step towards understanding the inflationary universe.
\r\n\r\nThis thesis describes my work on a balloon-borne polarimeter called SPIDER, which is designed to illuminate the physics of the early universe through measurements of the cosmic microwave background polarization. SPIDER consists of six single-frequency, on-axis refracting telescopes contained in a shared-vacuum liquid-helium cryostat. Its large format arrays of millimeter-wave detectors and tight control of systematics will give it unprecedented sensitivity. This thesis describes how the SPIDER detectors are characterized and calibrated for flight, as well as how the systematics requirements for the SPIDER system are simulated and measured.
", "date": "2014", "date_type": "degree", "id_number": "CaltechTHESIS:05302014-170605877", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302014-170605877", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Rebecca Tucker", "deposited_on": "2014-06-03 18:56:02", "doi": "10.7907/HNHF-HA43", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "chair" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "member" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2014-05-19", "gradofc_approval_date": "2014-06-02", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2014", "author_list": "Tucker, Rebecca Suzanne" }, { "id": "/id/eprint/8024", "eprint_id": 8024, "rev_number": 29, "documents": [ { "id": "/id/document/43857", "doc_id": 43857, "rev_number": 2, "files": [ { "id": "/id/file/130490", "fileid": 130490, "datasetid": "document", "objectid": 43857, "filename": "thesis_Morton.pdf", "mime_type": "application/pdf", "hash": "8f81cd0ea85fe588381487928516e01a", "hash_type": "MD5", "filesize": 3398384, "mtime": "2013-11-13 03:38:56", "url": "/8024/1/thesis_Morton.pdf" } ], "eprint_id": 8024, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis_Morton.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/43857" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/43857" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/43857" } ] } } ], "eprint_status": "archive", "userid": 10092, "dir": "disk0/00/00/80/24", "datestamp": "2013-11-20 18:10:08", "lastmod": "2023-05-30 22:27:27", "status_changed": "2013-11-20 18:10:08", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "tim.morton@gmail.com", "id": "Morton-Timothy-Davies", "name": { "family": "Morton", "given": "Timothy Davies" }, "orcid": "0000-0002-8537-5711", "show_email": "YES" } ] }, "title": "Demographic Studies of Extrasolar Planets", "ispublished": "unpub", "full_text_status": "public", "keywords": "exoplanet, Kepler, statistics", "abstract": "Uncovering the demographics of extrasolar planets is crucial to understanding the processes of their formation and evolution. In this thesis, we present four studies that contribute to this end, three of which relate to NASA's Kepler mission, which has revolutionized the field of exoplanets in the last few years.
\r\n\r\nIn the pre-Kepler study, we investigate a sample of exoplanet spin-orbit measurements---measurements of the inclination of a planet's orbit relative to the spin axis of its host star---to determine whether a dominant planet migration channel can be identified, and at what confidence. Applying methods of Bayesian model comparison to distinguish between the predictions of several different migration models, we find that the data strongly favor a two-mode migration scenario combining planet-planet scattering and disk migration over a single-mode Kozai migration scenario. While we test only the predictions of particular Kozai and scattering migration models in this work, these methods may be used to test the predictions of any other spin-orbit misaligning mechanism.
\r\n\r\nWe then present two studies addressing astrophysical false positives in Kepler data. The Kepler mission has identified thousands of transiting planet candidates, and only relatively few have yet been dynamically confirmed as bona fide planets, with only a handful more even conceivably amenable to future dynamical confirmation. As a result, the ability to draw detailed conclusions about the diversity of exoplanet systems from Kepler detections relies critically on understanding the probability that any individual candidate might be a false positive. We show that a typical a priori false positive probability for a well-vetted Kepler candidate is only about 5-10%, enabling confidence in demographic studies that treat candidates as true planets. We also present a detailed procedure that can be used to securely and efficiently validate any individual transit candidate using detailed information of the signal's shape as well as follow-up observations, if available.
\r\n\r\nFinally, we calculate an empirical, non-parametric estimate of the shape of the radius distribution of small planets with periods less than 90 days orbiting cool (less than 4000K) dwarf stars in the Kepler catalog. This effort reveals several notable features of the distribution, in particular a maximum in the radius function around 1-1.25 Earth radii and a steep drop-off in the distribution larger than 2 Earth radii. Even more importantly, the methods presented in this work can be applied to a broader subsample of Kepler targets to understand how the radius function of planets changes across different types of host stars.
\r\n\r\n", "date": "2014", "date_type": "degree", "id_number": "CaltechTHESIS:11082013-132329970", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:11082013-132329970", "related_url": { "items": [ { "description": "Article adapted for ch.4", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/729/2/138" }, { "description": "Article adapted for ch.5", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/738/2/170" }, { "description": "Article adapted for ch.6", "type": "doi", "url": "http://dx.doi.org/10.1088/0004-637X/761/1/6" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Timothy Morton", "deposited_on": "2013-11-20 18:10:08", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jjohnson@cfa.harvard.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "jjohnson@cfa.harvard.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-10-30", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2014", "author_list": "Morton, Timothy Davies" }, { "id": "/id/eprint/8425", "eprint_id": 8425, "rev_number": 44, "documents": [ { "id": "/id/document/49314", "doc_id": 49314, "rev_number": 4, "files": [ { "id": "/id/file/142884", "fileid": 142884, "datasetid": "document", "objectid": 49314, "filename": "alex_lockwood_thesis_2014.pdf", "mime_type": "application/pdf", "hash": "d8969a593276c1315e240b8764753af7", "hash_type": "MD5", "filesize": 1899454, "mtime": "2014-05-29 22:53:27", "url": "/8425/1/alex_lockwood_thesis_2014.pdf" } ], "eprint_id": 8425, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "alex_lockwood_thesis_2014.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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"metadata_visibility": "show", "creators": { "items": [ { "email": "alexandra.lockwood@gmail.com", "id": "Lockwood-Alexandra-Charlotte", "name": { "family": "Lockwood", "given": "Alexandra Charlotte" }, "show_email": "NO" } ] }, "title": "Understanding Planet Formation through High Precision Photometry and Spectroscopy", "ispublished": "unpub", "full_text_status": "public", "keywords": "dwarf planets; near-IR spectroscopy; direct detection of exoplanets; protoplanetary disks", "abstract": "From studies of protoplanetary disks to extrasolar planets and planetary debris, we aim to understand the full evolution of a planetary system. Observational constraints from ground- and space-based instrumentation allows us to measure the properties of objects near and far and are central to developing this understanding. We present here three observational campaigns that, when combined with theoretical models, reveal characteristics of different stages and remnants of planet formation. The Kuiper Belt provides evidence of chemical and dynamical activity that reveals clues to its primordial environment and subsequent evolution. Large samples of this population can only be assembled at optical wavelengths, with thermal measurements at infrared and sub-mm wavelengths currently available for only the largest and closest bodies. We measure the size and shape of one particular object precisely here, in hopes of better understanding its unique dynamical history and layered composition.
\r\n\r\nMolecular organic chemistry is one of the most fundamental and widespread facets of the universe, and plays a key role in planet formation. A host of carbon-containing molecules vibrationally emit in the near-infrared when excited by warm gas, T~1000 K. The NIRSPEC instrument at the W.M. Keck Observatory is uniquely configured to study large ranges of this wavelength region at high spectral resolution. Using this facility we present studies of warm CO gas in protoplanetary disks, with a new code for precise excitation modeling. A parameterized suite of models demonstrates the abilities of the code and matches observational constraints such as line strength and shape. We use the models to probe various disk parameters as well, which are easily extensible to others with known disk emission spectra such as water, carbon dioxide, acetylene, and hydrogen cyanide.
\r\n\r\nLastly, the existence of molecules in extrasolar planets can also be studied with NIRSPEC and reveals a great deal about the evolution of the protoplanetary gas. The species we observe in protoplanetary disks are also often present in exoplanet atmospheres, and are abundant in Earth's atmosphere as well. Thus, a sophisticated telluric removal code is necessary to analyze these high dynamic range, high-resolution spectra. We present observations of a hot Jupiter, revealing water in its atmosphere and demonstrating a new technique for exoplanet mass determination and atmospheric characterization. We will also be applying this atmospheric removal code to the aforementioned disk observations, to improve our data analysis and probe less abundant species. Guiding models using observations is the only way to develop an accurate understanding of the timescales and processes involved. The futures of the modeling and of the observations are bright, and the end goal of realizing a unified model of planet formation will require both theory and data, from a diverse collection of sources.
", "date": "2014", "date_type": "degree", "id_number": "CaltechTHESIS:05292014-141324161", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05292014-141324161", "related_url": { "items": [ { "description": "Chapter 2 Published in Earth, Moon, and Planets Journal", "type": "ads", "url": "http://adsabs.harvard.edu/abs/2014EM%26P..111..127L" }, { "description": "Chapter 3 Published in the Astrophysical Journal Letters", "type": "ads", "url": "http://adsabs.harvard.edu/abs/2014ApJ...783L..29L" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Foundation Graduate Research Fellowship" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Withheld until 2 June 2015. Released 2015-10-07", "deposited_by": "Alexandra Lockwood", "deposited_on": "2014-05-30 21:36:19", "doi": "10.7907/7F1H-FG47", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "co-chair" }, { "email": "hknutson@caltech.edu", "id": "Knutson-H-A", "name": { "family": "Knutson", "given": "Heather A." }, "orcid": "0000-0002-5375-4725", "role": "co-chair" }, { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "member" }, { "email": "jjohnson@cfa.harvard.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-12-18", "gradofc_approval_date": "2014-05-30", "thesis_awards": "Graduate Dean's Award for Outstanding Community Service, 2014", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. 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ok jan 2014 Re CaltechTHESIS PhD thesis release request for Perez Munoz Laura Maria (2013).txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/128297", "doc_id": 128297, "rev_number": 1, "files": [ { "id": "/id/file/373733", "fileid": 373733, "datasetid": "document", "objectid": 128297, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "b2a6951859f9b3248358200c541e921a", "hash_type": "MD5", "filesize": 30538, "mtime": "2021-06-24 02:45:38", "url": "/7782/9/indexcodes.txt" } ], "eprint_id": 7782, "pos": 9, "placement": 9, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": 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These circumstellar disks provide large reservoirs of gas and dust that will eventually be transformed into planetary systems. Theory and observations suggest that the earliest stage toward planet formation in a protoplanetary disk is the growth of particles, from sub-micron-sized grains to centimeter- sized pebbles. Theory indicates that small interstellar grains are well coupled into the gas and are incorporated to the disk during the proto-stellar collapse. These dust particles settle toward the disk mid-plane and simultaneously grow through collisional coagulation in a very short timescale. Observationally, grain growth can be inferred by measuring the spectral energy distribution at long wavelengths, which traces the continuum dust emission spectrum and hence the dust opacity. Several observational studies have indicated that the dust component in protoplanetary disks has evolved as compared to interstellar medium dust particles, suggesting at least 4 orders of magnitude in particle- size growth. However, the limited angular resolution and poor sensitivity of previous observations has not allowed for further exploration of this astrophysical process.
\r\n\r\nAs part of my thesis, I embarked in an observational program to search for evidence of radial variations in the dust properties across a protoplanetary disk, which may be indicative of grain growth. By making use of high angular resolution observations obtained with CARMA, VLA, and SMA, I searched for radial variations in the dust opacity inside protoplanetary disks. These observations span more than an order of magnitude in wavelength (from sub-millimeter to centimeter wavelengths) and attain spatial resolutions down to 20 AU. I characterized the radial distribution of the circumstellar material and constrained radial variations of the dust opacity spectral index, which may originate from particle growth in these circumstellar disks. Furthermore, I compared these observational constraints with simple physical models of grain evolution that include collisional coagulation, fragmentation, and the interaction of these grains with the gaseous disk (the radial drift problem). For the parameters explored, these observational constraints are in agreement with a population of grains limited in size by radial drift. Finally, I also discuss future endeavors with forthcoming ALMA observations.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:05302013-223659579", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302013-223659579", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Laura Maria Perez Munoz", "deposited_on": "2014-01-29 21:57:44", "doi": "10.7907/1BJC-4G54", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "advisor" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "chair" }, { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "member" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "johnjohn@astro.caltech.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-10-29", "gradofc_approval_date": "2013-05-31", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2013", "author_list": "P\u00e9rez Mu\u00f1oz, Laura Mar\u00eda" }, { "id": "/id/eprint/7866", "eprint_id": 7866, "rev_number": 27, "documents": [ { "id": "/id/document/41303", "doc_id": 41303, "rev_number": 6, "files": [ { "id": "/id/file/124998", "fileid": 124998, "datasetid": "document", "objectid": 41303, "filename": "20130524_aikin_thesis.pdf", "mime_type": "application/pdf", "hash": "c9f07a40a47e5fe06a5be3c0718def39", "hash_type": "MD5", "filesize": 55446839, "mtime": "2013-06-07 18:47:00", "url": "/7866/1/20130524_aikin_thesis.pdf" } ], "eprint_id": 7866, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original", "language": "en", "security": "internal", "license": "other", "main": "20130524_aikin_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", 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"items": [ { "email": "raikin@gmail.com", "id": "Aikin-Randol-Wallace", "name": { "family": "Aikin", "given": "Randol Wallace" }, "show_email": "YES" } ] }, "title": "Testing Inflationary Cosmology with the BICEP1 and BICEP2 Experiments", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology, Polarization, CMB, Cosmic Microwave Background, Physics, Experiment", "abstract": "Recent observations of the temperature anisotropies of the cosmic microwave background (CMB) favor an inflationary paradigm in which the scale factor of the universe inflated by many orders of magnitude at some very early time. Such a scenario would produce the observed large-scale isotropy and homogeneity of the universe, as well as the scale-invariant perturbations responsible for the observed (10 parts per million) anisotropies in the CMB. An inflationary epoch is also theorized to produce a background of gravitational waves (or tensor perturbations), the effects of which can be observed in the polarization of the CMB. The E-mode (or parity even) polarization of the CMB, which is produced by scalar perturbations, has now been measured with high significance. Con- trastingly, today the B-mode (or parity odd) polarization, which is sourced by tensor perturbations, has yet to be observed. A detection of the B-mode polarization of the CMB would provide strong evidence for an inflationary epoch early in the universe\u2019s history.
\r\n\r\nIn this work, we explore experimental techniques and analysis methods used to probe the B- mode polarization of the CMB. These experimental techniques have been used to build the Bicep2 telescope, which was deployed to the South Pole in 2009. After three years of observations, Bicep2 has acquired one of the deepest observations of the degree-scale polarization of the CMB to date. Similarly, this work describes analysis methods developed for the Bicep1 three-year data analysis, which includes the full data set acquired by Bicep1. This analysis has produced the tightest constraint on the B-mode polarization of the CMB to date, corresponding to a tensor-to-scalar ratio estimate of r = 0.04\u00b10.32, or a Bayesian 95% credible interval of r < 0.70. These analysis methods, in addition to producing this new constraint, are directly applicable to future analyses of Bicep2 data. Taken together, the experimental techniques and analysis methods described herein promise to open a new observational window into the inflationary epoch and the initial conditions of our universe.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:06072013-113004037", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06072013-113004037", "referencetext": { "items": [ "Aikin, R. W., P. A. Ade, S. Benton, J. J. Bock, J. A. Bonetti, J. A. Brevik, C. D. Dowell, L. Duband, J. P. Filippini, S. R. Golwala, M. Halpern, V. V. Hristov, K. Irwin, J. P. Kaufman, B. G. Keating, J. M. Kovac, C. L. Kuo, A. E. Lange, C. B. Netterfield, H. T. Nguyen, R. W. Ogburn, IV, A. Orlando, C. Pryke, S. Richter, J. E. Ruhl, M. C. Runyan, C. Sheehy, S. A. Stokes, R. Sudiwala, G. P. Teply, J. E. Tolan, A. D. Turner, P. Wilson, and C. L. Wong (2010, July). Optical Performance of the BICEP2 Telescope at the South Pole. In Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Volume 7741 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, pp. 77410V.\r\nBarkats, D. et al. (2013). 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D. thesis, California Institute of Technology." ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Foundation", "grant_number": "ANT-0742818" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Randol Aikin", "deposited_on": "2013-11-04 20:28:33", "doi": "10.7907/z9vx0df2", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "chair" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "member" }, { "email": "bradf@caltech.edu", "id": "Filippone-B-W", "name": { "family": "Filippone", "given": "Bradley W." }, "orcid": "0000-0002-2618-2688", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-05-24", "gradofc_approval_date": "2013-06-07", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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17:36:38", "status_changed": "2013-05-28 20:48:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "gwenrudie@gmail.com", "id": "Rudie-Gwen-Charlena", "name": { "family": "Rudie", "given": "Gwen Charlena" }, "show_email": "NO" } ] }, "title": "The Intergalactic and Circumgalactic Medium Surrounding Star-Forming Galaxies at Redshifts 2Chapter 2 of this thesis focuses on HI surrounding high-z star-forming galaxies drawn from the Keck Baryonic Structure Survey (KBSS). The KBSS is a unique spectroscopic survey of the distant universe designed to explore the details of the connection between galaxies and intergalactic baryons within the same survey volumes. The KBSS combines high-quality background QSO spectroscopy with large densely-sampled galaxy redshift surveys to probe the CGM at scales of ∼50 kpc to a few Mpc. Based on these data, Chapter 2 presents the first quantitative measurements of the distribution, column density, kinematics, and absorber line widths of neutral hydrogen surrounding high-z star-forming galaxies.
\r\n \r\nChapter 3 focuses on the thermal properties of the diffuse IGM. This analysis relies on measurements of the ∼6000 absorber line widths to constrain the thermal and turbulent velocities of absorbing "clouds." \r\nA positive correlation between the column density of HI and the minimum line width is recovered and implies a temperature-density relation within the low-density IGM for which higher-density regions are hotter, as is predicted by simple theoretical arguments.
\r\n\r\nChapter 4 presents new measurements of the opacity of the IGM and CGM to hydrogen-ionizing photons. The chapter begins with a revised measurement of the HI column density distribution based on this new absorption line catalog that, due to the inclusion of high-order Lyman lines, provides the first statistically robust measurement of the frequency of absorbers with HI column densities 14 \u2272 log(NHI/cm-2) \u2272 17.2. Also presented are the first measurements of the column density distribution of HI within the CGM (50 <d < 300 pkpc) of high-z galaxies. These distributions are used to calculate the total opacity of the IGM and IGM+CGM and to revise previous measurements of the mean free path of hydrogen-ionizing photons within the IGM. This chapter also considers the effect of the surrounding CGM on the transmission of ionizing photons out of the sites of active star-formation and into the IGM.
\r\n\r\nThis thesis concludes with a brief discussion of work in progress focused on understanding the distribution of metals within the CGM of KBSS galaxies. Appendix B discusses my contributions to the MOSFIRE instrumentation project.
\r\n\r\n", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:05202013-155707736", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05202013-155707736", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Mixed access. Full thesis withheld until 1 Oct 2016. Released 11/10/2016.", "deposited_by": "Gwen Rudie", "deposited_on": "2013-05-28 20:48:37", "doi": "10.7907/Z9PZ56T6", "alt_title": { "items": [ "The Intergalactic and Circumgalactic Medium Surrounding Star-Forming Galaxies at Redshifts 2 < z < 3" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "member" }, { "email": "jak@obs.carnegiescience.edu", "id": "Kollmeier-J-A", "name": { "family": "Kollmeier", "given": "Juna A." }, "orcid": "0000-0001-9852-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-05-17", "gradofc_approval_date": "2013-05-28", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2013", "author_list": "Rudie, Gwen Charlena" }, { "id": "/id/eprint/7713", "eprint_id": 7713, "rev_number": 33, "documents": [ { "id": "/id/document/38382", "doc_id": 38382, "rev_number": 2, "files": [ { "id": "/id/file/118887", "fileid": 118887, "datasetid": "document", "objectid": 38382, "filename": "AZimmermanThesis.pdf", "mime_type": "application/pdf", "hash": "c71a1ee1d5a42440d5070d9fe025e4cb", "hash_type": "MD5", "filesize": 34783402, "mtime": "2013-05-15 18:46:12", "url": "/7713/1/AZimmermanThesis.pdf" } ], "eprint_id": 7713, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "AZimmermanThesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"archival" }, { "id": "/id/document/128210", "doc_id": 128210, "rev_number": 1, "files": [ { "id": "/id/file/373646", "fileid": 373646, "datasetid": "document", "objectid": 128210, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "432450227936b4b60896d96d7d5a0d20", "hash_type": "MD5", "filesize": 43246, "mtime": "2021-06-24 02:39:25", "url": "/7713/8/indexcodes.txt" } ], "eprint_id": 7713, "pos": 8, "placement": 8, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/38382" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/38382" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/38382" } ] } } ], "eprint_status": "archive", "userid": 9871, "dir": "disk0/00/00/77/13", "datestamp": "2013-05-17 22:55:16", "lastmod": "2020-03-04 22:06:42", "status_changed": "2013-05-17 22:55:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "aaronbzimmerman@gmail.com", "id": "Zimmerman-Aaron-Benjamin", "name": { "family": "Zimmerman", "given": "Aaron Benjamin" }, "show_email": "YES" } ] }, "title": "Topics in Black Hole Perturbation Theory and the Visualization of Curved Spacetime", "ispublished": "unpub", "full_text_status": "public", "keywords": "General Relativity, Black Holes, Black Hole Perturbations, Numerical Relativity, Tensor Visualization", "abstract": "This thesis presents recent research into analytic topics in the classical theory of General Relativity. It is a thesis in two parts. The first part features investigations into the spectrum of perturbed, rotating black holes. These include the study of near horizon perturbations, leading to a new generic frequency mode for black hole ringdown; an treatment of high frequency waves using WKB methods for Kerr black holes; and the discovery of a bifurcation of the quasinormal mode spectrum of rapidly rotating black holes. These results represent new discoveries in the field of black hole perturbation theory, and rely on additional approximations to the linearized field equations around the background black hole. The second part of this thesis presents a recently developed method for the visualization of curved spacetimes, using field lines called the tendex and vortex lines of the spacetime. The works presented here both introduce these visualization techniques, and explore them in simple situations. These include the visualization of asymptotic gravitational radiation; weak gravity situations with and without radiation; stationary black hole spacetimes; and some preliminary study into numerically simulated black hole mergers. The second part of thesis culminates in the investigation of perturbed black holes using these field line methods, which have uncovered new insights into the dynamics of curved spacetime around black holes.", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:05152013-113945625", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05152013-113945625", "related_url": { "items": [ { "type": "doi", "url": "http://dx..doi.org/10.1103/PhysRevD.84.084012" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.86.104006" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.87.041502" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevLett.106.151101" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.84.044037" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.84.124014" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.86.084049" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.86.104028" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Aaron Zimmerman", "deposited_on": "2013-05-17 22:55:16", "doi": "10.7907/8809-P894", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "chair" }, { "email": "rana@ligo.caltech.edu", "id": "Adhikari-R", "name": { "family": "Adhikari", "given": "Rana" }, "role": "member" }, { "email": "seancarroll@gmail.com", "id": "Carroll-S-M", "name": { "family": "Carroll", "given": "Sean M." }, "role": "member" }, { "email": "cott@tapir.caltech.edu", "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-05-07", "gradofc_approval_date": "2013-05-17", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2013", "author_list": "Zimmerman, Aaron Benjamin" }, { "id": "/id/eprint/7629", "eprint_id": 7629, "rev_number": 23, "documents": [ { "id": "/id/document/37323", "doc_id": 37323, "rev_number": 4, "files": [ { "id": "/id/file/116487", "fileid": 116487, "datasetid": "document", "objectid": 37323, "filename": "matt_thesis.pdf", "mime_type": "application/pdf", "hash": "823e8f52232df446048339e4dc7c91e8", "hash_type": "MD5", "filesize": 3705189, "mtime": "2013-04-24 01:41:09", "url": "/7629/1/matt_thesis.pdf" } ], "eprint_id": 7629, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "matt_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/37323" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/37323" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/37323" } ] } } ], "eprint_status": "archive", "userid": 9830, "dir": "disk0/00/00/76/29", "datestamp": "2013-05-13 18:29:36", "lastmod": "2023-11-08 00:16:42", "status_changed": "2013-05-13 18:29:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mjkelley3@gmail.com", "id": "Kelley-Matthew-James", "name": { "family": "Kelley", "given": "Matthew James" }, "show_email": "YES" } ] }, "title": "Terahertz Time Domain Spectroscopy of Amino Acids and Sugars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Terahertz ; THz ; Far-Infrared ; GABA ; Amino Acid ; Sugar", "abstract": "A time-domain spectrometer for use in the terahertz (THz) spectral range was designed and constructed. Due to there being few existing methods of generating and detecting THz radiation, the spectrometer is expected to have vast applications to solid, liquid, and gas phase samples. In particular, knowledge of complex organic chemistry and chemical abundances in the interstellar medium (ISM) can be obtained when compared to astronomical data. The THz spectral region is of particular interest due to reduced line density when compared to the millimeter wave spectrum, the existence of high resolution observatories, and potentially strong transitions resulting from the lowest-lying vibrational modes of large molecules.
\r\n\r\nThe heart of the THz time-domain spectrometer (THz-TDS) is the ultrafast laser. Due to the femtosecond duration of ultrafast laser pulses and an energy-time uncertainty relationship, the pulses typically have a several-THz bandwidth. By various means of optical rectification, the optical pulse carrier envelope shape, i.e. intensity-time profile, can be transferred to the phase of the resulting THz pulse. As a consequence, optical pump-THz probe spectroscopy\r\nis readily achieved, as was demonstrated in studies of dye-sensitized TiO2, as discussed in chapter 4. Detection of the terahertz radiation is commonly based on electro-optic sampling and provides full phase information. This allows for accurate determination of both the real and imaginary index of refraction, the so-called optical constants, without additional analysis. A suite of amino acids and sugars, all of which have been found in meteorites, were studied in crystalline form embedded in a polyethylene matrix. As the temperature was varied between 10 and 310 K, various strong vibrational modes were found to shift in spectral intensity and frequency. Such modes can be attributed to intramolecular, intermolecular, or phonon modes, or to some combination of the three.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:04232013-183107863", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04232013-183107863", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Matthew Kelley", "deposited_on": "2013-05-13 18:29:36", "doi": "10.7907/FQ9S-JF63", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "hbgray@caltech.edu", "id": "Gray-H-B", "name": { "family": "Gray", "given": "Harry B." }, "orcid": "0000-0002-7937-7876", "role": "chair" }, { "email": "mo@caltech.edu", "id": "Okumura-M", "name": { "family": "Okumura", "given": "Mitchio" }, "orcid": "0000-0001-6874-1137", "role": "member" }, { "email": "tfm@caltech.edu", "id": "Miller-T-F", "name": { "family": "Miller", "given": "Thomas F." }, "orcid": "0000-0002-1882-5380", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-03-18", "gradofc_approval_date": "2013-05-10", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/35686" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/35686" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/35686" } ] } } ], "eprint_status": "archive", "userid": 9775, "dir": "disk0/00/00/75/00", "datestamp": "2013-04-09 23:21:09", "lastmod": "2021-10-26 17:33:57", "status_changed": "2013-04-09 23:21:09", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "newman.db@gmail.com", "id": "Newman-Andrew-Burch", "name": { "family": "Newman", "given": "Andrew Burch" }, "show_email": "YES" } ] }, "title": "Dark Matter and the Assembly History of Massive Galaxies and Clusters", "ispublished": "unpub", "full_text_status": "public", "keywords": "dark matter; galaxy clusters; gravitational lensing; stellar dynamics; galaxy structure and evolution; elliptical galaxies", "abstract": "In Part I of this thesis we study the distribution of dark matter and baryons in a sample of seven massive, relaxed galaxy clusters by combining multiple observational tools. Our aim is to make comprehensive mass profile measurements and compare these to the form of the universal density profile derived in numerical cold dark matter (CDM) simulations. By joining weak and strong gravitational lensing observations with resolved stellar kinematic data within the central brightest cluster galaxy (BCG), we constrain the density profile over the wide dynamic range of 3-3000 kpc in radius for the first time. We first compare lensing- and X-ray-derived mass measures to constrain the line-of-sight geometry of the clusters in our sample. We then show that the logarithmic slope of the total density profile - comprising both stars and dark matter - agrees closely with numerical simulations containing only dark matter down to radii of \u22437 kpc, despite the significant contribution of stellar material on such small scales. Our unique stellar kinematic data allow us to constrain two-component models of the stellar and dark matter distributions in the cluster cores. We find a mean logarithmic slope for the dark matter density of <\u03b2> = 0.50 ± 0.10 (random)+0.14-0.13 (systematic) at small radii, where \u03c1DM ∝ r-\u03b2. This is significantly shallower than a canonical CDM cusp having \u03b2 = 1. Alternatively, a cored dark matter profile with <log rcore / kpc> = 1.14 ± 0.13 (random)+0.14-0.22 (systematic) provides an equally good description. The mean mass-to-light ratio of the stars in the BCGs, derived from lensing and dynamics, is found to be consistent with estimates from stellar population synthesis modeling provided that a Salpeter initial mass function (IMF), or one with a similarly high mass-to-light ratio, is adopted. We find some evidence for a correlation between the inner dark matter profile and the size or luminosity of the BCG, which suggests a connection between the inner dark matter distribution and the assembly history of stars in the central galaxy. We discuss physical processes that might account for the small-scale dark matter distribution that we observe.
\r\n\r\nIn Part II we turn to the assembly of stars in massive, quiescent galaxies. Many observations now indicate that the extended stellar envelopes seen in these systems today have grown over the last 11 Gyr. We present a two-pronged program aimed at understanding the remarkable growth observed in the size of their stellar distributions over this interval. First, we conducted deep spectroscopic observations of a sample of 17 spheroidal galaxies at z = 1.05-1.60 to derive their internal velocity dispersions from stellar absorption lines. These dynamical data provide a robust verification of their compactness and masses, which were previously inferred photometrically. Second, in order to investigate the likely role of galaxy mergers in contributing to the observed size growth, we searched for satellites around a sample of massive, quiescent galaxies at z = 0.4-2. Using HST/WFC3 imaging from the CANDELS survey, we are able to probe faint companions with stellar masses down to 10% of that of the host galaxy. By coupling measurements of the number and stellar mass content of such companions with results from published merger simulations, we estimate the rate of size growth attributable to major and minor galaxy mergers. We compare this to the rate of size growth measured in the same large, homogeneous sample of quiescent galaxies, based on deep, high-resolution imaging in the rest-frame optical. We find that observed impending mergers might account for the size growth seen at z \u2272 1, provided that a relatively short merger timescale is valid. At progressively higher redshifts, however, the estimated merger rate is outstripped by the rate of size growth. Either the merger physics is not currently well understood, or additional processes must contribute significantly to early size growth of quiescent galaxies.
\r\n\r\nIn the final chapter we summarize our results and describe future prospects for elucidating the small-scale distribution of dark matter at intermediate mass scales, as well as the physical drivers of early spheroid evolution.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:03062013-151111064", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03062013-151111064", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Andrew Newman", "deposited_on": "2013-04-09 23:21:09", "doi": "10.7907/BNC2-1X24", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "chair" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "johnjohn@astro.caltech.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" }, { "email": "abenson@obs.carnegiescience.edu", "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew J." }, "orcid": "0000-0001-5501-6008", "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-02-04", "gradofc_approval_date": "2013-04-08", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"uri": "/id/document/41316" } ] } } ], "eprint_status": "archive", "userid": 9863, "dir": "disk0/00/00/78/57", "datestamp": "2013-06-07 23:41:07", "lastmod": "2021-11-05 22:48:50", "status_changed": "2013-06-07 23:41:07", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "david@dlevitan.com", "id": "Levitan-David-Benjamin", "name": { "family": "Levitan", "given": "David Benjamin" }, "show_email": "YES" } ] }, "title": "Finding Needles in the Haystack: A Search for AM CVn Systems Using the Palomar Transient Factory", "ispublished": "unpub", "full_text_status": "public", "keywords": "AM CVn Systems;Cataclysmic Variables;Synoptic Surveys;White Dwarfs;Population Study;Spectroscopy;Optical;Astronomy;Palomar;Keck;Ultra-Compact Binaries;Photometry;Semi-Detached System;Dwarf Novae", "note": "Title in 2013 Commencement program varies: Finding Needles in the Haystack: A Search for AM CVn Systems with the Palomar Transient Factory", "abstract": "The AM CVn systems are a rare class of ultra-compact astrophysical binaries. With orbital periods of under an hour and as short as five minutes, they are among the closest known binary star systems and their evolution has direct relevance to the type Ia supernova rate and the white dwarf binary population. However, their faint and rare nature has made population studies of these systems difficult and several studies have found conflicting results.
\r\n\r\nI undertook a survey for AM CVn systems using the Palomar Transient Factory (PTF) astrophysical synoptic survey by exploiting the \"outbursts\" these systems undergo. Such events result in an increase in luminosity by a factor of up to two-hundred and are detectable in time-domain photometric data of AM CVn systems. My search resulted in the discovery of eight new systems, over 20% of the current known population. More importantly, this search was done in a systematic fashion, which allows for a population study properly accounting for biases.
\r\n\r\nApart from the discovery of new systems, I used the time-domain data from the PTF and other synoptic surveys to better understand the long-term behavior of these systems. This analysis of the photometric behavior of the majority of known AM CVn systems has shown changes in their behavior at longer time scales than have previously been observed. This has allowed me to find relationships between the outburst properties of an individual system and its orbital period.
\r\n\r\nEven more importantly, the systematically selected sample together with these properties have allowed me to conduct a population study of the AM CVn systems. I have shown that the latest published estimates of the AM CVn system population, a factor of fifty below theoretical estimates, are consistent with the sample of systems presented here. This is particularly noteworthy since my population study is most sensitive to a different orbital period regime than earlier surveys. This confirmation of the population density will allow the AM CVn systems population to be used in the study of other areas of astrophysics.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:06062013-224902992", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06062013-224902992", "projects": { "items": [ "Palomar Transient Factory (PTF)" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "David Levitan", "deposited_on": "2013-06-07 23:41:07", "doi": "10.7907/MJJ0-7A67", "alt_title": { "items": [ "Finding Needles in the Haystack: A Search for AM CVn Systems with the Palomar Transient Factory" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "prince@srl.caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "prince@srl.caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-05-28", "gradofc_approval_date": "2013-06-07", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"status_changed": "2014-10-01 17:46:19", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "czakon@gmail.com", "id": "Czakon-Nicole-Gisela", "name": { "family": "Czakon", "given": "Nicole Gisela" }, "show_email": "NO" } ] }, "title": "Sunyaev-Zel\u2019dovich Observations Using Large-Format Millimeter Arrays", "ispublished": "unpub", "full_text_status": "public", "keywords": "Galaxy Clusters ; Large-Scale Structure Formation ; Bolocam ; Chandra ; Sunyaev-Zel'dovich Effect", "abstract": "Galaxy clusters are the largest gravitationally bound objects in the observable universe, and they are formed from the largest perturbations of the primordial matter power spectrum. During initial cluster collapse, matter is accelerated to supersonic velocities, and the baryonic component is heated as it passes through accretion shocks. This process stabilizes when the pressure of the bound matter prevents further gravitational collapse. Galaxy clusters are useful cosmological probes, because their formation progressively freezes out at the epoch when dark energy begins to dominate the expansion and energy density of the universe. A diverse set of observables, from radio through X-ray wavelengths, are sourced from galaxy clusters, and this is useful for self-calibration. The distributions of these observables trace a cluster's dark matter halo, which represents more than 80% of the cluster's gravitational potential. One such observable is the Sunyaev-Zel'dovich effect (SZE), which results when the ionized intercluster medium blueshifts the cosmic microwave background via Compton scattering. Great technical advances in the last several decades have made regular observation of the SZE possible. Resolved SZE science, such as is explored in this analysis, has benefitted from the construction of large-format camera arrays consisting of highly sensitive millimeter-wave detectors, such as Bolocam. Bolocam is a submillimeter camera, sensitive to 140 GHz and 268 GHz radiation, located at one of the best observing sites in the world: the Caltech Submillimeter Observatory on Mauna Kea in Hawaii. Bolocam fielded 144 of the original spider web NTD bolometers used in an entire generation of ground-based, balloon-borne, and satellite-borne millimeter wave instrumention. Over approximately six years, our group at Caltech has developed a mature galaxy cluster observational program with Bolocam. This thesis describes the construction of the instrument's full cluster catalog: BOXSZ. Using this catalog, I have scaled the Bolocam SZE measurements with X-ray mass approximations in an effort to characterize the SZE signal as a viable mass probe for cosmology. This work has confirmed the SZE to be a low-scatter tracer of cluster mass. The analysis has also revealed how sensitive the SZE-mass scaling is to small biases in the adopted mass approximation. Future Bolocam analysis efforts are set on resolving these discrepancies by approximating cluster mass jointly with different observational probes.", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:06052013-104216835", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06052013-104216835", "referencetext": { "items": [ "[1] Abell, G. O. 1958, Astrophys. J. Suppl., 3, 211\r\n[2] Abell, G. O., Corwin, Jr., H. G., & Olowin, R. P. 1989, Astrophys. J. Suppl., 70, 1\r\n[3] Ackermann, M., Ajello, M., Allafort, A., et al. 2013, Science, 339, 807\r\n[4] Ahmed, Z., Akerib, D. 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S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-05-17", "gradofc_approval_date": "2013-06-06", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2013", "author_list": "Czakon, Nicole Gisela" }, { "id": "/id/eprint/7185", "eprint_id": 7185, "rev_number": 36, "documents": [ { "id": "/id/document/15197", "doc_id": 15197, "rev_number": 5, "files": [ { "id": "/id/file/99245", "fileid": 99245, "datasetid": "document", "objectid": 15197, "filename": "WeggChristopherThesis.pdf", "mime_type": "application/pdf", "filesize": 13120181, "mtime": "2012-12-26 04:44:50", "url": "/7185/1/WeggChristopherThesis.pdf" } ], "eprint_id": 7185, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "WeggChristopherThesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28156" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28156" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28156" } ] } }, { "id": "/id/document/28156", "doc_id": 28156, "rev_number": 2, "files": [ { "id": "/id/file/99243", "fileid": 99243, "datasetid": "document", "objectid": 28156, "filename": "preview.png", "mime_type": "image/png", "hash": "bbde542f6b5fa6d7560658397e7c88a1", "hash_type": "MD5", "filesize": 35449, "mtime": "2012-12-26 04:44:50", "url": "/7185/2/preview.png" } ], "eprint_id": 7185, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15197" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/15197" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15197" } ] } }, { "id": "/id/document/127634", "doc_id": 127634, "rev_number": 1, "files": [ { "id": "/id/file/373070", "fileid": 373070, "datasetid": "document", "objectid": 127634, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "58ba3ce6f7a827c7c0ed912f0a55217e", "hash_type": "MD5", "filesize": 32341, "mtime": "2021-06-24 01:55:42", "url": "/7185/3/indexcodes.txt" } ], "eprint_id": 7185, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15197" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15197" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15197" } ] } } ], "eprint_status": "archive", "userid": 7608, "dir": "disk0/00/00/71/85", "datestamp": "2012-08-22 21:57:11", "lastmod": "2021-10-26 17:37:50", "status_changed": "2012-08-22 21:57:11", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "chriswegg@gmail.com", "id": "Wegg-Christopher", "name": { "family": "Wegg", "given": "Christopher" }, "show_email": "NO" } ] }, "title": "The Dynamics of White Dwarfs, Black Holes and Stellar Cusps", "ispublished": "unpub", "full_text_status": "public", "keywords": "Black Holes; White Dwarfs; Supermassive Black Holes; Kinematics; Galactic Dynamics; Extreme Mass-Ratio Inspirals;Supermassive Black Hole Binaries; Ultracool White Dwarfs; Singular Isothermal Sphere; Fokker-Planck; Tidal Disruptions; Pseudo-Newtonian Potential ", "abstract": "This thesis contains topics related mostly to the dynamics of white dwarfs (chapter 2), the dynamics of stars around binary super massive black holes (chapters 4, 5 and 6) and dynamics in the singular isothermal sphere (chapter 7).
\r\n\r\nIn chapter 2 the kinematics of young (< 3x108yr) galactic white dwarfs are investigated. A relationship between the mass and kinematics of white dwarfs is demonstrated, whereby high- mass white dwarfs have low velocity dispersion. This is the result of less scattering during the shorter lifetime of their more massive precursors. The kinematics of the highest-mass white dwarfs (> 0.95 Msun) are also investigated, and it is shown that they are consistent with the majority being formed via single-star evolution from massive progenitor stars.
\r\n\r\nIn chapter 3 it is shown that the coolest, oldest white dwarfs can be identified photometrically from their unique colors, and five new ultracool white dwarfs are spectroscopically confirmed.
\r\n\r\nIn chapter 4 it is shown that close binary supermassive black holes (SMBHs) should produce a burst of tidal disruptions of up to 0.1 yr\u22121 as they form. The quiescent rate is ~10\u22125 yr\u22121 per galaxy, and it is therefore shown that binary SMBHs can potentially be identified via multiple tidal disruptions from the same system.\r\n
\r\n\r\nIn chapter 5 we perform more extensive simulations of the dynamics of stars around binary SMBHs to better quantify and understand the stellar dynamics. By incorporating general relativistic corrections, we also investigate the processes undergone by compact remnants orbiting the binary SMBHs, analyzing both objects that plunge directly into the SMBHs, and those that undergo extreme mass ratio inspirals (EMRIs). The potential used to mimic general relativistic precession in these simulations is novel, and more accurate for the type of nearly parabolic orbits considered in this work: It is described in chapter 6.\r\n
\r\n\r\nIn chapter 7 an analytic solution to the manner in which stars diffuse in the background of a singular isothermal sphere is developed. It is shown a self-similar solution should exist, and this solution is found.\r\n
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:08152012-212758368", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08152012-212758368", "related_url": { "items": [ { "type": "arxiv", "url": "http://arxiv.org/abs/1206.1056" }, { "type": "pub", "url": "http://dx.doi.org/10.1088/2041-8205/738/1/L8" }, { "type": "pub", "url": "http://iopscience.iop.org/2041-8205/738/1/L8" }, { "type": "arxiv", "url": "http://arxiv.org/abs/1011.5874" }, { "type": "pub", "url": "http://dx.doi.org/10.1088/0004-637X/749/2/183" }, { "type": "pub", "url": "http://iopscience.iop.org/0004-637X/749/2/183/" }, { "type": "arxiv", "url": "http://arxiv.org/abs/1202.5336" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "George Porter", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Christopher Wegg", "deposited_on": "2012-08-22 21:57:11", "doi": "10.7907/YCAT-ES15", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "chair" }, { "email": "abenson@obs.carnegiescience.edu", "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew J." }, "orcid": "0000-0001-5501-6008", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-07-19", "gradofc_approval_date": "2012-08-21", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2013", "author_list": "Wegg, Christopher" }, { "id": "/id/eprint/7178", "eprint_id": 7178, "rev_number": 38, "documents": [ { "id": "/id/document/15171", "doc_id": 15171, "rev_number": 4, "files": [ { "id": "/id/file/99029", "fileid": 99029, "datasetid": "document", "objectid": 15171, "filename": "Thesis_TingHong_2013.pdf", "mime_type": "application/pdf", "filesize": 5591955, "mtime": "2012-12-26 04:44:41", "url": "/7178/3/Thesis_TingHong_2013.pdf" } ], "eprint_id": 7178, "pos": 3, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Thesis_TingHong_2013.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28142" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28142" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28142" } ] } }, { "id": "/id/document/28142", "doc_id": 28142, "rev_number": 2, "files": [ { "id": "/id/file/99027", "fileid": 99027, "datasetid": "document", "objectid": 28142, "filename": "preview.png", "mime_type": "image/png", "hash": "9f2daaa927181f895cd04ab1021b4696", "hash_type": "MD5", "filesize": 39172, "mtime": "2012-12-26 04:44:40", "url": "/7178/4/preview.png" } ], "eprint_id": 7178, "pos": 4, "placement": 4, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15171" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/15171" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15171" } ] } }, { "id": "/id/document/127620", "doc_id": 127620, "rev_number": 1, "files": [ { "id": "/id/file/373056", "fileid": 373056, "datasetid": "document", "objectid": 127620, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "1f6326228d027689a7542e85b7af43fb", "hash_type": "MD5", "filesize": 26107, "mtime": "2021-06-24 01:55:08", "url": "/7178/5/indexcodes.txt" } ], "eprint_id": 7178, "pos": 5, "placement": 5, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15171" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15171" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15171" } ] } } ], "eprint_status": "archive", "userid": 6977, "dir": "disk0/00/00/71/78", "datestamp": "2012-08-30 18:31:18", "lastmod": "2020-03-04 22:06:42", "status_changed": "2012-08-30 18:31:18", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "hongting823@gmail.com", "id": "Hong-Ting", "name": { "family": "Hong", "given": "Ting" }, "show_email": "NO" } ] }, "title": "Brownian Thermal Noise in Interferometric Gravitational Wave Detectors and Single Photon Optomechanics", "ispublished": "unpub", "full_text_status": "public", "keywords": "Brownian thermal noise, LIGO, optomechnanics, single photon", "abstract": "The Laser Interferometric Gravitational-Wave Observatory (LIGO) is designed to detect the Gravitational Waves (GW) predicted by Albert Einstein\u2019s general theory of relativity. The advanced LIGO project is ongoing an upgrade to increase the detection sensitivity by more than a factor of 10, which will make the events detection a routine occurrence. In addition to using higher power lasers, heavier test mass, and better isolation systems, several new designs and techniques are proposed in the long-term upgrade, such as modifying the optics configuration to reduce the quantum noise, active noise cancellation of the Newtonian noise, optimizing the coating structure, and employing non-Guassian laser beams etc.
\r\n\r\nIn the first part of my thesis (Chapters 2 and 3), I apply statistical mechanics and elastostatics to the LIGO coated mirrors, and study the thermal fluctuations that dominate advanced LIGO\u2019s most sensitive frequency band from 40 Hz to 200 Hz.
\r\n\r\nIn particular, in Chapter 2, I study the so-called coating Brownian noise, fluctuations of mirrors coated with multiple layers of dielectrics due to internal friction. Assuming coating materials to be isotropic and homogeneous, I calculate the cross spectra of Brownian fluctuations in the bulk and shear strains of the coating layers, as well as fluctuations in the height of the coating-substrate interface. The additional phase shifting and back-scattering caused by photo elastic effects are also considered for the first time.
\r\n\r\nIn Chapter 3, I study whether it is realistic to adopt higher-order Laguerre-Gauss modes in LIGO, in order to mitigate the effect of mirror thermal noise. We investigate the effect on the detector\u2019s contrast defect caused by the mode degeneracy. With both analytical calculation and numerical simulation, we show that with this approach, the detector\u2019s susceptibility to mirror figure errors is reduced greatly compared to using the nondegenerate modes, therefore making it unacceptable for LIGO requirements.
\r\n\r\nFor the future GW detectors, with much lower noises and higher sensitivity, this might be used to investigate the quantum behaviors of macroscopic mechanical objects. In recent years the linear optomechanical systems with cavity modes coupling to a mechanical oscillator have been studied extensively. In the second part of my thesis (Chapter 4), I study the interaction between a single photon and a high-finesse cavity with a movable mirror, in the so-called strong coupling regime, where the recoil of the photon can cause significant change in the momentum of the mirror. The results are applied to analyze the case with a Fabry-Perot cavity. We also present that with engineering the photon wave function, it is possible to prepare the oscillator into an arbitrary quantum state.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:07182012-212554378", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:07182012-212554378", "related_url": { "items": [ { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.84.102001" }, { "type": "arxiv", "url": "http://arxiv.org/abs/1110.3348" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0555406" }, { "agency": "NSF", "grant_number": "PHY-1068881" }, { "agency": "CAREER", "grant_number": "PHY-0956189" }, { "agency": "David and Barbara Groce Startup Fund" } ] }, "collection": "CaltechTHESIS", "reviewer": "George Porter", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Ting Hong", "deposited_on": "2012-08-30 18:31:18", "doi": "10.7907/B83T-7730", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "chair" }, { "email": "rana@caltech.edu", "id": "Adhikari-R", "name": { "family": "Adhikari", "given": "Rana" }, "role": "member" }, { "email": "schwab@caltech.edu", "id": "Schwab-K-C", "name": { "family": "Schwab", "given": "Keith C." }, "role": "member" }, { "email": "jrgreer@caltech.edu", "id": "Greer-J-R", "name": { "family": "Greer", "given": "Julia R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-07-16", "gradofc_approval_date": "2012-08-24", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"disk0/00/00/78/24", "datestamp": "2013-06-06 22:02:47", "lastmod": "2021-10-26 17:29:20", "status_changed": "2013-06-06 22:02:47", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "vera.gluscevic@gmail.com", "id": "Glu\u0161\u010devi\u0107-Vera", "name": { "family": "Glu\u0161\u010devi\u0107", "given": "Vera" }, "show_email": "YES" } ] }, "title": "CMB as a Probe of New Physics and Old Times", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology, cosmic microwave background, dark energy, quintessence, cosmic reionization", "abstract": "Cosmic birefringence (CB)---a rotation of photon-polarization plane in vacuum---is a generic signature of new scalar fields that could provide dark energy. Previously, WMAP observations excluded a uniform CB-rotation angle larger than a degree.
\r\n\r\nIn this thesis, we develop a minimum-variance--estimator formalism for reconstructing direction-dependent rotation from full-sky CMB maps, and forecast more than an order-of-magnitude improvement in sensitivity with incoming Planck data and future satellite missions. Next, we perform the first analysis of WMAP-7 data to look for rotation-angle anisotropies and report null detection of the rotation-angle power-spectrum multipoles below L=512, constraining quadrupole amplitude of a scale-invariant power to less than one degree. We further explore the use of a cross-correlation between CMB temperature and the rotation for detecting the CB signal, for different quintessence models. We find that it may improve sensitivity in case of marginal detection, and provide an empirical handle for distinguishing details of new physics indicated by CB.
\r\n\r\nWe then consider other parity-violating physics beyond standard models---in particular, a chiral inflationary-gravitational-wave background. We show that WMAP has no constraining power, while a cosmic-variance--limited experiment would be capable of detecting only a large parity violation. In case of a strong detection of EB/TB correlations, CB can be readily distinguished from chiral gravity waves.
\r\n\r\nWe next adopt our CB analysis to investigate patchy screening of the CMB, driven by inhomogeneities during the Epoch of Reionization (EoR). We constrain a toy model of reionization with WMAP-7 data, and show that data from Planck should start approaching interesting portions of the EoR parameter space and can be used to exclude reionization tomographies with large ionized bubbles.
\r\n\r\nIn light of the upcoming data from low-frequency radio observations of the redshifted 21-cm line from the EoR, we examine probability-distribution functions (PDFs) and difference PDFs of the simulated 21-cm brightness temperature, and discuss the information that can be recovered using these statistics. We find that PDFs are insensitive to details of small-scale physics, but highly sensitive to the properties of the ionizing sources and the size of ionized bubbles.
\r\n\r\nFinally, we discuss prospects for related future investigations.
\r\n\r\n", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:06032013-130145873", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06032013-130145873", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Vera Gluscevic", "deposited_on": "2013-06-06 22:02:47", "doi": "10.7907/VZ0P-XD08", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kamion@pha.jhu.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "chair" }, { "email": "johnjohn@astro.caltech.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" }, { "email": "seancarroll@gmail.com", "id": "Carroll-S-M", "name": { "family": "Carroll", "given": "Sean M." }, "orcid": "0000-0002-4226-5758", "role": "member" }, { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "member" }, { "email": "kamion@pha.jhu.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-02-28", "gradofc_approval_date": "2013-06-04", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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They are powerful, variable emitters from radio to gamma-ray wavelengths. Although the general picture of synchrotron emission at low energies and inverse Compton at high energies is well established, important aspects of blazars are not well understood. In particular, the location of the gamma-ray emission region is not clearly established, with some theories favoring a location close to the central engine, while others place it at parsec scales in the radio jet.
\r\n\r\nWe developed a program to locate the gamma-ray emission site in blazars, through the study of correlated variations between their gamma-ray and radio-wave emission. Correlated variations are expected when there is a relation between emission processes at both bands, while delays tell us about the relative location of their energy generation zones. Monitoring at 15 GHz using the Owens Valley Radio Observatory 40 meter telescope started in mid-2007. The program monitors 1593 blazars twice per week, including all blazars detected by the Fermi Gamma-ray Space Telescope (Fermi) north of -20 degrees declination. This program complements the continuous monitoring of gamma-rays by Fermi.
\r\n\r\nThree year long gamma-ray light curves for bright Fermi blazars are cross-correlated with four years of radio monitoring. The significance of cross-correlation peaks is investigated using simulations that account for the uneven sampling and noise properties of the light curves, which are modeled as red-noise processes with a simple power-law power spectral density. We found that out of 86 sources with high quality data, only three show significant correlations (AO 0235+164, B2 2308+34 and PKS 1502+106). Additionally, we find a significant correlation for Mrk 421 when including the strong gamma-ray/radio flare of late 2012. In all four cases radio variations lag gamma-ray variations, suggesting that the gamma-ray emission originates upstream of the radio emission. For PKS 1502+106 we locate the gamma-ray emission site parsecs away from the central engine, thus disfavoring the model of Blandford and Levinson (1995), while other cases are inconclusive. These findings show that continuous monitoring over long time periods is required to understand the cross-correlation between gamma-ray and radio-wave variability in most blazars.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:05302013-225100503", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302013-225100503", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX08AW31G" }, { "agency": "NASA", "grant_number": "NNX11A043G" }, { "agency": "NSF", "grant_number": "AST-0808050" }, { "agency": "NSF", "grant_number": "AST-1109911" }, { "agency": "Fulbright/CONICYT Chile" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Walter Max-Moerbeck Astudillo", "deposited_on": "2014-08-28 17:05:36", "doi": "10.7907/ZX5X-V114", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673", "role": "chair" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "george@astro.caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "orcid": "0000-0002-0603-3087", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-01-31", "gradofc_approval_date": "2013-06-06", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2013", "author_list": "Max-Moerbeck Astudillo, Walter Kennerth" }, { "id": "/id/eprint/7744", "eprint_id": 7744, "rev_number": 32, "documents": [ { "id": "/id/document/38788", "doc_id": 38788, "rev_number": 3, "files": [ { "id": "/id/file/119921", "fileid": 119921, "datasetid": "document", "objectid": 38788, "filename": "Thesis_Huan_Yang_2013.pdf", "mime_type": "application/pdf", "hash": "c8b160f870aac045be2da4f50fae813a", "hash_type": "MD5", "filesize": 9426787, "mtime": "2013-05-24 22:25:32", "url": "/7744/1/Thesis_Huan_Yang_2013.pdf" } ], "eprint_id": 7744, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis", "language": "en", "security": "public", "license": "other", "main": "Thesis_Huan_Yang_2013.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": 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century, not only revolutionized our understanding of the nature of space-time and the way matter exists and interacts, but also became the building blocks of what we currently know as modern physics. My thesis studies both subjects in great depths --- this intersection takes place in gravitational-wave physics.
\r\n\r\nGravitational waves are \"ripples of space-time\", long predicted by general relativity. Although indirect evidence of gravitational waves has been discovered from observations of binary pulsars, direct detection of these waves is still actively being pursued. An international array of laser interferometer gravitational-wave detectors has been constructed in the past decade, and a first generation of these detectors has taken several years of data without a discovery. At this moment, these detectors are being upgraded into second-generation configurations, which will have ten times better sensitivity. Kilogram-scale test masses of these detectors, highly isolated from the environment, are probed continuously by photons. The sensitivity of such a quantum measurement can often be limited by the Heisenberg Uncertainty Principle, and during such a measurement, the test masses can be viewed as evolving through a sequence of nearly pure quantum states.
\r\n\r\nThe first part of this thesis (Chapter 2) concerns how to minimize the adverse effect of thermal fluctuations on the sensitivity of advanced gravitational detectors, thereby making them closer to being quantum-limited. My colleagues and I present a detailed analysis of coating thermal noise in advanced gravitational-wave detectors, which is the dominant noise source of Advanced LIGO in the middle of the detection frequency band. We identified the two elastic loss angles, clarified the different components of the coating Brownian noise, and obtained their cross spectral densities.
\r\n\r\nThe second part of this thesis (Chapters 3-7) concerns formulating experimental concepts and analyzing experimental results that demonstrate the quantum mechanical behavior of macroscopic objects - as well as developing theoretical tools for analyzing quantum measurement processes. In Chapter 3, we study the open quantum dynamics of optomechanical experiments in which a single photon strongly influences the quantum state of a mechanical object. We also explain how to engineer the mechanical oscillator's quantum state by modifying the single photon's wave function.
\r\n\r\nIn Chapters 4-5, we build theoretical tools for analyzing the so-called \"non-Markovian\" quantum measurement processes. Chapter 4 establishes a mathematical formalism that describes the evolution of a quantum system (the plant), which is coupled to a non-Markovian bath (i.e., one with a memory) while at the same time being under continuous quantum measurement (by the probe field). This aims at providing a general framework for analyzing a large class of non-Markovian measurement processes. Chapter 5 develops a way of characterizing the non-Markovianity of a bath (i.e.,whether and to what extent the bath remembers information about the plant) by perturbing the plant and watching for changes in the its subsequent evolution. Chapter 6 re-analyzes a recent measurement of a mechanical oscillator's zero-point fluctuations, revealing nontrivial correlation between the measurement device's sensing noise and the quantum rack-action noise.
\r\n\r\nChapter 7 describes a model in which gravity is classical and matter motions are quantized, elaborating how the quantum motions of matter are affected by the fact that gravity is classical. It offers an experimentally plausible way to test this model (hence the nature of gravity) by measuring the center-of-mass motion of a macroscopic object.
\r\n\r\n\r\nThe most promising gravitational waves for direct detection are those emitted from highly energetic astrophysical processes, sometimes involving black holes - a type of object predicted by general relativity whose properties depend highly on the strong-field regime of the theory. Although black holes have been inferred to exist at centers of galaxies and in certain so-called X-ray binary objects, detecting gravitational waves emitted by systems containing black holes will offer a much more direct way of observing black holes, providing unprecedented details of space-time geometry in the black-holes' strong-field region.
\r\n\r\nThe third part of this thesis (Chapters 8-11) studies black-hole physics in connection with gravitational-wave detection.
\r\n\r\nChapter 8 applies black hole perturbation theory to model the dynamics of a light compact object orbiting around a massive central Schwarzschild black hole. In this chapter, we present a Hamiltonian formalism in which the low-mass object and the metric perturbations of the background spacetime are jointly evolved. Chapter 9 uses WKB techniques to analyze oscillation modes (quasi-normal modes or QNMs) of spinning black holes. We obtain analytical approximations to the spectrum of the weakly-damped QNMs, with relative error O(1/L^2), and connect these frequencies to geometrical features of spherical photon orbits in Kerr spacetime. Chapter 11 focuses mainly on near-extremal Kerr black holes, we discuss a bifurcation in their QNM spectra for certain ranges of (l,m) (the angular quantum numbers) as a/M → 1. With tools prepared in Chapter 9 and 10, in Chapter 11 we obtain an analytical approximate for the scalar Green function in Kerr spacetime.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:05222013-233805938", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05222013-233805938", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Institute for Quantum Information and Matter", "Astronomy Department" ] }, "deposited_by": "Huan Yang", "deposited_on": "2013-05-29 20:31:59", "doi": "10.7907/JMRS-DK55", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei.chen@gmail.com", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei.chen@gmail.com", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "chair" }, { "email": "cott@tapir.caltech.edu", "id": "Ott-C-D", "name": { "family": "Ott", "given": "Christian D." }, "orcid": "0000-0003-4993-2055", "role": "member" }, { "email": "rana@ligo.caltech.edu", "id": "Adhikari-R", "name": { "family": "Adhikari", "given": "Rana" }, "orcid": "0000-0002-5731-5076", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2013-05-10", "gradofc_approval_date": "2013-05-28", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2013", "author_list": "Yang, Huan" }, { "id": "/id/eprint/7591", "eprint_id": 7591, "rev_number": 20, "documents": [ { "id": "/id/document/36786", "doc_id": 36786, "rev_number": 2, "files": [ { "id": "/id/file/115017", "fileid": 115017, "datasetid": "document", "objectid": 36786, "filename": "tajones_thesis.pdf", "mime_type": "application/pdf", "hash": "b87cf5f43a9ffa4ff048616cd8a16b7c", "hash_type": "MD5", "filesize": 6609058, "mtime": "2013-04-09 05:25:24", "url": "/7591/1/tajones_thesis.pdf" } ], "eprint_id": 7591, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "tajones_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/36786" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/36786" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/36786" } ] } } ], "eprint_status": "archive", "userid": 9170, "dir": "disk0/00/00/75/91", "datestamp": "2013-05-07 21:29:33", "lastmod": "2021-10-26 17:32:07", "status_changed": "2013-05-07 21:29:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "tuckerdangerjones@gmail.com", "id": "Jones-Tucker-A", "name": { "family": "Jones", "given": "Tucker A." }, "show_email": "NO" } ] }, "title": "Detailed Properties of High Redshift Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Galaxy formation", "abstract": "Galaxies evolve throughout the history of the universe from the first star-forming sources, through gas-rich asymmetric structures with rapid star formation rates, to the massive symmetrical stellar systems observed at the present day. Determining the physical processes which drive galaxy formation and evolution is one of the most important questions in observational astrophysics. This thesis presents four projects aimed at improving our understanding of galaxy evolution from detailed measurements of star forming galaxies at high redshift.
\r\n\r\nWe use resolved spectroscopy of gravitationally lensed z \u2243 2 - 3 star forming galaxies to measure their kinematic and star formation properties. The combination of lensing with adaptive optics yields physical resolution of \u2243 100 pc, sufficient to resolve giant Hii regions. We find that ~ 70 % of galaxies in our sample display ordered rotation with high local velocity dispersion indicating turbulent thick disks. The rotating galaxies are gravitationally unstable and are expected to fragment into giant clumps. The size and dynamical mass of giant Hii regions are in agreement with predictions for such clumps indicating that gravitational instability drives the rapid star formation. The remainder of our sample is comprised of ongoing major mergers. Merging galaxies display similar star formation rate, morphology, and local velocity dispersion as isolated sources, but their velocity fields are more chaotic with no coherent rotation.
\r\n\r\nWe measure resolved metallicity in four lensed galaxies at z = 2.0 \u2212 2.4 from optical emission line diagnostics. Three rotating galaxies display radial gradients with higher metallicity at smaller radii, while the fourth is undergoing a merger and has an inverted gradient with lower metallicity at the center. Strong gradients in the rotating galaxies indicate that they are growing inside-out with star formation fueled by accretion of metal-poor gas at large radii. By comparing measured gradients with an appropriate comparison sample at z = 0, we demonstrate that metallicity gradients in isolated galaxies must flatten at later times. The amount of size growth inferred by the gradients is in rough agreement with direct measurements of massive galaxies. We develop a chemical evolution model to interpret these data and conclude that metallicity gradients are established by a gradient in the outflow mass loading factor, combined with radial inflow of metal-enriched gas.
\r\n\r\nWe present the first rest-frame optical spectroscopic survey of a large sample of low-luminosity galaxies at high redshift (L < L*, 1.5 < z < 3.5). This population dominates the star formation density of the universe at high redshifts, yet such galaxies are normally too faint to be studied spectroscopically. We take advantage of strong gravitational lensing magnification to compile observations for a sample of 29 galaxies using modest integration times with the Keck and Palomar telescopes. Balmer emission lines confirm that the sample has a median SFR \u223c 10 M_sun yr^\u22121 and extends to lower SFR than has been probed by other surveys at similar redshift. We derive the metallicity, dust extinction, SFR, ionization parameter, and dynamical mass from the spectroscopic data, providing the first accurate characterization of the star-forming environment in low-luminosity galaxies at high redshift. For the first time, we directly test the proposal that the relation between galaxy stellar mass, star formation rate, and gas phase metallicity does not evolve. We find lower gas phase metallicity in the high redshift galaxies than in local sources with equivalent stellar mass and star formation rate, arguing against a time-invariant relation. While our result is preliminary and may be biased by measurement errors, this represents an important first measurement that will be further constrained by ongoing analysis of the full data set and by future observations.
\r\n\r\nWe present a study of composite rest-frame ultraviolet spectra of Lyman break galaxies at z = 4 and discuss implications for the distribution of neutral outflowing gas in the circumgalactic medium. In general we find similar spectroscopic trends to those found at z = 3 by earlier surveys. In particular, absorption lines which trace neutral gas are weaker in less evolved galaxies with lower stellar masses, smaller radii, lower luminosity, less dust, and stronger Ly\u03b1 emission. Typical galaxies are thus expected to have stronger Ly\u03b1 emission and weaker low-ionization absorption at earlier times, and we indeed find somewhat weaker low-ionization absorption at higher redshifts. In conjunction with earlier results, we argue that the reduced low-ionization absorption is likely caused by lower covering fraction and/or velocity range of outflowing neutral gas at earlier epochs. This result has important implications for the hypothesis that early galaxies were responsible for cosmic reionization. We additionally show that fine structure emission lines are sensitive to the spatial extent of neutral gas, and demonstrate that neutral gas is concentrated at smaller galactocentric radii in higher redshift galaxies.
\r\n\r\nThe results of this thesis present a coherent picture of galaxy evolution at high redshifts 2 \u2272 z \u2272 4. Roughly 1/3 of massive star forming galaxies at this period are undergoing major mergers, while the rest are growing inside-out with star formation occurring in gravitationally unstable thick disks. Star formation, stellar mass, and metallicity are limited by outflows which create a circumgalactic medium of metal-enriched material. We conclude by describing some remaining open questions and prospects for improving our understanding of galaxy evolution with future observations of gravitationally lensed galaxies.
", "date": "2013", "date_type": "degree", "id_number": "CaltechTHESIS:04082013-194357946", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04082013-194357946", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Tucker Jones", "deposited_on": "2013-05-07 21:29:33", "doi": "10.7907/XB2C-1B49", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "chair" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-08-16", "gradofc_approval_date": "2013-05-07", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2013", "author_list": "Jones, Tucker A." }, { "id": "/id/eprint/7043", "eprint_id": 7043, "rev_number": 25, "documents": [ { "id": "/id/document/14794", "doc_id": 14794, "rev_number": 6, "files": [ { "id": "/id/file/96061", "fileid": 96061, "datasetid": "document", "objectid": 14794, "filename": "Moore_2012_thesis.pdf", "mime_type": "application/pdf", "filesize": 35726359, "mtime": "2012-12-26 04:43:08", "url": "/7043/1/Moore_2012_thesis.pdf" } ], "eprint_id": 7043, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete Thesis", "language": "en", "security": "public", "license": "other", "main": "Moore_2012_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28034" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28034" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28034" } ] } }, { "id": "/id/document/14795", "doc_id": 14795, "rev_number": 3, "files": [ { "id": "/id/file/207926", "fileid": 207926, "datasetid": "document", "objectid": 14795, "filename": "Moore_2012_thesis_source.zip", "mime_type": "application/zip", "filesize": 58328014, "mtime": "2016-08-22 21:23:57", "url": "/7043/2/Moore_2012_thesis_source.zip" } ], "eprint_id": 7043, "pos": 2, "format": "application/zip", "format_desc": "Original source files (LaTeX)", "language": "en", "security": "internal", "license": "other", "main": "Moore_2012_thesis_source.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/28034", "doc_id": 28034, "rev_number": 2, "files": [ { "id": "/id/file/96059", "fileid": 96059, "datasetid": "document", "objectid": 28034, "filename": "preview.png", "mime_type": "image/png", "hash": "fd05f9072290168d9b14a64610584712", "hash_type": "MD5", "filesize": 43014, "mtime": "2012-12-26 04:43:08", "url": "/7043/3/preview.png" } ], "eprint_id": 7043, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "validuser", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14794" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/14794" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14794" } ] } }, { "id": "/id/document/127432", "doc_id": 127432, "rev_number": 1, "files": [ { "id": "/id/file/372868", "fileid": 372868, "datasetid": "document", "objectid": 127432, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "f97ee0d871accd25f706ac2fa18447d7", "hash_type": "MD5", "filesize": 40391, "mtime": "2021-06-24 01:45:47", "url": "/7043/4/indexcodes.txt" } ], "eprint_id": 7043, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14794" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14794" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14794" } ] } } ], "eprint_status": "archive", "userid": 844, "dir": "disk0/00/00/70/43", "datestamp": "2012-05-22 16:27:59", "lastmod": "2020-03-10 19:20:58", "status_changed": "2012-05-22 16:27:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "dcmoore@gmail.com", "id": "Moore-David-Craig", "name": { "family": "Moore", "given": "David Craig" }, "show_email": "NO" } ] }, "title": "A Search for Low-Mass Dark Matter with the Cryogenic Dark Matter Search and the Development of Highly Multiplexed Phonon-Mediated Particle Detectors", "ispublished": "unpub", "full_text_status": "public", "keywords": "Dark matter direct detection, low-mass WIMPs, superconducting particle detectors, microwave kinetic inductance detectors", "abstract": "A wide variety of astrophysical observations indicate that approximately 85% of the matter in the universe is nonbaryonic and nonluminous. Understanding the nature of this \"dark matter\" is one of the most important outstanding questions in cosmology. Weakly Interacting Massive Particles (WIMPs) are a leading candidate for dark matter since they would be thermally produced in the early universe in the correct abundance to account for the observed relic density of dark matter. If WIMPs account for the dark matter, then rare interactions from relic WIMPs should be observable in terrestrial detectors. Recently, unexplained excess events in the DAMA/LIBRA, CoGeNT, and CRESST-II experiments have been interpreted as evidence of scattering from WIMPs with masses ~10 GeV and spin-independent scattering cross sections of 10-41-10-40 cm2.
\r\n\r\nThe Cryogenic Dark Matter Search (CDMS II) attempts to identify WIMP interactions using an array of cryogenic germanium and silicon particle detectors located at the Soudan Underground Laboratory in northern Minnesota. In this dissertation, data taken by CDMS II are reanalyzed using a 2 keV recoil energy threshold to increase the sensitivity to WIMPs with masses ~10 GeV. These data disfavor an explanation for the DAMA/LIBRA, CoGeNT, and CRESST-II results in terms of spin-independent elastic scattering of WIMPs with masses \u227212 GeV, under standard assumptions. At the time of publication, they provided the strongest constraints on spin-independent elastic scattering from 5-9 GeV, ruling out previously unexplored parameter space.
\r\n\r\nTo detect WIMPs or exclude the remaining parameter space favored by the most popular models will ultimately require detectors with target masses \u22731 ton, requiring an increase in mass by more than two orders of magnitude over CDMS II. For cryogenic detectors such as CDMS, scaling to such large target masses will require individual detector elements to be fabricated more quickly and cheaply, while maintaining the nearly background-free operation of the existing experiment. We describe the development of athermal phonon mediated particle detectors using Microwave Kinetic Inductance Detectors (MKIDs), which could provide a simpler path to extending the CDMS detector technology to the ton scale. Results from prototype devices have demonstrated energy resolutions as good as \u03c3 = 0.55 keV at 30 keV, comparable to existing CDMS II detectors. Such designs can be scaled to kg-scale detector elements, while reducing the complexity of the detector fabrication and cryogenic readout electronics relative to existing designs. Since MKIDs are naturally multiplexed in the frequency domain, MKID-based designs also allow much finer pixelization of the phonon sensor, which is expected to enhance background rejection for large detectors while simultaneously reducing the number of wires needed to read out the detectors.
", "date": "2012-06-15", "date_type": "degree", "id_number": "CaltechTHESIS:05172012-142723949", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05172012-142723949", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "David Moore", "deposited_on": "2012-05-22 16:27:59", "doi": "10.7907/X8JD-4R90", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "chair" }, { "email": "hitlin@caltech.edu", "id": "Hitlin-D-G", "name": { "family": "Hitlin", "given": "David G." }, "role": "member" }, { "email": "rbpatter@caltech.edu", "id": "Patterson-R-B", "name": { "family": "Patterson", "given": "Ryan B." }, "role": "member" }, { "email": "schwab@caltech.edu", "id": "Schwab-K-C", "name": { "family": "Schwab", "given": "Keith C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-05-08", "gradofc_approval_date": "2012-05-21", "thesis_awards": "John Stager Semple Memorial Prize in Physics, 2009", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15701" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15701" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15701" } ] } } ], "eprint_status": "archive", "userid": 1954, "dir": "disk0/00/00/71/61", "datestamp": "2012-06-12 21:23:41", "lastmod": "2020-03-10 23:26:51", "status_changed": "2012-06-12 21:23:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "o.noroozian@gmail.com", "id": "Noroozian-Omid", "name": { "family": "Noroozian", "given": "Omid" }, "show_email": "YES" } ] }, "title": "Superconducting Microwave Resonator Arrays for Submillimeter/Far-infrared Imaging", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomical Instrumentation\r\nKinetic Inductance Detector\r\nMicrowave resonator\r\nPhoton detector\r\nSubmillimeter imaging\r\nSuperconducting detector", "abstract": "Superconducting microwave resonators have the potential to revolutionize submillimeter and far-infrared astronomy, and with it our understanding of the universe. The field of low-temperature detector technology has reached a point where extremely sensitive devices like transition-edge sensors are now capable of detecting radiation limited by the background noise of the universe. However, the size of these detector arrays are limited to only a few thousand pixels. This is because of the cost and complexity of fabricating large-scale arrays of these detectors that can reach up to 10 lithographic levels on chip, and the complicated SQUID-based multiplexing circuitry and wiring for readout of each detector. In order to make substantial progress, next- generation ground-based telescopes such as CCAT or future space telescopes require focal planes with large-scale detector arrays of 104\u2013106 pixels. Arrays using microwave kinetic inductance detectors (MKID) are a potential solution. These arrays can be easily made with a single layer of superconducting metal film deposited on a silicon substrate and pattered using conventional optical lithography. Furthermore, MKIDs are inherently multiplexable in the frequency domain, allowing \u223c 103 detectors to be read out using a single coaxial transmission line and cryogenic amplifier, drastically reducing cost and complexity.
\r\n\r\nAn MKID uses the change in the microwave surface impedance of a superconducting thin-film microresonator to detect photons. Absorption of photons in the superconductor breaks Cooper pairs into quasiparticles, changing the complex surface impedance, which results in a perturbation of resonator frequency and quality factor. For excitation and readout, the resonator is weakly coupled to a transmission line. The complex amplitude of a microwave probe signal tuned on-resonance and transmitted on the feedline past the resonator is perturbed as photons are absorbed in the superconductor. The perturbation can be detected using a cryogenic amplifier and subsequent homodyne mixing at room temperature. In an array of MKIDs, all the resonators are coupled to a shared feedline and are tuned to slightly different frequencies. They can be read out simultaneously using a comb of frequencies generated\r\nand measured using digital techniques.
\r\n\r\nThis thesis documents an effort to demonstrate the basic operation of \u223c 256 pixel arrays of lumped-element MKIDs made from superconducting TiNx on silicon. The resonators are designed and simulated for optimum operation. Various properties of the resonators and arrays are measured and compared to theoretical expectations. A particularly exciting observation is the extremely high quality factors (\u223c 3 \u00d7 107) of our TiNx resonators which is essential for ultra-high sensitivity. The arrays are tightly packed both in space and in frequency which is desirable for larger full-size arrays. However, this can cause a serious problem in terms of microwave crosstalk between neighboring pixels. We show that by properly designing the resonator geometry, crosstalk can be eliminated; this is supported by our measurement results. We also tackle the problem of excess frequency noise in MKIDs. Intrinsic noise in the form of an excess resonance frequency jitter exists in planar superconducting resonators that are made on dielectric substrates. We conclusively show that this noise is due to fluctuations of the resonator capacitance. In turn, the capacitance fluctuations are thought to be driven by two-level system (TLS) fluctuators in a thin layer on the surface of the device. With a modified resonator design we demonstrate with measurements that this noise can be substantially reduced. An optimized version of this resonator was designed for the multiwavelength submillimeter kinetic inductance camera (MUSIC) instrument for the Caltech Submillimeter Observatory.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:06122012-091920562", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06122012-091920562", "projects": { "items": [ "Multiwavelength Submillimeter Kinetic Inductance Camera (MUSIC)", "Cornell Caltech Atacama Telescope (CCAT)" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Jet Propulsion Laboratory (JPL) under National Aeronautics and Space Administration (NASA)", "grant_number": "NNG06GC71G" }, { "agency": "Jet Propulsion Laboratory (JPL) under National Aeronautics and Space Administration (NASA)", "grant_number": "NNX10AC83G" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Keck Institute for Space Studies" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Omid Noroozian", "deposited_on": "2012-06-12 21:23:41", "doi": "10.7907/8MG2-NB23", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "chair" }, { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "member" }, { "email": "rutledge@caltech.edu", "id": "Rutledge-D-B", "name": { "family": "Rutledge", "given": "David B." }, "role": "member" }, { "email": "sweinreb@caltech.edu", "id": "Weinreb-S", "name": { "family": "Weinreb", "given": "Sander" }, "role": "member" }, { "email": "hajimiri@caltech.edu", "id": "Hajimiri-A", "name": { "family": "Hajimiri", "given": "Ali" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-04-18", "gradofc_approval_date": "2012-06-12", "review_status": "approved", "option_major": { "items": [ "eleceng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Noroozian, Omid" }, { "id": "/id/eprint/7056", "eprint_id": 7056, "rev_number": 28, "documents": [ { "id": "/id/document/14822", "doc_id": 14822, "rev_number": 4, "files": [ { "id": "/id/file/96366", "fileid": 96366, "datasetid": "document", "objectid": 14822, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 21870219, "mtime": "2012-12-26 04:43:20", "url": "/7056/1/thesis.pdf" } ], "eprint_id": 7056, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28050" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28050" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28050" } ] } }, { "id": "/id/document/28050", "doc_id": 28050, "rev_number": 2, "files": [ { "id": "/id/file/96364", "fileid": 96364, "datasetid": "document", "objectid": 28050, "filename": "preview.png", "mime_type": "image/png", "hash": "8938f59dc9466e238773a98f9a11a513", "hash_type": "MD5", "filesize": 34547, "mtime": "2012-12-26 04:43:19", "url": "/7056/2/preview.png" } ], "eprint_id": 7056, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14822" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/14822" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14822" } ] } }, { "id": "/id/document/127449", "doc_id": 127449, "rev_number": 1, "files": [ { "id": "/id/file/372885", "fileid": 372885, "datasetid": "document", "objectid": 127449, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "b11339546718d916e057b783fa49835c", "hash_type": "MD5", "filesize": 41957, "mtime": "2021-06-24 01:46:37", "url": "/7056/3/indexcodes.txt" } ], "eprint_id": 7056, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14822" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14822" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14822" } ] } } ], "eprint_status": "archive", "userid": 9458, "dir": "disk0/00/00/70/56", "datestamp": "2012-06-05 17:14:02", "lastmod": "2022-08-25 00:01:13", "status_changed": "2012-06-05 17:14:02", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "k.batygin@gmail.com", "id": "Batygin-Konstantin", "name": { "family": "Batygin", "given": "Konstantin" }, "orcid": "0000-0002-7094-7908", "show_email": "NO" } ] }, "title": "Orbits and Interiors of Planets", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Interiors, Orbital Dynamics, Celestial Mechanics", "abstract": "The focus of this thesis is a collection of problems of timely interest in orbital dynamics and interior structure of planetary bodies.
\r\n\r\nThe first three chapters are dedicated to understanding the interior structure of close-in, gaseous extrasolar planets (hot Jupiters). In order to resolve a long-standing problem of anomalously large hot Jupiter radii, we proposed a novel magnetohydrodynamic mechanism responsible for inflation. The mechanism relies on the electro-magnetic interactions between fast atmospheric flows and the planetary magnetic field in a thermally ionized atmosphere, to induce electrical currents that flow throughout the planet. The resulting Ohmic dissipation acts to maintain the interior entropies, and by extension the radii of hot Jupiters at an enhanced level. Using self-consistent calculations of thermal evolution of hot Jupiters under Ohmic dissipation, we demonstrated a clear tendency towards inflated radii for effective temperatures that give rise to significant ionization of K and Na in the atmosphere, a trend fully consistent with the observational data. Furthermore, we found that in absence of massive cores, low-mass hot Jupiters can over-flow their Roche-lobes and evaporate on Gyr time-scales, possibly leaving behind small rocky cores. In systems where a transiting hot Jupiter is perturbed by a long-period companion, apsidal precession of the hot Jupiter that results from its tidal bulge plays an important, and often dominant role in determining the nature of the dynamical state onto which the system settles. This precession is in turn a strong function of the planet's degree of central concentration and is characterized by the planetary Love number. Utilizing this connection, we have shown that in tidally relaxed systems, measurement of the hot Jupiter's eccentricity directly yields the planetary Love number, which can then be used to place meaningful constraints on the physical structure of the planet with the aid of thermal evolution calculations.
\r\n\r\nChapters four through six focus on the improvement and implications of a model for orbital evolution of the solar system, driven by dynamical instability (termed the ``Nice\" model). Hydrodynamical studies of the orbital evolution of planets embedded in protoplanetary disks suggest that giant planets have a tendency to assemble into multi-resonant configurations. Following this argument, we used analytical methods as well as self-consistent numerical N-body simulations to identify fully-resonant primordial states of the outer solar system, whose dynamical evolutions give rise to orbital architectures that resemble the current solar system. We found a total of only eight such initial conditions, providing independent constraints for the solar system's birth environment. Next, we addressed a significant drawback of the original Nice model, namely its inability to create the physically unique, cold classical population of the Kuiper Belt. Specifically, we showed that a locally-formed cold belt can survive the transient instability, and its relatively calm dynamical structure can be reproduced. We developed a simple analytical model for dynamical excitation in the cold classical region and showed that comparatively fast apsidal precession and nodal recession of Neptune, during its eccentric phase, are essential for preservation of an unexcited state. Subsequently, we confirmed our findings with self-consistent N-body simulations, suggesting that the cold classical Kuiper belt's unique physical characteristics are a result of its remote formation site. Finally, we showed that the solar system may have initially hosted an additional ice-giant planet, that was ejected from the system during the transient phase of instability. Namely, we demonstrated that a large array of 5-planet (2 gas giants + 3 ice giants) multi-resonant initial states can lead to an adequate formation of the outer solar system, deeming the construction of a unique model of solar system's early dynamical evolution impossible.
\r\n\r\nThe last four chapters of this thesis address various aspects and consequences of dynamical relaxation of planetary orbits through dissipative effects as well as the formation of planets in binary stellar systems. Using octopole-order secular perturbation theory, we demonstrated that in multi-planet systems, tidal dissipation often drives orbits onto dynamical ``fixed points,\" characterized by apsidal alignment and lack of periodic variations in eccentricities. We applied this formalism towards investigating the possibility that the large orbital eccentricity of the transiting Neptune-mass planet Gliese 436b is maintained in the face of tidal dissipation by a second planet in the system and computed a locus of possible orbits for the putative perturber. Following up along similar lines, we used various permutations of secular theory to show that when applied specifically to close-in low-mass planetary systems, various terms in the perturbation equations become separable, and the true masses of the planets can be solved for algebraically. In practice, this means that precise knowledge of the system's orbital state can resolve the sin(i) degeneracy inherent to non-transiting planets. Subsequently, we investigated the onset of chaotic motion in dissipative planetary systems. We worked in the context of classical secular perturbation theory, and showed that planetary systems approach chaos via the so-called period-doubling route. Furthermore, we demonstrated that chaotic strange attractors can exist in mildly damped systems, such as photo-evaporating nebulae that host multiple planets. Finally, we considered planetary formation in highly inclined binary systems, where orbital excitation due to the Kozai resonance apparently implies destructive collisions among planetesimals. Through a proper account of gravitational interactions within the protoplanetary disk, we showed that fast apsidal recession induced by disk self-gravity tends to erase the Kozai effect, and ensure that the disk's unwarped, rigid structure is maintained, resolving the difficulty in planet-formation. We also showed that the Kozai effect can continue to be wiped out as a result of apsidal precession, arising from planet-planet interactions in a mature planetary system. However, if such a system undergoes a dynamical instability, its architecture may change in such a way that the Kozai effect becomes operative, giving rise to the near-unity eccentricities, observed in some extrasolar planetary systems.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:05202012-233257444", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05202012-233257444", "related_url": { "items": [ { "description": "Author website", "type": "author", "url": "http://www.gps.caltech.edu/~kbatygin/Home.html" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Konstantin Batygin", "deposited_on": "2012-06-05 17:14:02", "doi": "10.7907/KQVW-GF86", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "co-advisor" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "chair" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-01-21", "gradofc_approval_date": "2012-06-04", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Batygin, Konstantin" }, { "id": "/id/eprint/7032", "eprint_id": 7032, "rev_number": 25, "documents": [ { "id": "/id/document/14776", "doc_id": 14776, "rev_number": 4, "files": [ { "id": "/id/file/95766", "fileid": 95766, "datasetid": "document", "objectid": 14776, "filename": "NicholsDavidA2012Thesis.pdf", "mime_type": "application/pdf", "filesize": 21570916, "mtime": "2012-12-26 04:42:54", "url": "/7032/1/NicholsDavidA2012Thesis.pdf" } ], "eprint_id": 7032, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete Thesis", "language": "en", "security": "public", "license": "other", "main": "NicholsDavidA2012Thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28015" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28015" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28015" } ] } }, { "id": "/id/document/28015", "doc_id": 28015, "rev_number": 2, "files": [ { "id": "/id/file/95764", "fileid": 95764, "datasetid": "document", "objectid": 28015, "filename": "preview.png", "mime_type": "image/png", "hash": "5fd2253cc63e9afaf6ddb0e4dd6c4be0", "hash_type": "MD5", "filesize": 36291, "mtime": "2012-12-26 04:42:53", "url": "/7032/2/preview.png" } ], "eprint_id": 7032, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14776" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/14776" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14776" } ] } }, { "id": "/id/document/127412", "doc_id": 127412, "rev_number": 1, "files": [ { "id": "/id/file/372848", "fileid": 372848, "datasetid": "document", "objectid": 127412, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "3b25fb2caa860b4b42155a70abe6eeee", "hash_type": "MD5", "filesize": 44876, "mtime": "2021-06-24 01:44:32", "url": "/7032/3/indexcodes.txt" } ], "eprint_id": 7032, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14776" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14776" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14776" } ] } } ], "eprint_status": "archive", "userid": 8599, "dir": "disk0/00/00/70/32", "datestamp": "2012-05-17 15:48:52", "lastmod": "2021-10-26 17:41:56", "status_changed": "2012-05-17 15:48:52", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "d1a2nichols3@gmail.com", "id": "Nichols-David-Andrew", "name": { "family": "Nichols", "given": "David Andrew" }, "show_email": "NO" } ] }, "title": "Visualizing, Approximating, and Understanding Black-Hole Binaries", "ispublished": "unpub", "full_text_status": "public", "keywords": "black holes; gravitational waves; analytical relativity; numerical relativity", "abstract": "Numerical-relativity simulations of black-hole binaries and advancements in gravitational-wave detectors now make it possible to learn more about the collisions of compact astrophysical bodies. To be able to infer more about the dynamical behavior of these objects requires a fuller analysis of the connection between the dynamics of pairs of black holes and their emitted gravitational waves. The chapters of this thesis describe three approaches to learn more about the relationship between the dynamics of black-hole binaries and their gravitational waves: modeling momentum flow in binaries with the Landau-Lifshitz formalism, approximating binary dynamics near the time of merger with post-Newtonian and black-hole-perturbation theories, and visualizing spacetime curvature with tidal tendexes and frame-drag vortexes.
\r\n\r\nIn Chapters 2--4, my collaborators and I present a method to quantify the flow of momentum in black-hole binaries using the Landau-Lifshitz formalism. Chapter 2 reviews an intuitive version of the formalism in the first-post-Newtonian approximation that bears a strong resemblance to Maxwell\u2019s theory of electromagnetism. Chapter 3 applies this approximation to relate the simultaneous bobbing motion of rotating black holes in the superkick configuration---equal-mass black holes with their spins anti-aligned and in the orbital plane---to the flow of momentum in the spacetime, prior to the black holes\u2019\r\nmerger. Chapter 4 then uses the Landau-Lifshitz formalism to explain the dynamics of a head-on merger of spinning black holes, whose spins are anti-aligned and transverse to the infalling motion. Before they merge, the black holes move with a large, transverse, velocity, which we can explain using the post-Newtonian approximation; as the holes merge and form a single black hole, we can use the Landau-Lifshitz formalism without any approximations to connect the slowing of the final black hole to its absorbing momentum density during the merger.
\r\n\r\nIn Chapters 5--7, we discuss using analytical approximations, such as post-Newtonian and black-hole-perturbation theories, to gain further understanding into how gravitational waves are generated by black-hole binaries. Chapter 5 presents a way of combining post-Newtonian and black-hole-perturbation theories---which we call the hybrid method---for head-on mergers of black holes. It was able to produce gravitational waveforms and gravitational recoils that agreed well with comparable results from numerical-relativity simulations. Chapter 6 discusses a development of the hybrid model to include a radiation-reaction force, which is better suited for studying inspiralling black-hole binaries. The gravitational waveform from the hybrid method for inspiralling mergers agreed qualitatively with that from numerical-relativity simulations; when applied to the superkick configuration, it gave a simplified picture of the formation of the large black-hole kick. Chapter 7 describes an approximate method of calculating the frequencies of the ringdown gravitational waveforms of rotating black holes (quasinormal modes). The method generalizes a geometric interpretation of black-hole quasinormal modes and explains a degeneracy in the spectrum of these modes.
\r\n\r\nIn Chapters 8--11, we describe a new way of visualizing spacetime curvature using tools called tidal tendexes and frame-drag vortexes. This relies upon a time-space split of spacetime, which allows one to break the vacuum Riemann curvature tensor into electric and magnetic parts (symmetric, trace-free tensors that have simple physical interpretations). The regions where the eigenvalues of these tensors are large form the tendexes and vortexes of a spacetime, and the integral curves of their eigenvectors are its tendex and vortex lines, for the electric and magnetic parts, respectively. Chapter 8 provides an overview of these visualization tools and presents initial results from numerical-relativity simulations. Chapter 9 uses topological properties of vortex and tendex lines to classify properties of gravitational waves far from a source. Chapter 10 describes the formalism in more detail, and discusses the vortexes and tendexes of multipolar spacetimes in linearized gravity about flat space. The chapter helps to explain how near-zone vortexes and tendexes become gravitational waves far from a weakly gravitating, time-varying source. Chapter 11 is a detailed investigation of the vortexes and tendexes of stationary and perturbed black holes. It develops insight into how perturbations of (strongly gravitating) black holes extend from near the horizon to become gravitational waves.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:05152012-231012129", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05152012-231012129", "related_url": { "items": [ { "type": "arxiv", "url": "http://arxiv.org/abs/0808.2510" }, { "type": "arxiv", "url": "http://arxiv.org/abs/0902.4077" }, { "type": "arxiv", "url": "http://arxiv.org/abs/0907.0869" }, { "type": "arxiv", "url": "http://arxiv.org/abs/1007.2024" }, { "type": "arxiv", "url": "http://arxiv.org/abs/1109.0081" }, { "type": "arxiv", "url": "http://arxiv.org/abs/1012.4869" }, { "type": "arxiv", "url": "http://arxiv.org/abs/1107.2959" }, { "type": "arxiv", "url": "http://arxiv.org/abs/1108.5486" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "David Nichols", "deposited_on": "2012-05-17 15:48:52", "doi": "10.7907/8D56-9Y02", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "chair" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "member" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-04-30", "gradofc_approval_date": "2012-05-16", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Nichols, David Andrew" }, { "id": "/id/eprint/7030", "eprint_id": 7030, "rev_number": 29, "documents": [ { "id": "/id/document/14773", "doc_id": 14773, "rev_number": 4, "files": [ { "id": "/id/file/95743", "fileid": 95743, "datasetid": "document", "objectid": 14773, "filename": "thesis_samuel_lee.pdf", "mime_type": "application/pdf", "filesize": 3353790, "mtime": "2012-12-26 04:42:52", "url": "/7030/1/thesis_samuel_lee.pdf" } ], "eprint_id": 7030, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis_samuel_lee.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28014" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28014" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28014" } ] } }, { "id": "/id/document/28014", "doc_id": 28014, "rev_number": 2, "files": [ { "id": "/id/file/95741", "fileid": 95741, "datasetid": "document", "objectid": 28014, "filename": "preview.png", "mime_type": "image/png", "hash": "2d8e33cda5a2848980ca8d2f4c55e731", "hash_type": "MD5", "filesize": 31575, "mtime": "2012-12-26 04:42:52", "url": "/7030/2/preview.png" } ], "eprint_id": 7030, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14773" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/14773" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14773" } ] } }, { "id": "/id/document/127411", "doc_id": 127411, "rev_number": 1, "files": [ { "id": "/id/file/372847", "fileid": 372847, "datasetid": "document", "objectid": 127411, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "d39bbe9d8cfbd66848f7f3d57e2af498", "hash_type": "MD5", "filesize": 38335, "mtime": "2021-06-24 01:44:24", "url": "/7030/3/indexcodes.txt" } ], "eprint_id": 7030, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14773" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14773" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14773" } ] } } ], "eprint_status": "archive", "userid": 8650, "dir": "disk0/00/00/70/30", "datestamp": "2012-05-15 22:51:21", "lastmod": "2021-10-26 17:41:01", "status_changed": "2012-05-23 18:08:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "lee.samuel.k@gmail.com", "id": "Lee-Samuel-Kuhnman", "name": { "family": "Lee", "given": "Samuel Kuhnman" }, "show_email": "NO" } ] }, "title": "Three Paths to Particle Dark Matter", "ispublished": "unpub", "full_text_status": "public", "keywords": "particle dark matter; dark-matter annihilation; directional detection of dark matter; gravitinos; finite-temperature field theory", "abstract": "In this thesis, we explore examples of each of the three primary strategies for the detection of particle dark matter: indirect detection, direct detection, and collider production.
\r\n\r\nWe first examine the indirect detection of weakly interacting massive particle (WIMP) dark matter via the gamma-ray photons produced by astrophysical WIMP annihilation. Such photons may be observed by the Fermi Gamma-ray Space Telescope. We propose the gamma-ray-flux probability distribution function (PDF) as a probe of the Galactic halo substructure predicted to exist by N-body simulations. The PDF is calculated for a phenomenological model of halo substructure; it is shown that the PDF may allow a statistical detection of substructure.
\r\n\r\nNext, we consider the direct detection of WIMPs. We explore the ability of directional nuclear-recoil detectors to constrain the local velocity distribution of WIMP dark matter by performing Bayesian parameter estimation on simulated recoil-event data sets. We discuss in detail how directional information, when combined with measurements of the recoil-energy spectrum, helps break degeneracies in the velocity-distribution parameters. Considering the possibility that velocity structures such as cold tidal streams or a dark disk may also be present in addition to the Galactic halo, we discuss the potential of upcoming experiments to probe such structures.
\r\n\r\nWe then study the collider production of light gravitino dark matter. Light gravitino production results in spectacular signals, including di-photons, delayed photons, kinked charged tracks, and heavy metastable charged particles. We find that observable numbers of light-gravitino events may be found in future collider data sets. Remarkably, this data is also well suited to distinguish between scenarios with light gravitino dark matter, with striking implications for early-Universe cosmology.
\r\n\r\nFinally, we investigate the related matter of radiative corrections to the decay rate of charged fermions caused by the presence of a thermal bath of photons. The cancellation of finite-temperature infrared divergences in the decay rate is described in detail. Temperature-dependent radiative corrections to the two-body decay of a hypothetical charged fermion and to electroweak decays of a muon are given. We touch upon possible implications of these results for charged particles in the early Universe.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:05152012-125430182", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05152012-125430182", "related_url": { "items": [ { "type": "doi", "url": "http://dx.doi.org/10.1088/1475-7516/2009/07/007" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.82.015012" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.85.025018" }, { "type": "doi", "url": "http://dx.doi.org/10.1088/1475-7516/2012/04/029" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "U.S. Department of Energy", "grant_number": "DE-FG03-92-ER40701" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Samuel Lee", "deposited_on": "2012-05-15 22:51:21", "doi": "10.7907/Q603-SH04", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kamion@pha.jhu.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "chair" }, { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "kamion@pha.jhu.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" }, { "email": "wise@theory.caltech.edu", "id": "Wise-M-B", "name": { "family": "Wise", "given": "Mark B." }, "orcid": "0000-0002-9125-801X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-04-16", "gradofc_approval_date": "2012-05-22", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"eprint_status": "archive", "userid": 135, "dir": "disk0/00/00/65/63", "datestamp": "2011-10-19 18:52:34", "lastmod": "2021-10-26 17:41:24", "status_changed": "2011-10-19 18:52:34", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "matmat@caltech.edu", "id": "Matuszewski-Mateusz-Konrad", "name": { "family": "Matuszewski", "given": "Mateusz Konrad" }, "show_email": "YES" } ] }, "title": "The Faint Intergalactic Redshifted Emission Balloon and the Cosmic Web Imager: Two Integral Field Spectrographs Designed to Study Emission from the Intergalactic Medium", "ispublished": "unpub", "full_text_status": "public", "keywords": "FIREBall; CWI; intergalactic medium; circumgalactic medium; integral field spectroscopy; astronomical instrumentation", "abstract": "Gas in the intergalactic medium serves as the fuel for galaxies. It carries signatures of galactic feedback, including matter and energy outflows. Understanding the morphology, thermodynamics, chemistry, and kinematics of this gas is key to understanding galaxy formation and evolution. The principal method of characterizing this gas has been the study of the Lyman α forest and associated metal systems. While this work has yielded deep insights into the nature of intergalactic matter, the scarcity of suitable background sources does allow for a full three-dimensional picture. Numerical simulations and theoretical work indicate that this gas produces faint and extended recombinant line emission. Its signatures in Lyα(1216 Å), OVI(1033 Å), CIV(1550 Å) are expected to be the strongest. Recent advances in technology and fresh ideas in instrumentation are allowing access to the predicted surface brightness of intergalactic emission. The Faint Intergalactic Redshifted Emission Balloon (FIREBall) and the Cosmic Web Imager (CWI) are two integral field spectrographs probing different redshift regimes, which have been designed for the specific purpose of detecting and mapping emission from the intergalactic medium. FIREBall, operating in the balloon ultraviolet window around 2000 Å, probes the redshift range 0.3 < z < 1, while CWI, a ground-based optical instrument, studies the Universe at 2.5 < z < 7.0. Both instruments collected their first science data in mid-2009. This manuscript discusses the science case for the spectrographs, focuses on their designs, construction, testing, first light, target selection, observations, data reduction, and analysis. Initial results are presented and discussed.", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:08012011-200227855", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08012011-200227855", "projects": { "items": [ "Faint Intergalactic Redshifted Emission Balloon", "Cosmic Web Imager" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNA08AO39G" }, { "agency": "NSF", "grant_number": "AST-0505381" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Mateusz Matuszewski", "deposited_on": "2011-10-19 18:52:34", "doi": "10.7907/AGDX-5C14", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-06-30", "gradofc_approval_date": "2011-10-12", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14757" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14757" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14757" } ] } } ], "eprint_status": "archive", "userid": 6154, "dir": "disk0/00/00/65/42", "datestamp": "2011-08-15 23:35:33", "lastmod": "2020-03-10 19:21:10", "status_changed": "2011-08-15 23:35:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "zeesh.ahmed@gmail.com", "id": "Ahmed-Zeeshan", "name": { "family": "Ahmed", "given": "Zeeshan" }, "show_email": "NO" } ] }, "title": "A Dark-Matter Search Using the Final CDMS II Dataset and a Novel Detector of Surface Radiocontamination", "ispublished": "unpub", "full_text_status": "public", "keywords": "Dark Matter, Weakly Interacting Massive Particles, Cryogenic Dark Matter Search, CDMS, WIMPs, Low-temperature detectors", "abstract": "Substantial evidence from galaxies, galaxy clusters, and cosmological scales suggests that ~85% of the matter of our universe is invisible. The missing matter, or \"dark matter\" is likely composed of non-relativistic, non-baryonic particles, which have very rare interactions with baryonic matter and with one another. Among dark matter candidates, Weakly Interacting Massive Particles (WIMPs) are particularly well motivated. In the early universe, thermally produced particles with weak-scale mass and interactions would `freeze out\u2019 at the correct density to be dark matter today. Extensions to the Standard Model of particle physics, such as Supersymmetry, which solve gauge hierarchy and coupling unification problems, naturally provide such particles.
\r\n\r\nInteractions of WIMPs with baryons are expected to be rare, but might be detectable in low-noise detectors. The Cryogenic Dark Matter Search (CDMS) experiment uses ionization- and phonon- sensitive germanium particle detectors to search for such interactions. CDMS detectors are operated at the Soudan Underground Laboratory in Minnesota, within a shielded environment to lower cosmogenic and radioactive background. The combination of phonon and ionization signatures from the detectors provides excellent residual-background rejection.
\r\n\r\nThis dissertation presents improved techniques for phonon calibration of CDMS II detectors and the analysis of the final CDMS II dataset with 612 kg-days of exposure. We set a limit of 3.8x10^(-44) cm^2 on WIMP-nucleon spin-independent scattering cross section for a WIMP mass of 70 GeV/c^2. At the time this analysis was published, these data presented the most stringent limits on WIMP scattering for WIMP masses over 42 GeV/c^2, ruling out previously unexplored parameter space.
\r\n\r\nNext-generation rare-event searches such as SuperCDMS, COUPP, and CLEAN will be limited in sensitivity, unless they achieve stringent control of the surface radioactive contamination on their detectors. Low-penetrating radiation, such as alpha and beta particles, will mimic signal in these experiments. This dissertation also presents the design and prototyping of a novel detector for surface radiocontaminants, called the BetaCage --- a neon-gas time projection chamber built from radiopure materials and operated underground with shielding similar to CDMS II. The BetaCage will enable beta screening of materials at world-best sensitivity of 10^(-5)/cm^2/keV/day, providing a valuable tool to the physics community.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:07182011-183516791", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:07182011-183516791", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Updated version submitted by author 5/9/2012", "deposited_by": "Zeeshan Ahmed", "deposited_on": "2011-08-15 23:35:33", "doi": "10.7907/W7TT-1E07", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "chair" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "member" }, { "email": "bradf@caltech.edu", "id": "Filippone-B-W", "name": { "family": "Filippone", "given": "Bradley W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-07-14", "gradofc_approval_date": "2011-08-03", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"pos": 9, "placement": 9, "mime_type": "text/x-c", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/13590" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13590" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13590" } ] } } ], "eprint_status": "archive", "userid": 5454, "dir": "disk0/00/00/65/34", "datestamp": "2011-10-19 18:55:09", "lastmod": "2021-10-26 17:42:23", "status_changed": "2011-10-19 18:55:09", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "amy.trangsrud@gmail.com", "id": "Trangsrud-Amy-Ruth", "name": { "family": "Trangsrud", "given": "Amy Ruth" }, "show_email": "NO" } ] }, "title": "The SPIDER CMB Polarimeter", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astrophysics; Experiment; Cosmic Microwave Background; Polarization; Inflation; SPIDER; Bolometers; Antenna-coupled Transition Edge Sensors", "abstract": "SPIDER is a balloon-borne millimeter-wave telescope designed to study the polarization of the Cosmic Microwave Background (CMB). SPIDER will map 10% of the full sky with degree-scale beams to search for the distinctive inflationary gravitational wave signal on angular scales between 1 degree and 10 degrees, thereby probing the energy scale of inflation. In its first flight, SPIDER will field 2,400 antenna-coupled bolometers split between two bands centered at 93 GHz and 148 GHz. Slot antenna arrays, band defining microstrip filters and superconducting bolometers are all fabricated photolithographically on a shared silicon substrate. SPIDER's detectors are split amongst six monochromatic on-axis refractors in a shared helium-cooled cryostat. This thesis reviews the design of SPIDER and its antenna-coupled bolometers, and details the currently achieved performance of SPIDER's receivers.", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:07022011-083421311", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:07022011-083421311", "projects": { "items": [ "SPIDER" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "NNX09AP08H" }, { "agency": "NASA", "grant_number": "NNX07AL64G" }, { "agency": "Gordon and Betty Moore Foundation" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Amy Trangsrud", "deposited_on": "2011-10-19 18:55:09", "doi": "10.7907/83YV-A258", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "advisor" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "chair" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-07-26", "gradofc_approval_date": "2011-10-12", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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Along with our results we provide concise overviews of the considered phenomena and outline major open questions.
\r\n\r\nThe first part of this work is focused on the epoch of inflation. We analyze the evolution of early density fluctuations which originate during inflation and connect physical fields driving inflation with observable parameters. We study several inflationary scenarios, specifically one field inflation, in which the only field present during that epoch is the inflaton field and two field inflation, in which along with the inflaton field the epoch of inflation is effected by the second scalar field - curvaton field. Single field inflationary models predict nearly Gaussian initial conditions and hence a detection of non-Gaussianity would be a signature of more complex inflationary scenarios. In this work we study the effect of primordial non-Gaussianity on the cosmic microwave background (CMB) and on large-scale structure in a two-field inflationary model in which both the inflaton and curvaton fields contribute to the primordial density fluctuations. We show that in addition to the previously described enhancement of the galaxy bias on large scales, this setup results in large-scale stochasticity. We provide joint constraints on the local non-Gaussianity parameter f nl and the ratio of the amplitude of primordial perturbations due to the inflaton and curvaton using WMAP and Sloan Digital Sky Survey (SDSS) data.
\r\n\r\nThe second and largest part of this study is focused on the formation of the first cosmic structures and the effect of relative velocity between dark matter and baryonic fluids. In that part we discuss a very important and previously unnoticed effect which significantly changes the process of structure formation in the early universe. At the time of recombination, baryons and photons decoupled and the sound speed in the baryonic fluid dropped from relativistic, to the thermal velocity of the hydrogen atoms. This is less than the relative velocity of baryons and dark matter computed via linear perturbation theory, so we infer that there are supersonic coherent flows of the baryons relative to the underlying potential wells created by the dark matter. As a result, the advection of small-scale perturbations (near the baryonic Jeans scale) by large-scale velocity flows is important for the formation of the first structures. This effect involves a quadratic term in the cosmological perturbation theory equations and hence has not been included in studies based on linear perturbation theory. We show that the relative motion suppresses the abundance of the first bound objects, even if one only investigates dark matter halos, and leads to qualitative changes in their spatial distribution, such as introducing scale-dependent bias and stochasticity. We further discuss possible observable implications of this effect for high-redshift galaxy clustering and reionization. Specifically we discuss in detail the effect of the relative velocity on the gas content in the early galaxies, minihaloes and the first stars. This part of the thesis also includes a concise overview of the recent studies that investigated various aspects of the relative velocity effect and showed its importance for topics ranging from star formation to precision cosmology.
\r\n\r\nThe third and final part of the thesis covers interaction between expanding shocks of the supernovae explosions with the interstellar medium. The shocks of supernovae remnants represent a unique cosmic environment which allows detailed studies of plasma physics and high-energy astrophysics phenomena in conditions unreachable in the Earth-based laboratories. Specifically, shocks of supernovae remnants are associated with production of cosmic rays - the most energetic particles that we can observe. In our study we are specifically focused on the science of Balmer-dominated shocks (BDS) - a subset of collisionless, fast shocks dominated by hydrogen line emission with both broad and narrow components. The unique feature of BDS is that they are directly observable and their observations provide an opportunity for direct testing of the phase space structure and ion velocity distribution inside of shocks.
\r\n\r\nUnderstanding of physical phenomena occurring inside of astrophysical shocks requires precise knowledge of cross sections for high-nl proton-hydrogen collisions. Until now scientists have been using approximations for these cross sections which fall short of the precision needed for robust analysis of the observed data and can no longer satisfy needs of the astrophysical community. Guided by the demand in high-precision calculations of the cross sections we developed and implemented a robust method for direct solution of the Schroedinger partial differential equation on a grid. In this work we provide a detailed description of our computational algorithm for calculating cross sections in high-nl proton-hydrogen collisions and show results for n ≤ 4. We describe the code we developed, show the results of consistency tests and describe possible extensions. Finally, we show how our results are applied to the studies of Balmer-dominated shocks and specifically how the precise cross sections for n ≤ 4 can be used in computing Balmer decrement - the ratio of Halpha and Hbeta line intensities.
\r\n", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:01042012-160039824", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01042012-160039824", "related_url": { "items": [ { "type": "author", "url": "http://www.tseliakhovich.org" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.82.043531" }, { "type": "doi", "url": "http://dx.doi.org/10.1103/PhysRevD.82.083520" }, { "type": "doi", "url": "http://dx.doi.org/10.1111/j.1365-2966.2011.19541.x" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Dmitriy Tseliakhovich", "deposited_on": "2012-01-26 23:36:14", "doi": "10.7907/T279-PV49", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "abenson@caltech.edu", "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew J." }, "orcid": "0000-0001-5501-6008", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-12-16", "gradofc_approval_date": "2012-01-26", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Tseliakhovich, Dmitriy" }, { "id": "/id/eprint/6945", "eprint_id": 6945, "rev_number": 137, "documents": [ { "id": "/id/document/14600", "doc_id": 14600, "rev_number": 14, "files": [ { "id": "/id/file/94235", "fileid": 94235, "datasetid": "document", "objectid": 14600, "filename": "richards_joseph_l_2012_thesis.pdf", "mime_type": "application/pdf", "filesize": 10085683, "mtime": "2012-12-26 04:41:54", "url": "/6945/1/richards_joseph_l_2012_thesis.pdf" } ], "eprint_id": 6945, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete Thesis", "language": "en", "security": "public", "license": "other", "main": "richards_joseph_l_2012_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { 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22:37:20", "status_changed": "2012-05-01 22:46:13", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "bigjoe@alum.mit.edu", "id": "Richards-Joseph-Lee", "name": { "family": "Richards", "given": "Joseph Lee" }, "show_email": "NO" } ] }, "title": "The Radio Variability of Gamma-Ray Blazars", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy; astrophysics; radio; radio astronomy; blazars; active galactic nuclei; gamma-ray", "abstract": "Since late 2007, we have regularly monitored over 1100 systematically selected blazars at 15 GHz using the Owens Valley Radio Observatory 40 m radio telescope. The number of sources in the program has grown to nearly 1600, including all the active galactic nuclei associated with Fermi Large Area Telescope (LAT) gamma-ray point source detections north of our declination limit of -20\u00b0. Here, we describe the first 42 months of this program, including the design and implementation of an automated data reduction pipeline and a MySQL database system for storing the reduced data and intermediate data products. Using the \"intrinsic modulation index,\" a maximum-likelihood method, we estimate the variability amplitudes for 1413 sources from their radio light curves and compare the properties of physically defined subpopulations of the sample. We find that, among our preselected sample, gamma-ray-loud blazars detected by the LAT are significantly more variable at 15 GHz, attributable to a difference in variability between the gamma-ray-loud and gamma-ray-quiet flat spectrum radio quasars. The BL Lacertae objects in the samples do not show this division in variability amplitudes. In the first two years of our program, a 3\u03c3-significant difference between variability amplitudes for sources at redshift z \u2265 1 and for sources at z < 1 was found. This difference is found no longer to be significant in the full 42-month data set, particularly after we apply an analysis method to account for the effect of cosmological time dilation. ", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:04182012-140409324", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04182012-140409324", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Joseph Richards", "deposited_on": "2012-05-01 22:46:14", "doi": "10.7907/N69P-KG16", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-10-11", "gradofc_approval_date": "2012-04-30", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Richards, Joseph Lee" }, { "id": "/id/eprint/6882", "eprint_id": 6882, "rev_number": 34, "documents": [ { "id": "/id/document/14476", "doc_id": 14476, "rev_number": 4, "files": [ { "id": "/id/file/93027", "fileid": 93027, "datasetid": "document", "objectid": 14476, "filename": "codythesis.pdf", "mime_type": "application/pdf", "filesize": 36025508, "mtime": "2012-12-26 04:41:16", "url": "/6882/1/codythesis.pdf" } ], "eprint_id": 6882, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "codythesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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22:15:10", "status_changed": "2012-05-07 16:35:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "annmarie_cody@yahoo.com", "id": "Cody-Ann-Marie", "name": { "family": "Cody", "given": "Ann Marie" }, "orcid": "0000-0002-3656-6706", "show_email": "NO" } ] }, "title": "A Search for Pulsation in Young Brown Dwarfs and Very Low Mass Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy; brown dwarfs; star formation", "abstract": "In 2005, Palla and Baraffe proposed that brown dwarfs and very low mass stars (<0.1 solar masses) may be unstable to radial oscillations during the pre-main-sequence deuterium burning phase. With associated oscillation periods of 1-4 hours, this potentially new class of pulsation offers unprecedented opportunities to probe the interiors and evolution of low-mass objects in the 1-15 million year age range. Furthermore, several previous reports of short-period variability have suggested that deuterium-burning pulsation is in fact at work in young clusters.
\r\n\r\nFor my dissertation, I developed a photometric monitoring campaign to search for low-amplitude periodic variability in young brown dwarfs and very low mass stars using meter-class telescopes from both the ground and space. The resulting high-precision, high-cadence time-series photometry targeted four young clusters and achieved sensitivity to periodic oscillations with photometric amplitudes down to several millimagnitudes. This unprecedented variability census probed timescales ranging from minutes to weeks in a sample of ~200 young, low-mass cluster members of IC 348, Sigma Orionis, Chamaeleon I, and Upper Scorpius. While I find a dearth of photometric periods under 10 hours, the campaign's high time resolution and precision have enabled detailed study of diverse light curve behavior in the clusters: rotational spot modulation, accretion signatures, and occultations by surrounding disk material. Analysis of the data has led to the establishment of a lower limit for the timescale of periodic photometric variability in young low-mass and substellar objects, an extension of the rotation period distribution to the brown dwarf regime, as well as insights into the connection between variability and circumstellar disks in the Sigma Orionis and Chamaeleon I clusters.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:03302012-134254713", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03302012-134254713", "related_url": { "items": [ { "type": "doi", "url": "https://doi.org/10.1088/0067-0049/191/2/389" }, { "type": "doi", "url": "https://doi.org/10.1088/0004-637X/741/1/9" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Ann Marie Cody", "deposited_on": "2012-05-07 16:35:00", "doi": "10.7907/N3M2-TA49", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-12-15", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"items": [ { "email": "justusbrevik@gmail.com", "id": "Brevik-Justus-Albert", "name": { "family": "Brevik", "given": "Justus Albert" }, "orcid": "0000-0002-8058-5197", "show_email": "NO" } ] }, "title": "Searching for Primordial Gravitational Waves at Degree Scales from the South Pole", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmic microwave background, polarization, polarimeter, B-mode polarization, antenna-coupled TES bolometers, SQUID multiplexer", "abstract": "We report on the preliminary performance of the Bicep2 mm-wave polarimeter, deployed in 2009 to the South Pole and will observe through 2012. Bicep2 is currently imaging the polarization of the cosmic microwave background at 150 GHz using an array of 512 antenna-coupled superconducting bolometers. It has been designed for high sensitivity and low systematics in order to pursue the primordial B-mode polarization signal. The instrument and its characterization are presented in this thesis, with particular attention to the detectors and readout system. The instrument sensitivity, mapping speed are discussed along with the expected constraint on the scalar-to-tensor ratio that should be made from one year of data.", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:05302012-095444014", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302012-095444014", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "justus.brevik@nist.gov", "deposited_by": "Justus Brevik", "deposited_on": "2013-03-01 19:09:45", "doi": "10.7907/E6Z2-CV94", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174", "role": "chair" }, { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212", "role": "member" }, { "email": "rana@caltech.edu", "id": "Adhikari-R", "name": { "family": "Adhikari", "given": "Rana" }, "orcid": "0000-0002-5731-5076", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-05-25", "gradofc_approval_date": "2012-05-30", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Brevik, Justus Albert" }, { "id": "/id/eprint/6987", "eprint_id": 6987, "rev_number": 31, "documents": [ { "id": "/id/document/14696", "doc_id": 14696, "rev_number": 4, "files": [ { "id": "/id/file/95018", "fileid": 95018, "datasetid": "document", "objectid": 14696, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 10179111, "mtime": "2012-12-26 04:42:26", "url": "/6987/2/thesis.pdf" } ], "eprint_id": 6987, "pos": 2, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/27979" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/27979" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/27979" } ] } }, { "id": "/id/document/27979", "doc_id": 27979, "rev_number": 2, "files": [ { "id": "/id/file/95016", "fileid": 95016, "datasetid": "document", "objectid": 27979, "filename": "preview.png", "mime_type": "image/png", "hash": "8847eaff02d3f8e3a52cc6a1f97e2e05", "hash_type": "MD5", "filesize": 32234, "mtime": "2012-12-26 04:42:26", "url": "/6987/3/preview.png" } ], "eprint_id": 6987, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14696" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/14696" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14696" } ] } }, { "id": "/id/document/127362", "doc_id": 127362, "rev_number": 1, "files": [ { "id": "/id/file/372798", "fileid": 372798, "datasetid": "document", "objectid": 127362, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "3adf815dfd30f370168d597b8797ad98", "hash_type": "MD5", "filesize": 27717, "mtime": "2021-06-24 01:42:09", "url": "/6987/4/indexcodes.txt" } ], "eprint_id": 6987, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14696" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14696" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14696" } ] } } ], "eprint_status": "archive", "userid": 7940, "dir": "disk0/00/00/69/87", "datestamp": "2012-05-03 17:55:17", "lastmod": "2021-10-26 17:17:53", "status_changed": "2012-05-03 17:55:17", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "elisabeth.krause@gmx.de", "id": "Krause-Anna-Elisabeth", "name": { "family": "Krause", "given": "Anna Elisabeth" }, "show_email": "NO" } ] }, "title": "Topics in Large-Scale Structure", "ispublished": "unpub", "full_text_status": "public", "keywords": "astrophysics theory;cosmology; large-scale structure of the universe; weak lensing; galaxy clustering; galaxy clusters", "abstract": "This thesis presents my personal survey of topics and methods in large-scale structure, covering a range of cosmological probes and analytical, numerical, and observational techniques.
\r\n\r\nChapters 2--4 present analytic calculations of systematic effects relevant for the interpretation of data from upcoming large-scale structure surveys: In chapter 2 we derive the relation between measured galaxy ellipticities and the cosmic shear power spectrum up to fourth order in the matter density field, accounting for multiple deflections along the light path, reduced shear, and magnification bias. In chapter 3 we develop a new third-order cosmic shear statistics, which separates shear three point correlation functions exactly into E- and B-mode correlations on a finite interval. Chapter 4 considers the effect of tidal galaxy alignments on the projected galaxy bispectrum, which are found to bias the inferred galaxy bias parameters.
\r\n\r\nChapter 5 focusses on the halo-occupation distribution formalism, which constrains the relation between galaxy luminosities and the masses of their host halos through clustering measurements. We extend this method to model the cross-correlation functions between a galaxy sample of interest and multiple tracer populations simultaneously. This technique improves the accuracy of clustering analyses for sparse galaxy populations, and we apply it to constrain the environment of $(NUV-r)$ selected green valley galaxy samples. These galaxy samples are constructed by matching the Sloan Digital Sky Survey with the latest Galaxy Evolution Explorer source catalog which provides NUV photometry. We present cross-correlation function measurements and determine the halo occupation distribution of these transitional galaxies using the multiple tracer technique.
\r\n\r\nIn chapter 6 we examine sources of scatter in scaling relations between galaxy cluster mass and thermal Sunyaev-Zeldovich (SZ) effect using cluster samples extracted from cosmological hydrodynamical simulations. This sample enables us to study for the first time the detailed evolution of merging clusters around the scaling relation for a cosmologically representative distribution of merger parameters. We find major mergers to cause an asymmetric scatter such that the inferred mass of merging systems is biased low. As the fraction of dynamically disturbed clusters increases with redshift, this analysis indicates that mergers cause a redshift-dependent bias in cluster mass scaling relations.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:04272012-102231664", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04272012-102231664", "related_url": { "items": [ { "type": "pub", "url": "http://dx.doi.org/10.1051/0004-6361/200913524" }, { "type": "pub", "url": "http://dx.doi.org/10.1111/j.1365-2966.2010.17638.x" }, { "type": "pub", "url": "http://dx.doi.org/10.1111/j.1365-2966.2011.19844.x" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Anna Elisabeth Krause", "deposited_on": "2012-05-03 17:55:17", "succeeds": 6986, "doi": "10.7907/9HX2-RW58", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "abenson@its.caltech.edu", "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew J." }, "orcid": "0000-0001-5501-6008", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-04-16", "gradofc_approval_date": "2012-04-30", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Krause, Anna Elisabeth" }, { "id": "/id/eprint/7136", "eprint_id": 7136, "rev_number": 33, "documents": [ { "id": "/id/document/15058", "doc_id": 15058, "rev_number": 4, "files": [ { "id": "/id/file/98206", "fileid": 98206, "datasetid": "document", "objectid": 15058, "filename": "tsg_thesis.pdf", "mime_type": "application/pdf", "filesize": 9877751, "mtime": "2012-12-26 04:44:18", "url": "/7136/1/tsg_thesis.pdf" } ], "eprint_id": 7136, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "tsg_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28120" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28120" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28120" } ] } }, { "id": "/id/document/28120", "doc_id": 28120, "rev_number": 2, "files": [ { "id": "/id/file/98204", "fileid": 98204, "datasetid": "document", "objectid": 28120, "filename": "preview.png", "mime_type": "image/png", "hash": "40ae7c60e822d35bec68158802429c77", "hash_type": "MD5", "filesize": 42759, "mtime": "2012-12-26 04:44:18", "url": "/7136/2/preview.png" } ], "eprint_id": 7136, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15058" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/15058" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15058" } ] } }, { "id": "/id/document/127567", "doc_id": 127567, "rev_number": 1, "files": [ { "id": "/id/file/373003", "fileid": 373003, "datasetid": "document", "objectid": 127567, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "66c89fecee2bae2c1aa24852be9d1b8d", "hash_type": "MD5", "filesize": 27752, "mtime": "2021-06-24 01:52:16", "url": "/7136/3/indexcodes.txt" } ], "eprint_id": 7136, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15058" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15058" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15058" } ] } } ], "eprint_status": "archive", "userid": 6314, "dir": "disk0/00/00/71/36", "datestamp": "2012-06-06 23:13:43", "lastmod": "2021-11-05 22:50:07", "status_changed": "2012-06-06 23:13:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "tsg@astro.ufrj.br", "id": "Goncalves-Thiago-Signorini", "name": { "family": "Gon\u00e7alves", "given": "Thiago Signorini" }, "show_email": "NO" } ] }, "title": "Topics in Galaxy Evolution: Early Star Formation and Quenching", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies: formation; galaxies:starburst; galaxies:evolution; galaxies:kinematics and dynamics; galaxies:high-redshift", "abstract": "In this thesis, we present three projects designed to shed light on yet unanswered questions on galaxy formation and evolution. The first two concern a sample of UV-bright starburst galaxies in the local universe (z~0.2). These objects are remarkably similar to star-forming galaxies that were abundant at high redshifts (2<z<3) - the Lyman break galaxies - and can help explain the very distinctive properties observed at such epochs. Thus, these galaxies are denominated Lyman break analogs, or LBAs.
\r\n\r\nFirst, we describe a survey of kinematics of the nebular gas in such objects, and how that can help explain the formation process, including gas assembly, in these starbursts. We show strong evidence that the gas kinematics resemble those observed at high redshifts. However, by artificially manipulating our observations to mimic our objects at greater distances, we show how low resolution and signal-to-noise ratios can lead to erroneous conclusions, in particular when attempting to diagnose mergers as the origin of the starburst.
\r\n\r\nThen, we present results from a pilot survey to study the cold, molecular gas reservoir in such objects. Again, we show that the observed properties are analogous to those observed at high redshift, in particular with respect to baryonic gas fractions in the galaxy, higher than normally found in low-extinction objects in the local universe. Furthermore, we show how gas surface density and star-formation surface density follow the same relation as local galaxies, albeit at much higher values.
\r\n\r\nFinally, we discuss an observational project designed to measure the mass flux density from the blue sequence to the red sequence across the so-called green valley. We obtain the deepest spectra ever observed of green valley galaxies at intermediate redshifts (z~0.8) in order to measure spectral features from which we can measure the star formation histories of individual galaxies. We measure a mass flux ratio that is higher than observed in the local universe, indicating the red sequence was growing faster when the universe was half its present age than today.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:06052012-140445171", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06052012-140445171", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Thiago Goncalves", "deposited_on": "2012-06-06 23:13:43", "doi": "10.7907/E5T6-AC13", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "chair" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "member" }, { "email": "ds@astro.columbia.edu", "id": "Schiminovich-D", "name": { "family": "Schiminovich", "given": "David" }, "role": "member" }, { "email": "abenson@its.caltech.edu", "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew J." }, "orcid": "0000-0001-5501-6008", "role": "member" }, { "email": "johnjohn@astro.caltech.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-08-26", "gradofc_approval_date": "2012-06-06", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Gon\u00e7alves, Thiago Signorini" }, { "id": "/id/eprint/7110", "eprint_id": 7110, "rev_number": 32, "documents": [ { "id": "/id/document/15019", "doc_id": 15019, "rev_number": 4, "files": [ { "id": "/id/file/97716", "fileid": 97716, "datasetid": "document", "objectid": 15019, "filename": "Bhalerao-V-B-thesis.pdf", "mime_type": "application/pdf", "filesize": 4907106, "mtime": "2012-12-26 04:44:04", "url": "/7110/1/Bhalerao-V-B-thesis.pdf" } ], "eprint_id": 7110, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete thesis file", "language": "en", "security": "public", "license": "other", "main": "Bhalerao-V-B-thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { 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"en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15024" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15024" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15024" } ] } } ], "eprint_status": "archive", "userid": 9479, "dir": "disk0/00/00/71/10", "datestamp": "2012-06-01 22:29:20", "lastmod": "2020-03-09 17:29:01", "status_changed": "2012-06-01 22:29:20", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "varunbhalerao@gmail.com", "id": "Bhalerao-Varun-B", "name": { "family": "Bhalerao", "given": "Varun B." }, "orcid": "0000-0002-6112-7609", "show_email": "YES" } ] }, "title": "Neutron Stars and NuSTAR: A Systematic Survey of Neutron Star Masses in High Mass X-ray Binaries & Characterization of CdZnTe Detectors for NuSTAR", "ispublished": "unpub", "full_text_status": "public", "keywords": "X-ray astronomy; Space telescope; X-ray binaries; Neutron Stars", "note": "The thesis title listed in 2012 commencement program -- Neutron Stars and NuSTAR: A Systematic Survey of Neutron Star Masses in High Mass X-ray Binaries and Characterization of CdZnTe Detectors for NuSTAR -- varies from the actual thesis title.", "abstract": "My thesis centers around the study of neutron stars, especially those in massive binary systems. To this end, it has two distinct components: the observational study of neutron stars in massive binaries with a goal of measuring neutron star masses and participation in NuSTAR, the first imaging hard X-ray mission, one that is extremely well suited to the study of massive binaries and compact objects in our Galaxy.
\r\n\r\nThe Nuclear Spectroscopic Telescope Array (NuSTAR) is a NASA Small Explorer mission that will carry the first focusing high energy X-ray telescope to orbit. NuSTAR has an order-of-magnitude better angular resolution and has two orders of magnitude higher sensitivity than any currently orbiting hard X-ray telescope. I worked to develop, calibrate, and test CdZnTe detectors for NuSTAR. I describe the CdZnTe detectors in comprehensive detail here \u2014 from readout procedures to data analysis. Detailed calibration of detectors is necessary for analyzing astrophysical source data obtained by the NuSTAR. I discuss the design and implementation of an automated setup for calibrating flight detectors, followed by calibration procedures and results.
\r\n\r\nNeutron stars are an excellent probe of fundamental physics. The maximum mass of a neutron star can put stringent constraints on the equation of state of matter at extreme pressures and densities. From an astrophysical perspective, there are several open questions in our understanding of neutron stars. What are the birth masses of neutron stars? How do they change in binary evolution? Are there multiple mechanisms for the formation of neutron stars? Measuring masses of neutron stars helps answer these questions. Neutron stars in high-mass X-ray binaries have masses close to their birth mass, providing an opportunity to disentangle the role of \"nature\" and \"nurture\" in the observed mass distributions. In 2006, masses had been measured for only six such objects, but this small sample showed the greatest diversity in masses among all classes of neutron star binaries. Intrigued by this diversity \u2014 which points to diverse birth masses \u2014 we undertook a systematic survey to measure the masses of neutron stars in nine high-mass X-ray binaries. In this thesis, I present results from this ongoing project.
\r\n\r\nWhile neutron stars formed the primary focus of my work, I also explored other topics in compact objects. Appendix A describes the discovery and complete characterization of a 1RXS J173006.4+033813, a polar cataclysmic variable. Appendix B describes the discovery of a diamond planet orbiting a millisecond pulsar, and our search for its optical counterpart.
", "date": "2012", "date_type": "degree", "id_number": "CaltechTHESIS:05312012-150403422", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05312012-150403422", "related_url": { "items": [ { "description": "NUSTAR website", "type": "org", "url": "http://www.nustar.caltech.edu" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Varun Bhalerao", "deposited_on": "2012-06-01 22:29:20", "doi": "10.7907/CVT1-VR08", "alt_title": { "items": [ "Neutron Stars and NuSTAR: A Systematic Survey of Neutron Star Masses in High Mass X-ray Binaries and Characterization of CdZnTe Detectors for NuSTAR" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "advisor" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "chair" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "member" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "role": "member" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2012-05-24", "gradofc_approval_date": "2012-06-01", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2012", "author_list": "Bhalerao, Varun B." }, { "id": "/id/eprint/6395", "eprint_id": 6395, "rev_number": 47, "documents": [ { "id": "/id/document/12786", "doc_id": 12786, "rev_number": 6, "files": [ { "id": "/id/file/82712", "fileid": 82712, "datasetid": "document", "objectid": 12786, "filename": "Kasliwal_PhD_Thesis.pdf", "mime_type": "application/pdf", "filesize": 7367790, "mtime": "2012-12-26 04:35:28", "url": "/6395/1/Kasliwal_PhD_Thesis.pdf" } ], "eprint_id": 6395, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Kasliwal PhD Thesis", "language": "en", "security": "public", "license": "other", "main": "Kasliwal_PhD_Thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"/id/document/12786" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/12786" } ] } } ], "eprint_status": "archive", "userid": 4941, "dir": "disk0/00/00/63/95", "datestamp": "2011-05-31 23:09:38", "lastmod": "2021-11-05 22:51:36", "status_changed": "2011-05-31 23:09:38", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mansi@astro.caltech.edu", "id": "Kasliwal-Mansi-Manoj", "name": { "family": "Kasliwal", "given": "Mansi Manoj" }, "orcid": "0000-0002-5619-4938", "show_email": "YES" } ] }, "title": "Bridging the Gap: Elusive Explosions in the Local Universe", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy; transient; nova; supernova; palomar; keck; survey; local universe; nearby galaxies; photometry; spectroscopy; optical; radio; infrared; ultraviolet; gamma-ray; x-ray; evla; swift; gap; macronova; white dwarf; neutron star; black hole; ", "abstract": "For centuries, we have known that our dynamic universe is adorned by cosmic fireworks: energetic and ephemeral beacons of light from a single star that are a million (nova) to a billion (supernova) times brighter than our sun. However, it had been an age-old conundrum that the brightest nova is approximately 1000 times fainter than than the faintest supernova; why should nature leave such a wide \"gap\"?
\r\n\r\nIn search of an answer, I undertook three systematic surveys for my thesis. Since I was looking for transients fainter, faster and rarer than supernovae, I focused my search on galaxies in the local universe. We now have convincing evidence of multiple, distinct populations of rare transients bridging this \"gap\". Perhaps, we are witnessing new stellar physics --- shell detonations in ultra-compact white dwarf binaries, electron-capture supernovae, white dwarfs collapsing into neutron stars and birth of black-holes.
\r\n\r\nA small number of intensively followed-up discoveries of elusive transients sets the stage for population studies with the upcoming \"Large Synoptic Survey Telescope\". This effort works towards building a complete inventory of transients in the local universe (d < 200 Mpc). It better prepares us for the search for potential electromagnetic counterparts to events in the emerging fields of gravitational wave, neutrino and ultra high energy cosmic ray astronomy as these experiments are also limited to the local universe.
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G. 2001, PASP, 113, 308\r\n\r\nMoriya, T., Tomi" ] }, "projects": { "items": [ "Palomar Transient Factory (PTF)", "Palomar 60-inch Fast Transients In Nearest Galaxies (P60-FasTING)", "Canada France Hawaii Telescope Coma and Virgo Exploration for Transients (CFHT-COVET)" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation", "grant_number": "Hale Fellowship" }, { "agency": "NASA", "grant_number": "NNX09AN54G" }, { "agency": "NASA", "grant_number": "NNX10AK32G" }, { "agency": "Smithsonian", "grant_number": "G09-0046-X" }, { "agency": "Palomar Transient Factory Collaboration" }, { "agency": "National Science Foundation", "grant_number": "AST-1009987" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Mansi Kasliwal", "deposited_on": "2011-05-31 23:09:38", "doi": "10.7907/EA7Q-WX87", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. 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S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "dfrail@nrao.edu", "id": "Frail-D-A", "name": { "family": "Frail", "given": "Dale A." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-04-26", "gradofc_approval_date": "2011-05-31", "thesis_awards": "Everhart Distinguished Graduate Student Lecturer Award, 2011", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"Bode-Jason-Nathaniel", "name": { "family": "Bode", "given": "Jason Nathaniel" }, "show_email": "NO" } ] }, "title": "Black Hole Mergers and Their Electromagnetic Counterparts", "ispublished": "unpub", "full_text_status": "public", "keywords": "Black Holes, super-massive black holes, extreme mass-ratio inspirals, circumbinary disks, electromagnetic counterparts to gravitational wave signals", "abstract": "Over the past ten years it has become increasingly clear that most, if not all, galaxies have super-massive black holes lurking in their cores. The implications for this are large as they not only have significant effects on the host galaxies, far beyond what would have been naively expected, but would provide several significant gravitational wave sources to the Laser Interferometer Space Antenna (LISA). This thesis is primarily concerned with these gravitational wave sources and the possible electromagnetic counterparts. In particular, when two galaxies merge, it leads to the ultimate merger of their individual SMBHs. If gas is present near the time of merger a circumbinary disk forms around the binary. By assuming the disk is pressureless, and looking at the limits of this approximation, in Chapter 2 we develop an analytic theory of the reaction of such a gaseous disk to the gravitational wave mass loss and recoil kicks which occur during a SMBH merger. However, to understand the effects of finite pressure, in Chapter 3 we develop a one-dimensional hydrodynamic code. The efficiency of the code and the power of the analytic solution allow us to explain the entirety of possible reactions. These results are also favorably compared with far more complicated 3D relativistic magneto-hydrodynamics simulations. LISA will not see only the mergers of two SMBHs, it would also see the inspirals of stellar-mass objects into a SMBH. In Chapter 4 we discuss a new channel of formation of these extreme mass ratio inspirals (EMRIs). This new channel of EMRI formation is rich physically and, in particular, almost always requiring either the Kozai mechanism or an as-of-yet unnoticed phenomenon which we dub the reverse Kozai mechanism. We find that this channel of EMRI formation produces modest numbers of EMRIs when compared to the primary channel of EMRI formation, which, under optimistic detection scenarios for the most recent LISA design, results in the plausible detection of several. Finally, an unrelated project that considers solving the self-similar Type-II strong-shock problem in slightly asymmetric media is given in Chapter 5. We show that the results can even be applied to explosions along weak discontinuities in the density. 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I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"/id/document/12863" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/12863" } ] } } ], "eprint_status": "archive", "userid": 2002, "dir": "disk0/00/00/64/74", "datestamp": "2011-05-31 23:06:02", "lastmod": "2020-03-10 23:27:11", "status_changed": "2011-05-31 23:06:02", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "sumner@post.harvard.edu", "id": "Sumner-Matthew-Casey", "name": { "family": "Sumner", "given": "Matthew Casey" }, "show_email": "NO" } ] }, "title": "Optimizing End-to-End System Performance for Millimeter and Submillimeter Spectroscopy of Protostars: Wideband Heterodyne Receivers and Sideband-Deconvolution Techniques for Rapid Molecular-Line Surveys", "ispublished": "unpub", "full_text_status": "public", "keywords": "astrochemistry; submillimeter astronomy; millimeter astronomy; millimeter-wave; protostars; molecular lines; maximum likelihood; star formation; Caltech Submillimeter Observatory; CSO; unbiased line survey; heterodyne receiver", "abstract": "This thesis describes the construction, integration, and use of a new 230-GHz ultra-wideband heterodyne receiver, as well as the development and testing of a new sideband-deconvolution algorithm, both designed to enable rapid, sensitive molecular-line surveys.
\r\n\r\nThe 230-GHz receiver, known as Z-Rex, is the first of a new generation of wideband receivers to be installed at the Caltech Submillimeter Observatory (CSO). Intended as a proof-of-concept device, it boasts an ultra-wide IF output range of \\sim 6 - 18 GHz, offering as much as a twelvefold increase in the spectral coverage that can be achieved with a single LO setting. A similarly wideband IF system has been designed to couple this receiver to an array of WASP2 spectrometers, allowing the full bandwidth of the receiver to be observed at low resolution, ideal for extra-galactic redshift surveys. A separate IF system feeds a high-resolution 4-GHz AOS array frequently used for performing unbiased line surveys of galactic objects, particularly star-forming regions. The design and construction of the wideband IF system are presented, as is the work done to integrate the receiver and the high-resolution spectrometers into a working system. The receiver is currently installed at the CSO where it is available for astronomers' use.
\r\n\r\nIn addition to demonstrating wideband design principles, the receiver also serves as a testbed for a synthesizer-driven, active LO chain that is under consideration for future receiver designs. Several lessons have been learned, including the importance of driving the final amplifier of the LO chain into saturation and the absolute necessity of including a high-Q filter to remove spurious signals from the synthesizer output. The on-telescope performance of the synthesizer-driven LO chain is compared to that of the Gunn-oscillator units currently in use at the CSO. Although the frequency agility of the synthesized LO chain gives it a significant advantage for unbiased line surveys, the cleaner signal and broader tuning range of the Gunn continue to make it the preferred choice.
\r\n\r\nThe receiver and high-resolution spectrometer system were brought into a fully operational state late in 2007, when they were used to perform unbiased molecular-line surveys of several galactic sources, including the Orion KL hot core and a position in the L1157 outflow. In order to analyze these data, a new data pipeline was needed to deconvolve the double-sideband signals from the receiver and to model the molecular spectra. A highly automated sideband-deconvolution system has been created, and spectral-analysis tools are currently being developed.
\r\n\r\nThe sideband deconvolution relies on chi-square minimization to determine the optimal single-sideband spectrum in the presence of unknown sideband-gain imbalances and spectral baselines. Analytic results are presented for several different methods of approaching the problem, including direct optimization, nonlinear root finding, and a hybrid approach that utilizes a two-stage process to separate out the relatively weak nonlinearities so that the majority of the parameters can be found with a fast linear solver. Analytic derivations of the Jacobian matrices for all three cases are presented, along with a new Mathematica utility that enables the calculation of arbitrary gradients.
\r\n\r\nThe direct-optimization method has been incorporated into software, along with a spectral simulation engine that allows different deconvolution scenarios to be tested. The software has been validated through the deconvolution of simulated data sets, and initial results from L1157 and Orion are presented.
\r\n\r\nBoth surveys demonstrate the power of the wideband receivers and improved data pipeline to enable exciting scientific studies. The L1157 survey was completed in only 20 hours of telescope time and offers moderate sensitivity over a > 50-GHz range, from 220 GHz to approximately 270 or 280 GHz. The speed with which this survey was completed implies that the new systems will permit unbiased line surveys to become a standard observational tool. The Orion survey is expected to offer ~ 30 mK sensitivity over a similar frequency range, improving previous results by an order of magnitude. The new receiver's ability to cover such broad bandwidths permits very deep surveys to be completed in a reasonable time, and the sideband-deconvolution algorithm is capable of preserving these low noise levels. Combined, these tools can provide line spectra with the sensitivity required for constraining astrochemical models and investigating prebiotic molecules.
", "date": "2011", "date_type": "degree", "id_number": "CaltechTHESIS:05302011-143941777", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302011-143941777", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Matthew Sumner", "deposited_on": "2011-05-31 23:06:02", "doi": "10.7907/HD7X-2A80", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "chair" }, { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "member" }, { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2010-09-23", "gradofc_approval_date": "2011-05-31", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2011", "author_list": "Sumner, Matthew Casey" }, { "id": "/id/eprint/6404", "eprint_id": 6404, "rev_number": 26, "documents": [ { "id": "/id/document/12618", "doc_id": 12618, "rev_number": 4, "files": [ { "id": "/id/file/82895", "fileid": 82895, "datasetid": "document", "objectid": 12618, "filename": "yacine_thesis.pdf", "mime_type": "application/pdf", "filesize": 3852550, "mtime": "2012-12-26 04:35:34", "url": "/6404/1/yacine_thesis.pdf" } ], "eprint_id": 6404, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "yacine_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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1, "files": [ { "id": "/id/file/372104", "fileid": 372104, "datasetid": "document", "objectid": 126670, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "9d56e3ad8c56913554920caba641b4d6", "hash_type": "MD5", "filesize": 34520, "mtime": "2021-06-24 01:02:31", "url": "/6404/8/indexcodes.txt" } ], "eprint_id": 6404, "pos": 8, "placement": 8, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/12618" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/12618" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/12618" } ] } } ], "eprint_status": "archive", "userid": 5578, "dir": "disk0/00/00/64/04", "datestamp": "2011-05-27 20:35:31", "lastmod": "2021-10-26 17:20:12", "status_changed": "2011-05-27 20:35:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "yah2@nyu.edu", "id": "Ali-Haimoud-Yacine", "name": { "family": "Ali-Haimoud", "given": "Yacine" }, "show_email": "NO" } ] }, "title": "A New Spin on Primordial Hydrogen Recombination and a Refined Model for Spinning Dust Radiation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology; Cosmic Microwave Background; Primordial Recombination; Galactic Microwave Radiation; Interstellar Medium; Spinning Dust Radiation", "abstract": "This thesis describes theoretical calculations in two subjects: the primordial recombination of the electron-proton plasma about 400,000 years after the Big Bang and electric dipole radiation from spinning dust grains in the present-day interstellar medium.
\r\n\r\nPrimordial hydrogen recombination has recently been the subject of a renewed attention because of the impact of its theoretical uncertainties on predicted cosmic microwave background (CMB) anisotropy power spectra. The physics of the primordial recombination problem can be divided into two qualitatively different aspects. On the one hand, a detailed treatment of the non-thermal radiation field in the optically thick Lyman lines is required for an accurate recombination history near the peak of the visibility function. On the other hand, stimulated recombinations and out-of equilibrium effects are important at late times and a multilevel calculation is required to correctly compute the low-redshift end of the ionization history. Another facet of the problem is the requirement of computational efficiency, as a large number of recombination histories must be evaluated in Markov chains when analyzing CMB data. In this thesis, an effective multilevel atom method is presented, that speeds up multilevel atom computations by more than 5 orders of magnitude. The impact of previously ignored radiative transfer effects is quantified, and explicitly shown to be negligible. Finally, the numerical implementation of a fast and highly accurate primordial recombination code partly written by the author is described.
\r\n\r\nThe second part of this thesis is devoted to one of the potential galactic foregrounds for CMB experiments: the rotational emission from small dust grains. The rotational state of dust grains is described, first classically, and assuming that grains are rotating about their axis of greatest inertia. This assumption is then lifted, and a quantum-mechanical calculation is presented for disk-like grains with a randomized nutation state. In both cases, the probability distribution for the total grain angular momentum is computed with a Fokker-Planck equation, and the resulting emissivity is evaluated, as a function of environmental parameters. These computations are implemented in a public code written by the author.
", "date": "2011", "date_type": "degree", "id_number": "CaltechTHESIS:05172011-165447651", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05172011-165447651", "referencetext": { "items": [ "Y. Ali-Haimoud and C. M. Hirata, Phys. Rev. D, 82, 063521 (2010)", "Y. Ali-Haimoud, D. Grin, and C. M. Hirata, Phys. Rev. D, 82, 123502 (2010)", "Y. Ali-Haimoud and C. M. Hirata, Phys. Rev. D, 83, 043513 (2011)", "Y. Ali-Haimoud, C. M. Hirata and M. Kamionkowski, Phys. Rev. D, 83, 083508 (2011)", "Y. Ali-Haimoud, C. M. Hirata, and C. Dickinson, MNRAS, 395, 1055 (2009)", "K. Silsbee, Y. Ali-Haimoud, and C. M. Hirata, MNRAS, 411, 2750 (2011)" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "U.S. Department of Energy", "grant_number": "DE-FG03-92-ER40701" }, { "agency": "National Science Foundation", "grant_number": "AST-0607857 and AST-0807337" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Yacine Ali-Haimoud", "deposited_on": "2011-05-27 20:35:31", "doi": "10.7907/QMFZ-0C90", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "chirata@tapir.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2011-05-09", "gradofc_approval_date": "2011-05-27", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2011", "author_list": "Ali-Haimoud, Yacine" }, { "id": "/id/eprint/5968", "eprint_id": 5968, "rev_number": 27, "documents": [ { "id": "/id/document/10714", "doc_id": 10714, "rev_number": 4, "files": [ { "id": "/id/file/73012", "fileid": 73012, "datasetid": "document", "objectid": 10714, "filename": "final_submitted.pdf", "mime_type": "application/pdf", "filesize": 20498544, "mtime": "2012-12-26 04:29:26", "url": "/5968/1/final_submitted.pdf" } ], "eprint_id": 5968, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Schwamb Thesis", "language": "en", "security": "public", "license": "other", "main": "final_submitted.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"/id/document/10714" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/10714" } ] } } ], "eprint_status": "archive", "userid": 2167, "dir": "disk0/00/00/59/68", "datestamp": "2011-03-29 16:28:11", "lastmod": "2020-03-04 21:57:49", "status_changed": "2011-03-29 16:28:11", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mschwamb@gps.caltech.edu", "id": "Schwamb-Megan-E", "name": { "family": "Schwamb", "given": "Megan E." }, "show_email": "YES" } ] }, "title": "Beyond Sedna: Probing the Distant Solar System", "ispublished": "unpub", "full_text_status": "public", "keywords": "Kuiper belt ; Solar system", "abstract": "This thesis presents studies in observational planetary astronomy probing the structure of the Kuiper belt and beyond. The discovery of Sedna on a highly eccentric orbit beyond Neptune challenges our understanding of the solar system and suggests the presence of a population of icy bodies residing past the Kuiper belt. With a perihelion of 76 AU, Sedna is well beyond the reach of the gas-giants and could not be scattered onto its highly eccentric orbit from interactions with Neptune alone. Sedna\u2019s aphelion at \u223c1000 AU is too far from the edge of the solar system to feel the perturbing effects of passing stars or galactic tides in the present-day solar neighborhood. Sedna must have been emplaced in its orbit at an earlier time when massive unknown bodies were present in or near the solar system. The orbits of distant Sedna-like bodies are dynamically frozen and serve as the relics of their formation process.
\r\n\r\nWe have performed two surveys to search for additional members of the Sedna population. In order to find the largest and brightest Sedna-like bodies we have searched \u223c12,000 square degrees within +/- 30 degrees of the ecliptic to a limiting R magnitude of 21.3 using the QUEST camera on the 1.2m Samuel Oschin Telescope. To search for the fainter, more common members of this distant class of solar system bodies, we have performed an deep survey using the Subaru Prime Focus Camera on the 8.2m Subaru telescope covering 43 square degrees to a limiting R magnitude of 25.3. Searching over a two-night baseline, we were sensitive to motions out to distances of approximately 1000 AU.
\r\n\r\nWe present the results of these surveys. We discuss the implications for a distant Sedna-like population beyond the Kuiper belt and discuss future prospects for detecting and studying these distant bodies, focusing in particular on the constraints we can place on the embedded stellar cluster environment the early Sun may have been born in, where the location and distribution of Sedna-like orbits sculpted by multiple stellar encounters is indicative of the birth cluster size. These surveys were specifically designed to find the select members of a distant Sedna population but were also sensitive to the dynamically excited off ecliptic populations of the Kuiper belt including the hot classicals, resonant, scattered disk, and detached Kuiper belt populations. We present our observed latitude distributions and implications for the plutino population.
", "date": "2011", "date_type": "degree", "id_number": "CaltechTHESIS:07082010-134040468", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:07082010-134040468", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Megan Schwamb", "deposited_on": "2011-03-29 16:28:11", "doi": "10.7907/W4B2-1B44", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2010-06-24", "gradofc_approval_date": "2011-03-25", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2011", "author_list": "Schwamb, Megan E." }, { "id": "/id/eprint/5984", "eprint_id": 5984, "rev_number": 37, "documents": [ { "id": "/id/document/10758", "doc_id": 10758, "rev_number": 6, "files": [ { "id": "/id/file/73219", "fileid": 73219, "datasetid": "document", "objectid": 10758, "filename": "thesis_mcohen.pdf", "mime_type": "application/pdf", "filesize": 18435212, "mtime": "2012-12-26 04:29:32", "url": "/5984/1/thesis_mcohen.pdf" } ], "eprint_id": 5984, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis_mcohen.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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1, "files": [ { "id": "/id/file/371538", "fileid": 371538, "datasetid": "document", "objectid": 126104, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "dfe4776039ddb561e7d35fbbf5ae3e3e", "hash_type": "MD5", "filesize": 36897, "mtime": "2021-06-24 00:33:16", "url": "/5984/8/indexcodes.txt" } ], "eprint_id": 5984, "pos": 8, "placement": 8, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/10758" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/10758" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/10758" } ] } } ], "eprint_status": "archive", "userid": 2338, "dir": "disk0/00/00/59/84", "datestamp": "2010-09-14 21:15:58", "lastmod": "2021-10-26 18:36:39", "status_changed": "2010-09-14 21:15:58", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mcohen2@gmail.com", "id": "Cohen-Michael-Isaac", "name": { "family": "Cohen", "given": "Michael Isaac" }, "show_email": "NO" } ] }, "title": "Topics in Gravitation \u2013 Numerical Simulations of Event Horizons and Parameter Estimation for LISA", "ispublished": "unpub", "full_text_status": "public", "keywords": "event horizon numerical relativity binary black hole merger parameter estimation cosmic string LISA MLDC", "abstract": "In Part I, we consider numerical simulations of event horizons. Event horizons are the defining physical features of black hole spacetimes, and are of considerable interest in studying black hole dynamics. Here, we reconsider three techniques to find event horizons in numerical spacetimes, and find that straightforward integration of geodesics backward in time is most robust. We apply this method to various systems, from a highly spinning Kerr hole through to an asymmetric binary black hole inspiral. We find that the exponential rate at which outgoing null geodesics diverge from the event horizon of a Kerr black hole is the surface gravity of the hole. In head-on mergers we are able to track quasi-normal ringing of the merged black hole through seven oscillations, covering a dynamic range of about 105. In the head-on \"kick\" merger, we find that computing the Landau-Lifshitz velocity of the event horizon is very useful for an improved understanding of the kick behaviour. Finally, in the inspiral simulations, we find that the topological structure of the black holes does not produce an intermediate toroidal phase, though the structure is consistent with a potential re-slicing of the spacetime in order to introduce such a phase. We further discuss the topological structure of non-axisymmetric collisions.
\r\n\r\nIn Part II, we consider parameter estimation of cosmic string burst gravitational waves in Mock LISA data. A network of observable, macroscopic cosmic (super-)strings may well have formed in the early Universe. If so, the cusps that generically develop on cosmic-string loops emit bursts of gravitational radiation that could be detectable by gravitational-wave interferometers, such as the ground-based LIGO/Virgo detectors and the planned, space-based LISA detector. We develop two versions of a LISA-oriented string-burst search pipeline within the context of the Mock LISA Data Challenges, which rely on the publicly available MultiNest and PyMC software packages, respectively. We use the F-statistic to analytically maximize over the signal\u2019s amplitude and polarization, A and \u03c8, and use the FFT to search quickly over burst arrival times tC. We also demonstrate an approximate, Bayesian version of the F-statistic that incorporates realistic priors on A and \u03c8. We calculate how accurately LISA can expect to measure the physical parameters of string-burst sources, and compare to results based on the Fisher-matrix approximation. To understand LISA\u2019s angular resolution for string-burst sources, we draw maps of the waveform fitting factor [maximized over (A, \u03c8, tC)] as a function of sky position; these maps dramatically illustrate why (for LISA) inferring\r\nthe correct sky location of the emitting string loop will often be practically impossible. In addition, we identify and elucidate several symmetries that are embedded in this search problem, and we derive the distribution of cut-off frequencies fmax for observable bursts.
", "date": "2011", "date_type": "degree", "id_number": "CaltechTHESIS:08032010-144145071", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08032010-144145071", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Brinson Foundation" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-0652995" }, { "agency": "NSF", "grant_number": "DMS-0553302" }, { "agency": "NASA", "grant_number": "NNG05GG52G" }, { "agency": "NASA", "grant_number": "NNX07AM80G" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Michael Cohen", "deposited_on": "2010-09-14 21:15:58", "doi": "10.7907/TG6W-Z732", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "advisor" }, { "email": "curt.j.cutler@jpl.nasa.gov", "id": "Cutler-C-J", "name": { "family": "Cutler", "given": "Curt J." }, "role": "co-advisor" }, { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "role": "chair" }, { "email": "kip@cltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" }, { "email": "curt.j.cutler@jpl.nasa.gov", "id": "Cutler-C-J", "name": { "family": "Cutler", "given": "Curt J." }, "role": "member" }, { "email": "scheel@tapir.caltech.edu", "id": "Scheel-M", "name": { "family": "Scheel", "given": "Mark" }, "orcid": "0000-0001-6656-9134", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2010-07-26", "gradofc_approval_date": "2010-08-13", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2011", "author_list": "Cohen, Michael Isaac" }, { "id": "/id/eprint/5995", "eprint_id": 5995, "rev_number": 27, "documents": [ { "id": "/id/document/10839", "doc_id": 10839, "rev_number": 4, "files": [ { "id": "/id/file/73582", "fileid": 73582, "datasetid": "document", "objectid": 10839, "filename": "Sullivan_thesis_(FINAL).pdf", "mime_type": "application/pdf", "filesize": 34555058, "mtime": "2012-12-26 04:29:46", "url": "/5995/1/Sullivan_thesis_(FINAL).pdf" } ], "eprint_id": 5995, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Complete Thesis", "language": "en", "security": "public", "license": "other", "main": "Sullivan_thesis_(FINAL).pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"archive", "userid": 922, "dir": "disk0/00/00/59/95", "datestamp": "2010-11-01 20:58:09", "lastmod": "2020-03-04 22:00:04", "status_changed": "2010-11-01 20:58:09", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "sullivan@caltech.edu", "id": "Sullivan-Ian-Sorensen", "name": { "family": "Sullivan", "given": "Ian Sorensen" }, "show_email": "NO" } ] }, "title": "CIBER: A Near-Infrared Probe of the Epoch of Reionization", "ispublished": "unpub", "full_text_status": "public", "keywords": "Near-infrared background fluctuations; Astrophysics; Reionization; Sounding rocket", "abstract": "The Cosmic Infrared Background Experiment (CIBER) is a NASA sounding rocket payload that was first launched in February 2009. CIBER consists of four co-aligned instruments designed to study the near-Infrared background by measuring fluctuations and the absolute spectrum. The platform of a sounding rocket enables observations of the near-Infrared background outside of narrow atmospheric windows that are uncontaminated by airglow.\r\n \r\nCIBER uses two spectrometers to measure the absolute brightness spectrum of the extragalactic near-Infrared background. One, a high-resolution Fabry-Perot spectometer, is tuned to the 854.5 nm CaII line of the solar spectrum, and is designed to measure the absolute brightness of the Zodiacal Light directly, which is the source of greatest uncertainty in the near-Infrared background spectrum. The second spectrometer measures the near-Infrared background spectrum from 700 nm to 1800 nm, spanning the wavelength range where a Lyman limit cutoff feature from reionization could appear. \r\n\r\nCIBER also houses two Infrared imaging telescopes, which have identical optics that give 2 x 2 degree field of views with 7 arcsecond pixels, but have different band defining filters. The first imager has a wide band centered at 1600 nm, and images the background at the expected peak of the spectrum. The imagers\u2019 wide field of view allows them to measure the distinctive power spectrum of first-light galaxy fluctuations peaking at 10 arcminutes. The second imager has a wide band centered at 1000 nm that is intended to image at wavelengths shorter than the Lyman cutoff, and provides a powerful systematic test for any detection made at 1600 nm. First-light fluctuations should have a distinctive spatial power spectrum with very red 1600 nm / 1000 nm color, distinctly redder than the approximately solar color of any residual fluctuations arising from Zodiacal light, Galactic starlight, or moderate-redshift galaxies.\r\n\r\nThis work describes the design and characterization of the instruments for the first launch, and the modifications and further characterization that have led to a second flight in July 2010 that successfully eliminated the most serious instrumental problems identified in the first flight.\r\n", "date": "2011", "date_type": "degree", "id_number": "CaltechTHESIS:08172010-183547836", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08172010-183547836", "referencetext": { "items": [ "Abel, T., Bryan, G.L., and Norman, M.L. \"The Formation of the First Star in the Universe.\" Science 295: 93, 2002", "Aharonian, F., et al. \"Discovery of Very-High-Energy \uf067-Rays from the Galactic Centre Ridge\" Nature 440: 1018-1021, 2006", "Bock, J.J., Kawada, M., Lange, A.E., Matsumoto, T., Uemizu, K., Watabe, T., Yost, S.A., Fazio, G., Forrest, W.J., Pipher, J.L.,Price, S.D. \"Rocketborne Instrument to Search for Infrared Emission from Baryonic Dark Matter in Galactic Halos\" Proceedings SPIE 3354: 1139, 1998", "Bowman, J and Rogers Nature (submitted), 2010", "Bromm, V., Coppi, P., and Larson, R. \"The Formation of the First Stars. I. The Primordial Star-Forming Cloud\" Astrophysical Journal 564:23-51, 2002", "Brown, S.W., Eppeldauer, G.P., Rice, J.P., Zhang, J., and Lykke, K.R., \"Spectral Irradiance and Radiance Responsivity Calibrations using Uniform Sources (SIRCUS) facility at NIST\" Proceedings SPIE 5542: 363, 2004", "Ciardi, B., and Loeb, A. \"Expected number and flux distribution of gamma-ray-burst afterglows with high redshifts\" Astrophysical Journal 540:687, 2000", "Chary R.-R., Cooray, A., and Sullivan, I. \"Contribution to Unresolved Infrared Fluctuations from Dwarf Galaxies at Redshifts of 2-3\" Astrophysical Journal 681:53, 2008", "Cooray, A. and Yoshida, N. \"First Sources in Infrared Light: Stars, Supernovae and Miniquasars\" Monthly Notices of the Royal Astronomical Society 351 L71-L77, 2004", "Cooray, A., Bock, J.J., Keating, B., Lange, A.E., Matsumoto, T. \"First Star Signature in Infrared Background Anisotropies\" Astrophysical Journal 606:611-624, 2004; Erratum-ibid.622:1363, 2005", "Cooray, A., Sullivan, I., Chary, R.R., Bock, J.J., Dickenson, M., Ferguson, H.C., Keating, B., Lange, A.E., Wright, E. \"IR Background Anisotropies in Spitzer GOODS Images and Constraints on First Galaxies\" Astrophysical Journal 659:L91 L94, 2007", "Dwek, E., Arendt, R.G., Krennrich, F. \"The Near Infrared Background: Interplanetary Dust or Primordial Stars?\" Astrophysical Journal 635:784-794, 2005", "Dwek, E., Krennrich, F., and Arendt, R.G. \"Is There an Imprint of Primordial Stars in the TeV \uf067-Ray Spectrum of Blazars?\" Astrophysical Journal 634:155, 2005", "Fan, X., Strauss, M.A., Becker, R.H., White, R.L., Gunn, J.E., Knapp, G.R., Richards, G.T., Schneider, D.P., Brinkmann, J., Fukugita, M. \"Constraining the Evolution of the Ionizing Background and the Epoch of Reionization with z~6 Quasars II: A Sample of 19 Quasars\" Astronomical Journal 132:117-136, 2006", "Fan, X., Carilli, C.L., and Keating, B. \"Observational Constraints on Cosmic Reionization\" Annual Review of Astronomy and Astrophysics 44:415-462, 2006", "Kashlinsky, A., Arendt, R.G., Mather, J., Moseley, S.H. \"Tracing the First Stars with Fluctuations of the Cosmic Infrared Background. \" Nature 438: 45-50, 2005", "Kashlinsky, A., Arendt, R.G., Mather, J., Moseley, S.H. \"Demonstrating the Negligible Contribution of Optical HST ACS Galaxies to Source-Subtracted Cosmic Infrared Background Fluctuations in Deep Spitzer IRAC Images\" Astrophysical Journal 666:L1-L4, 2007", "Kelsall, T., Weiland, J. L., Franz, B. A., Reach, W. T., Arendt, R. G., Dwek, E., Freudenreich, H. T., Hauser, M. G., Moseley, S. H., Odegard, N. P., Silverberg, R. F., and Wright, E. L. \"The COBE Diffuse Infrared Background Experiment Search for the Cosmic Infrared Background: II. Model of the Interplanetary Dust Cloud\" Astrophysical Journal 508:44-73, 1998", "Komatsu, E., et al. \"Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation\" Astrophysical Journal Supplement Series (submitted), 2010", "Kovac, J., Leitch, E.M., Pryke, C., Carlstrom, J.E., Halverson, N.W., and Holzapfel, W.L. \"Detection of Polarization in the Cosmic Microwave Background using DASI.\" Nature 420:772-787, 2002", "Matsumoto, T., Matsuura, S, Murakami, H., Tanaka, M., Freund, M., and Lim, M. \"IRTS Observations of the Near-Infrared Extragalactic Background Light.\" Astrophysical Journal 626:31-43, 2005", "Mattila, K. \"The 1\uf06dm Discontinuity in the Extragalactic Background Light Spectrum: an Artefact of Foreground Subtraction.\" Monthly Notices of the Royal Astronomical Society 372:1253-1258, 2006", "Morales, M., and Wyithe, S. \"Reionization and Cosmology with 21 cm Fluctuations\" Annual Review of Astronomy and Astrophysics 48:127-171, 2010", "Primack J.R., Somerville, R.S., Bullock, J.S., Devriendt, J.E.G. \"Probing Galaxy Formation with High Energy Gamma-Rays\" AIP Conference Proceedings 558:463 478, 2001", "Pritchard, J., and Loeb, A. \"Evolution of the 21 cm Signal Throughout Cosmic History\" Physical Review D 78.103511, 2008", "Sullivan, I.S., et al. \"Clustering of the IR Background Light with Spitzer: Contribution from Resolved Sources\" Astrophysical Journal 657:37-50, 2007", "Tanvir, N.R., et al. \"A Glimpse of the End of the Dark Ages: the Gamma-Ray Burst of 23 April 2009 at Redshift 8.3\" Nature 461:1254 1257, 2009", "Thompson, R., Eisenstein, D., Fan, X., Rieke, M., and Kennicutt, R.C. \"Constraints on the Cosmic Near-Infrared Background Excess from NICMOS Deep Field Observations\" Astrophysical Journal 657:669, 2007", "Tsumura, K., Battle, J., Bock, J., Cooray, A., Hristov, V., Keating, B., Lee, D.H., Levenson, L.R., Mason, P, Matsumoto, T., Matsuura, S., Nam, U.W., Renbarger, T., Sullivan, I., Suzuki, K., Wada, T., and Zemcov, M. \"Observations of the Near-Infrared Spectrum of the Zodiacal Light with CIBER\" Astrophysical Journal 719: 394-402, 2010", "Wright, E.L. \"The Infrared Sky\" New Astronomy Reviews 49: 407-412, 2005", "York D.G. and the SDSS Collaboration \"The Sloan Digital Sky Survey: Technical Summary\" Astronomy Journal 120:1579-1587, 2000" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Ian Sullivan", "deposited_on": "2010-11-01 20:58:09", "doi": "10.7907/EFS6-PJ64", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "chair" }, { "email": "jjb@astro.caltech.edu", "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "role": "member" }, { "email": "acooray@uci.edu", "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2010-08-06", "gradofc_approval_date": "2010-10-28", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2011", "author_list": "Sullivan, Ian Sorensen" }, { "id": "/id/eprint/5710", "eprint_id": 5710, "rev_number": 25, "documents": [ { "id": "/id/document/9833", "doc_id": 9833, "rev_number": 5, "files": [ { "id": "/id/file/63144", "fileid": 63144, "datasetid": "document", "objectid": 9833, "filename": "Busch_Thesis_Revised.pdf", "mime_type": "application/pdf", "filesize": 58995910, "mtime": "2012-12-26 03:24:22", "url": "/5710/1/Busch_Thesis_Revised.pdf" } ], "eprint_id": 5710, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Busch_Thesis_Revised.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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Understanding their physical properties is essential to understanding the evolution of the solar system, and asteroid morphology is a complex field in its own right. The histories of individual asteroids, and particularly near-Earth objects, reflect continuous interaction among their shapes, rotation states, and orbits due to the effects of radiation pressure.
\r\n\r\nRadar astronomy has provided detailed information on the orbits, sizes, shapes, rotation states, and composition of many asteroids. To improve the capabilities of asteroid radar observations, I have developed the technique of radar speckle tracking. The echoes from different points on the surface of a radar target interfere with each other, producing a pattern of bright and dark speckles across the surface of the Earth. Using radio astronomy techniques, I track the motion of speckles between several ground stations during a radar experiment to accurately determine the rotation state of the target. Speckle tracking is a powerful tool to both determine the orbital evolution of near-Earth asteroids, particularly potential Earth impactors, and to survey the overall physical properties of the asteroid population.
\r\n\r\nIn addition, I have studied applying the techniques of adaptive optics and radio interferometry to asteroid science. These will become more useful with the next generation of asteroid-detecting surveys and the construction of large sub-millimeter interferometers. Interferometry in particular will soon be able to survey the entire asteroid belt.
\r\n", "date": "2010-06-11", "date_type": "degree", "id_number": "CaltechTHESIS:04082010-125341638", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04082010-125341638", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Gayle Hammer", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Michael Busch", "deposited_on": "2010-05-07 21:52:23", "doi": "10.7907/ZVGV-8X89", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "co-advisor" }, { "id": "Ostro-Steven-J", "name": { "family": "Ostro", "given": "Steven J." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "oa@gps.caltech.edu", "id": "Aharonson-O", "name": { "family": "Aharonson", "given": "Oded" }, "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2010-04-05", "gradofc_approval_date": "2010-05-06", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2010", "author_list": "Busch, Michael William" }, { "id": "/id/eprint/5767", "eprint_id": 5767, "rev_number": 18, "documents": [ { "id": "/id/document/9944", "doc_id": 9944, "rev_number": 5, "files": [ { "id": "/id/file/64428", "fileid": 64428, "datasetid": "document", "objectid": 9944, "filename": "thesis_milan.pdf", "mime_type": "application/pdf", "filesize": 14032540, "mtime": "2012-12-26 03:25:07", "url": "/5767/1/thesis_milan.pdf" } ], "eprint_id": 5767, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis_milan.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/9944" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/9944" } ] } } ], "eprint_status": "archive", "userid": 271, "dir": "disk0/00/00/57/67", "datestamp": "2010-05-07 22:01:24", "lastmod": "2020-03-09 17:29:50", "status_changed": "2010-05-07 22:01:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "milan@astro.caltech.edu", "id": "Bogosavljevi\u0107-Milan", "name": { "family": "Bogosavljevi\u0107", "given": "Milan" }, "show_email": "NO" } ] }, "title": "Lyman Continuum and Lyman \u03b1 Emission from Galaxies at High Redshift", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology; observations - galaxies; evolution - galaxies; high redshift", "abstract": "In this thesis we present two studies of star-forming galaxies at z \u22482-3 based on deep spectroscopic and narrow band imaging observations. The first study addresses pressing questions regarding the nature of galaxies \r\nwith significant escaping Lyman continuum radiation. Our second study investigates the nature of spatially extended Lyman alpha emission first observed in the form of luminous Lyman alpha \"blobs.\"
\r\n\r\nIn part I of this thesis we present the results of a deep spectroscopic survey to detect Lyman continuum radiation from individual galaxies at z\u22483. Our measurements suggest that the escape fraction is strongly variable among galaxies at all luminosities, but that there is a significant preference for higher escape fraction in objects with luminosity lower than L_star. The\r\nintegrated escaping radiation from galaxies is sufficient to complement the contribution of AGN in keeping the hydrogen in the Universe ionized. Using supporting near-IR and mid-IR photometry we derive model stellar population parameters and discover that Lyman continuum is preferentially detected among objects with lowest values for dust extinction and star-formation rate. This finding may indicate a connection between Lyman continuum escape and the evolutionary stage of a galaxy.
\r\n\r\nIn part II we present deep imaging observations in a narrow band centered on Lyman \u03b1 and H \u03b1 at the redshift of a known protocluster of star-forming galaxies (z=2.3). We discover 6 new giant and bright Lyman \u03b1 \"blobs\" and identify a large number of Lyman \u03b1 and H \u03b1 emitters at the protocluster redshift. We find an anticorrelation between Lyman \u03b1 and H \u03b1 selection, which is explained by the observation that H \u03b1 emitters show Lyman \u03b1 line in absorption in their spectra. However, the composite Lyman \u03b1 narrow-band image of H \u03b1 emitters uncovers extended emission resembling Lyman \u03b1 blobs in miniature. We conclude that faint Lyman \u03b1 emission from gas within a radius of 40 kpc (or more) is likely a feature common to most galaxies at these redshifts. If ionizing photons produced in star-forming regions are responsible for this faint Lyman \u03b1 \"glow\", then this extended flux represents a significant fraction of total predicted Lyman \u03b1 equivalent width.
\r\n", "date": "2010", "date_type": "degree", "id_number": "CaltechTHESIS:05032010-143815140", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05032010-143815140", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Gayle Hammer", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Milan Bogosavljevic", "deposited_on": "2010-05-07 22:01:24", "doi": "10.7907/KR0M-DH91", "alt_title": { "items": [ "Lyman Continuum and Lyman Alpha Emission from Galaxies at High Redshift" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "email": "george@astro.caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2010-01-14", "gradofc_approval_date": "2010-05-06", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2010", "author_list": "Bogosavljevi\u0107, Milan" }, { "id": "/id/eprint/5892", "eprint_id": 5892, "rev_number": 28, "documents": [ { "id": "/id/document/10363", "doc_id": 10363, "rev_number": 5, "files": [ { "id": "/id/file/67959", "fileid": 67959, "datasetid": "document", "objectid": 10363, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 6337361, "mtime": "2012-12-26 03:27:03", "url": "/5892/1/thesis.pdf" } ], "eprint_id": 5892, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/26003" }, 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} ] } }, { "id": "/id/document/125951", "doc_id": 125951, "rev_number": 1, "files": [ { "id": "/id/file/371385", "fileid": 371385, "datasetid": "document", "objectid": 125951, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "b6c7e8b48c848e404c91a774eadfbe4c", "hash_type": "MD5", "filesize": 42864, "mtime": "2021-06-24 00:29:02", "url": "/5892/6/indexcodes.txt" } ], "eprint_id": 5892, "pos": 6, "placement": 6, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/10363" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/10363" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/10363" } ] } } ], "eprint_status": "archive", "userid": 1849, "dir": "disk0/00/00/58/92", "datestamp": "2010-06-04 18:13:00", "lastmod": "2021-10-26 17:46:22", "status_changed": "2010-06-04 18:13:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Grin-Daniel", "name": { "family": "Grin", "given": "Daniel" }, "show_email": "NO" } ] }, "title": "The Lukewarm Frontier: Some Cosmological Consequences of 'Low Energy' Physics", "ispublished": "unpub", "full_text_status": "public", "keywords": "Axions, hydrogen recombination, effective field theory, gravity, cosmology, low-temperature reheating, kination, atomic physics.", "abstract": "In this thesis, we present four projects featuring low characteristic energy scales relative to the scales relevant for supersymmetric dark matter production or inflation. We present a telescope search for decaying relic axions in the 3 \u2212 8 eV mass range. We utilize larger telescope exposure and superior cluster mass modeling to improve sensitivity. Our results impose new stringent limits to the two-photon coupling or relic density of axions. We extend these results to non-standard sterile neutrinos.
\r\n\r\nWe then reconsider cosmological constraints to axions. Our understanding of physics before big-bang nucleosynthesis is tenuous, and after arguing that a non-standard thermal history before nucleosynthesis is plausible and perhaps even natural, we calculate the abundance and typical momenta of thermal axions in such scenarios. We generalize existing cosmological constraints to axions, showing that the allowed axion mass range expands significantly in non-standard thermal histories. We then estimate the sensitivity of future experiments to axion masses and reheating temperatures.
\r\n\r\nWe then study the ~ eV-scale physics of cosmological hydrogen ~ 10^4 states of hydrogen up to a maximum n ~ 250, and studying the associated convergence problem. We show that the recombination history is sufficiently converged for analysis of microwave anisotropy data from the Planck satellite if the maximum n ~ 128, and that previously ignored electric quadrupole transitions are indeed negligible to the precision necessary for Planck.
\r\n\r\nWe conclude by presenting a new astrophysical limit to effective \ufb01eld theories of gravity in which the graviton propagator is damped at energies greater than a milli-eV.
\r\n", "date": "2010", "date_type": "degree", "id_number": "CaltechTHESIS:05312010-162432249", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05312010-162432249", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Gayle Hammer", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Daniel Grin", "deposited_on": "2010-06-04 18:13:00", "doi": "10.7907/EN34-1095", "alt_title": { "items": [ "Some Cosmological Consequences of Low Energy Physics" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kamion@its.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "chair" }, { "email": "kamion@its.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" }, { "email": "hirata@its.caltech.edu", "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher M." }, "orcid": "0000-0002-2951-4932", "role": "member" }, { "email": "wise@its.caltech.edu", "id": "Wise-M-B", "name": { "family": "Wise", "given": "Mark B." }, "orcid": "0000-0002-9125-801X", "role": "member" }, { "email": "johnjohn@astro.caltech.edu", "id": "Johnson-J-A", "name": { "family": "Johnson", "given": "John A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2010-05-26", "gradofc_approval_date": "2010-06-03", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2010", "author_list": "Grin, Daniel" }, { "id": "/id/eprint/3227", "eprint_id": 3227, "rev_number": 13, "documents": [ { "id": "/id/document/5718", "doc_id": 5718, "rev_number": 2, "files": [ { "id": "/id/file/33850", "fileid": 33850, "datasetid": "document", "objectid": 5718, "filename": "kraus_thesis.pdf", "mime_type": "application/pdf", "filesize": 6729132, "mtime": "2012-12-26 02:58:15", "url": "/3227/1/kraus_thesis.pdf" } ], "eprint_id": 3227, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "kraus_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "kraus_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22260" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22260" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22260" } ] } }, { "id": "/id/document/9385", "doc_id": 9385, "rev_number": 3, "files": [ { "id": "/id/file/204025", "fileid": 204025, "datasetid": "document", "objectid": 9385, "filename": "Kraus_Adam_L_2010.PDF", "mime_type": "application/pdf", "filesize": 43986, "mtime": "2016-08-22 21:16:37", "url": "/3227/2/Kraus_Adam_L_2010.PDF" } ], "eprint_id": 3227, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Kraus_Adam_L_2010.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/22260", "doc_id": 22260, "rev_number": 2, "files": [ { "id": "/id/file/33848", "fileid": 33848, "datasetid": "document", "objectid": 22260, "filename": "preview.png", "mime_type": "image/png", "hash": "45208eb7c88c8eb74f6302316309cd74", "hash_type": "MD5", "filesize": 15376, "mtime": "2012-12-26 02:58:15", "url": "/3227/3/preview.png" } ], "eprint_id": 3227, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5718" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5718" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5718" } ] } }, { "id": "/id/document/123473", "doc_id": 123473, "rev_number": 1, "files": [ { "id": "/id/file/368886", "fileid": 368886, "datasetid": "document", "objectid": 123473, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "85c6b6ea29b54be3c95577ec0145966e", "hash_type": "MD5", "filesize": 54741, "mtime": "2021-06-23 22:40:55", "url": "/3227/4/indexcodes.txt" } ], "eprint_id": 3227, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5718" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5718" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5718" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/27", "datestamp": "2009-09-03", "lastmod": "2023-05-30 22:15:31", "status_changed": "2009-09-25 02:54:52", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "alk@astro.caltech.edu", "id": "Kraus-Adam-L", "name": { "family": "Kraus", "given": "Adam L." }, "show_email": "YES" } ] }, "title": "Multiple Star Formation", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy; binary stars; star formation", "abstract": "In this thesis, I present a study of the formation and evolution of stars, particularly multiple stellar systems. Binary stars provide a key constraint on star formation because any successful model should reproduce the mass-dependent frequency, distribution of separations, and distribution of mass ratios. I have pursued a number of surveys for different ranges of parameter space, all yielding one overarching conclusion: binary formation is fundamentally tied to mass. Solar-mass stars have a high primordial binary frequency (50%--75%) and a wide range of separations (extending to >10,000 AU), but as the system mass decreases, the frequency and separation distribution also decrease. For brown dwarfs, binaries are rare (~10%--15%) and have separations of <5 AU. Inside of this outer separation cutoff, the separation distribution appears to be log-flat for solar-mass stars, and perhaps for lower-mass systems. Solar-mass binary systems appear to have a flat mass ratio distribution, but for primary masses <0.3 Msun, the distribution becomes increasingly biased toward similar-mass companions.
\r\n\r\nMy results also constrain the binary formation timescale and the postformation evolutionary processes that sculpt binary populations. The dynamical interaction timescale in sparse associations like Taurus and Upper Sco is far longer than their ages, which suggests that those populations are dynamically pristine. However, binary systems in denser clusters undergo significant dynamical processing that strips outer binary companions; the difference in wide binary properties between my sample and the field is explained by the composite origin of the field population. I also have placed the individual components of young binary systems on the HR diagram in order to infer their coevality. In Taurus, binary systems are significantly more coeval (\u0394\u03c4~0.5 Myr) than the association as a whole (\u0394\u03c4~3--5 Myr).
\r\n\r\nFinally, my survey of young very-low-mass stars and brown dwarfs found no planetary-mass companions like the prototypical system 2M1207A+b. Modeling the population as either \"super-Planets\" or \"failed binaries\" indicates that the total frequency of companions with masses >1 MJup is <1%--2%. My survey of young solar-mass stars found no brown dwarf companions; evidence in favor of the brown dwarf desert is marginal, but my results do not exclude its existence.
\r\n", "date": "2010", "date_type": "degree", "id_number": "CaltechETD:etd-08252009-233632", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08252009-233632", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-09-03", "doi": "10.7907/N0KT-QH17", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "nzs@radio.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-08-25", "thesis_defense_date": "2009-07-13", "thesis_approved_date": "2009-09-03", "gradofc_approval_date": "2009-09-01", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2010", "author_list": "Kraus, Adam L." }, { "id": "/id/eprint/5284", "eprint_id": 5284, "rev_number": 25, "documents": [ { "id": "/id/document/8520", "doc_id": 8520, "rev_number": 4, "files": [ { "id": "/id/file/53001", "fileid": 53001, "datasetid": "document", "objectid": 8520, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 2524728, "mtime": "2012-12-26 03:17:54", "url": "/5284/1/thesis.pdf" } ], "eprint_id": 5284, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/24964" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/24964" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/24964" } ] } }, { "id": "/id/document/9338", "doc_id": 9338, "rev_number": 3, "files": [ { "id": "/id/file/204808", "fileid": 204808, "datasetid": "document", "objectid": 9338, "filename": "Braakman_Rogier_2010.PDF", "mime_type": "application/pdf", "filesize": 42622, "mtime": "2016-08-22 21:18:09", "url": "/5284/2/Braakman_Rogier_2010.PDF" } ], "eprint_id": 5284, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Braakman_Rogier_2010.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/24964", "doc_id": 24964, "rev_number": 2, "files": [ { "id": "/id/file/52999", "fileid": 52999, "datasetid": "document", "objectid": 24964, "filename": "preview.png", "mime_type": "image/png", "hash": "84bfa5a80a4ab7b6bc0474cfe166cfae", "hash_type": "MD5", "filesize": 14335, "mtime": "2012-12-26 03:17:54", "url": "/5284/3/preview.png" } ], "eprint_id": 5284, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/8520" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/8520" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/8520" } ] } }, { "id": "/id/document/125339", "doc_id": 125339, "rev_number": 1, "files": [ { "id": "/id/file/370773", "fileid": 370773, "datasetid": "document", "objectid": 125339, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "5f7f29f5b5bc9d219793e9ce526c2fcd", "hash_type": "MD5", "filesize": 43529, "mtime": "2021-06-24 00:06:09", "url": "/5284/4/indexcodes.txt" } ], "eprint_id": 5284, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/8520" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/8520" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/8520" } ] } } ], "eprint_status": "archive", "userid": 24, "dir": "disk0/00/00/52/84", "datestamp": "2009-12-21 18:16:15", "lastmod": "2023-11-08 00:16:43", "status_changed": "2022-11-07 22:35:35", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "braakman@mit.edu", "id": "Braakman-Rogier", "name": { "family": "Braakman", "given": "Rogier" }, "orcid": "0000-0002-4485-8450", "show_email": "NO" } ] }, "title": "Gas-Phase Terahertz Spectroscopy and the Study of Complex Interstellar Chemistry", "ispublished": "unpub", "full_text_status": "public", "keywords": "interstellar chemistry; ro-vibrational spectroscopy; THz spectroscopy; Fabry-Perot cavities", "abstract": "Terahertz spectroscopy holds great promise in the advancement of the field of astrochemistry. The sensitive observation of interstellar THz radiation is expected to lower detection limits and allow the study of larger and more complex species than is currently possible at millimeter wavelengths, which will place further constraints on chemical models and permit a direct comparison to the organic compounds seen in carbonaceous chondrites. With the successful recent launch of the Herschel Space Telescope, which will give high-fidelity access to interstellar THz radiation for the first time, and the completion of the Atacama Large Millimeter Array (ALMA) by 2013, the THz astronomy era is upon us. Unfortunately, laboratory THz spectroscopy presents significant challenges and will be soon be lagging behind the newly available observational platforms. Technologies to extend the capabilities of high-resolution spectroscopic systems into the THz domain are actively being pursued on many fronts, but affordable systems that are broadly tunable, sensitive and achieve the necessary resolution are not yet available. The work in this thesis should therefore be seen as part of the effort in the transition from centimeter-/millimeter-wave to THz spectroscopy that is currently taking place in the astrochemistry community.
\r\n\r\nAs part of this thesis, observational searches for the complex organics hydroxyacetone (CH\u2083COCH\u2082OH), 2-cyanoethanol (OHCH\u2082CH\u2082CN) and methoxyacetonitrile (CH\u2083OCH\u2082CN) were attempted at millimeter wavelengths. The unsuccessful nature of these searches highlight the current limits of studying interstellar chemistry using pure rotational spectroscopy. The characterization of the laboratory spectra of these molecules is nonetheless important as it will aid in the assignment and description of the rotational substructure and band shapes of their THz torsional spectra, features that may allow their interstellar detection; and this thesis presents methods by which such complex spectra may be rapidly and efficiently collected and fit using automated spectrometers and modern software tools.
\r\n\r\nThe description of the spectrum of hydroxyacetone is furthermore of interest due to the presence of the very low barrier to internal rotation in this molecule. Many interstellar compounds, both known and potential future targets, have functional groups capable of internal rotation in their structure; and so the effort in understanding the complex effects of the low barrier rotor in this case will benefit the general effort to further understand internal rotation.
\r\n\r\nIn searching for new interstellar molecules, both at millimeter wavelengths and at higher THz frequencies, characterization of the complete spectra of known interstellar molecules is of great importance to allow substraction of their contribution to observational spectra. In this thesis, the ground-state rotational spectrum of methanol, the most important \"interstellar weed\", is catalogued and described in detail through most of the THz region that will be accessible with Herschel and ALMA.
\r\n\r\nLastly, as part of the effort to increase the sensitivity of THz spectrometers, the use of Fabry-Perot cavities at these frequencies is explored. Such resonant cavities hold the potential to significantly increase the possible path lengths in spectroscopic system and to allow novel and sensitive detection techniques. Optimal configurations and the limits on achievable path lengths and Q-factors of such cavities are discussed, as are the possible extensions of Fourier Transform MicroWave (FT-MW) techniques to THz frequencies.
", "date": "2010", "date_type": "degree", "id_number": "CaltechTHESIS:09252009-142627047", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09252009-142627047", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Rogier Braakman", "deposited_on": "2009-12-21 18:16:15", "doi": "10.7907/R2KK-E302", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mo@its.caltech.edu", "id": "Okumura-M", "name": { "family": "Okumura", "given": "Mitchio" }, "orcid": "0000-0001-6874-1137", "role": "chair" }, { "email": "jkbarton@caltech.edu", "id": "Barton-J-K", "name": { "family": "Barton", "given": "Jacqueline K." }, "orcid": "0000-0001-9883-1600", "role": "member" }, { "email": "ram@caltech.edu", "id": "Marcus-R-A", "name": { "family": "Marcus", "given": "Rudolph A." }, "orcid": "0000-0001-6547-1469", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2009-08-20", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2010", "author_list": "Braakman, Rogier" }, { "id": "/id/eprint/3140", "eprint_id": 3140, "rev_number": 18, "documents": [ { "id": "/id/document/5585", "doc_id": 5585, "rev_number": 3, "files": [ { "id": "/id/file/32991", "fileid": 32991, "datasetid": "document", "objectid": 5585, "filename": "PBCameron_thesis.pdf", "mime_type": "application/pdf", "filesize": 3150386, "mtime": "2012-12-26 02:57:25", "url": "/3140/1/PBCameron_thesis.pdf" } ], "eprint_id": 3140, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "PBCameron_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "PBCameron_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/5585" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5585" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5585" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/40", "datestamp": "2008-10-22", "lastmod": "2020-03-09 17:30:06", "status_changed": "2009-09-25 02:52:20", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "pbc@caltech.edu", "id": "Cameron-Patrick-Brian", "name": { "family": "Cameron", "given": "Patrick Brian" }, "show_email": "NO" } ] }, "title": "The Formation and Evolution of Neutron Stars: Astrometry, Timing, and Transients", "ispublished": "unpub", "full_text_status": "public", "keywords": "adaptive optics; compact objects; neutron stars", "abstract": "In order to address open questions regarding the death of massive stars and the evolution of the stellar fossils left behind, we use techniques spanning the electromagnetic spectrum to study the youngest and oldest neutron stars. We begin by exploring and developing a new technique --- ground-based astrometry with adaptive optics. This technology is relatively new to astronomy, and has incredible potential for tracking the motions of stars. We enumerate experimental design consideration for mitigating systematic errors and present an optimal estimation algorithm capable of delivering unprecedented astrometric precision and accuracy from the ground. We verify the performance of our technique using experimental data, and discuss the astrometric potential of adaptive optics on large aperture telescopes. We then apply our knowledge to track the motions of magnetars. These objects harbor ultra-strong magnetic fields and give rise to the most intense high-energy transients in the sky. The proper motion survey presented here is the first of its kind, and is capable of directly addressing the open questions regarding their origin and evolution in a model independent fashion. We also present radio studies of the aftermath of the brightest magnetar flare ever recorded. Finally, we shift to probing the emission mechanism of the oldest neutron stars, millisecond pulsars in globular clusters, that are revived at the end of their by lives their binary companions.\r\n", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-08152008-140704", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08152008-140704", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released Jan. 4, 2016. ", "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-22", "doi": "10.7907/HTW7-8X31", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "chair" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "role": "member" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "member" }, { "email": "rgd@astro.caltech.edu", "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-15", "thesis_defense_date": "2008-06-02", "thesis_approved_date": "2008-10-22", "gradofc_approval_date": "2008-10-08", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Cameron, Patrick Brian" }, { "id": "/id/eprint/2224", "eprint_id": 2224, "rev_number": 31, "documents": [ { "id": "/id/document/4108", "doc_id": 4108, "rev_number": 3, "files": [ { "id": "/id/file/23878", "fileid": 23878, "datasetid": "document", "objectid": 4108, "filename": "01ragozzine_preamble.pdf", "mime_type": "application/pdf", "filesize": 143979, "mtime": "2012-12-26 02:48:31", "url": "/2224/1/01ragozzine_preamble.pdf" } ], "eprint_id": 2224, "pos": 1, "placement": 2, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "01ragozzine_preamble.pdf", "language": "en", "security": "public", "license": "other", "main": "01ragozzine_preamble.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": 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These problems are introduced and discussed in Chapter 1, to help provide context for the subsequent chapters. In Chapter 2, I discuss a new technique for probing the interior density distributions of extra-solar planets by observing apsidal precession. Using a detailed theoretical and observational model of this precession, I conclude that NASA's Kepler mission will be able to detect the presence or absence of a massive core in very hot Jupiters with eccentricities greater than 0.003. The remaining chapters discuss the orbital dynamics of Kuiper belt objects (KBOs) orbiting the Sun beyond Neptune. The family of dwarf planet Haumea (2003 EL61) is characterized in Chapter 3, including a list of candidate family members sorted by dynamical proximity. Using a numerical integration of resonance diffusion, I also show that the Haumea family is at least 1 Gyr old and is probably primordial. In Chapter 4, I analyze and fit astrometric data for the two satellites of Haumea (Hi'iaka and Namaka) to determine their orbital properties and the masses of Haumea and Hi'iaka. The implications of the new orbital solution are discussed, including the exciting conclusion that Haumea and Namaka are currently starting a season of mutual events. A more general investigation of the orbital and tidal evolution of KBO binaries is given in Chapter 5. A new orbital evolution model is described that accounts for perturbations from the Sun, self-consistent tidal evolution, and non-hydrostatic quadrupoles of solid KBOs. Using this model, I find that the orbital parameters of KBO binaries may have been modified significantly over the age of the solar system. Applied to the Orcus-Vanth binary, this model shows that a short-period circular orbit does not necessarily imply a collisional formation. In all, the work in this thesis has sought to analyze observational data by using the theoretical tools of orbital dynamics. ", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-05282009-164537", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05282009-164537", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-05-29", "doi": "10.7907/NRNC-XK21", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "chair" }, { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "co-chair" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "email": "oa@gps.caltech.edu", "id": "Aharonson-O", "name": { "family": "Aharonson", "given": "Oded" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-05-28", "thesis_defense_date": "2009-05-15", "thesis_approved_date": "2009-05-29", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"2009-05-29", "lastmod": "2023-11-08 00:16:43", "status_changed": "2009-09-25 02:29:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "cosalyk@vassar.edu", "id": "Salyk-Colette-Vanessa", "name": { "family": "Salyk", "given": "Colette Vanessa" }, "orcid": "0000-0003-3682-6632", "show_email": "NO" } ] }, "title": "Molecular Spectroscopy of Planet-Forming Regions in Circumstellar Disks", "ispublished": "unpub", "full_text_status": "public", "keywords": "circumstellar disks; infrared spectroscopy; planet formation; protoplanetary disks; star formation", "abstract": "Planets, now known to be common companions of nearby stars, are believed to originate in circumstellar disks - disks of gas and dust that form around collapsing protostars. Because of their small angular size, disks in nearby star-forming regions are difficult to spatially resolve. However, since radial temperature gradients are set up by the luminous central star, the peak wavelength of blackbody emission is a proxy for disk location, and spectroscopic observations can thus be used to study disk structure. In this thesis, I present spectroscopic observations of circumstellar disks obtained with the Keck Near Infrared Spectrograph (NIRSPEC) and the Spitzer Space Telescope Infrared Spectrograph (IRS).
\r\n\r\nHigh-resolution (R ~ 25000) M-band spectra have been obtained with NIRSPEC for over 100 circumstellar disks. CO vibrational emission in the M-band is nearly ubiquitous from classical, optically thick disks, and can be used to examine the disks' inner structure and gas content. The emission is consistent with high temperatures and densities, and small emitting areas, suggesting that it originates at small disk radii - a few AU or less. An analysis of CO lineshapes shows that the CO gas is truncated at or near the dust sublimation radius for low and mid-mass stars but at larger radii for more luminous stars. CO emission is also present from many transitional disks - disks in which the inner regions have been depleted of small dust grains -demonstrating that many of their inner disks have significant quantities of gas. Although the formation mechanism for transitional disks is not yet known, gas-rich inner disks are consistent with formation via tidal clearing by a giant planet.
\r\n\r\nSpitzer-IRS spectra have been obtained for 82 disks, as part of the Cores to Disks (c2d) legacy program and other archived programs, and as part of a targeted IRS GO-5 survey at high S/N. Water vapor and other gaseous molecules, including OH, HCN, C2H2, and CO2, are detected from ~ 40% of disks. Excitation temperatures for the molecular species of ~ 500 K or higher and emitting radii of a few AU suggest an origin in the planet-forming regions of the disks. There are no strong correlations between detection rates or line equivalent widths and stellar or disk parameters. However, molecular detection rates are correlated with each other, and with disk color, suggesting a dependence on disk structure. Unlike for classical disks, transitional disks show no evidence for H2O, OH, or any organic molecules, perhaps because these molecules are easily photodissociated in the optically thin inner disk.
\r\n", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-05272009-151203", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05272009-151203", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Released to public 1/25/2019 // No end date. Partially withheld: full thesis, ch. 7,9. // 03152017: Withheld Files Released and Restricted to Caltech community only until 15 September 2017.", "deposited_by": "Imported from ETD-db", "deposited_on": "2009-05-29", "doi": "10.7907/E4YF-FZ95", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-05-27", "thesis_defense_date": "2009-05-14", "thesis_approved_date": "2009-05-29", "gradofc_approval_date": "2009-05-29", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Salyk, Colette Vanessa" }, { "id": "/id/eprint/143", "eprint_id": 143, "rev_number": 17, "documents": [ { "id": "/id/document/224", "doc_id": 224, "rev_number": 2, "files": [ { "id": "/id/file/1404", "fileid": 1404, "datasetid": "document", "objectid": 224, "filename": "Thesis.pdf", "mime_type": "application/pdf", "filesize": 8308114, "mtime": "2012-12-26 02:27:37", "url": "/143/1/Thesis.pdf" } ], "eprint_id": 143, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "Thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17049" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17049" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17049" } ] } }, { "id": "/id/document/17049", "doc_id": 17049, "rev_number": 2, "files": [ { "id": "/id/file/1402", "fileid": 1402, "datasetid": "document", "objectid": 17049, "filename": "preview.png", "mime_type": "image/png", "hash": "907b746f10ebd53a06d56f49547c1648", "hash_type": "MD5", "filesize": 18980, "mtime": "2012-12-26 02:27:37", "url": "/143/2/preview.png" } ], "eprint_id": 143, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/224" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/224" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/224" } ] } }, { "id": "/id/document/119722", "doc_id": 119722, "rev_number": 1, "files": [ { "id": "/id/file/365088", "fileid": 365088, "datasetid": "document", "objectid": 119722, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "71bb548a585be1381683e78e1696cce9", "hash_type": "MD5", "filesize": 42785, "mtime": "2021-06-23 20:16:09", "url": "/143/3/indexcodes.txt" } ], "eprint_id": 143, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/224" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/224" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/224" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/01/43", "datestamp": "2009-02-06", "lastmod": "2020-03-10 23:39:04", "status_changed": "2009-09-25 01:29:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "michael.oliver.boyle@gmail.com", "id": "Boyle-Michael", "name": { "family": "Boyle", "given": "Michael" }, "orcid": "0000-0002-5075-5116", "show_email": "YES" } ] }, "title": "Accurate Gravitational Waveforms from Binary Black-hole Systems", "ispublished": "unpub", "full_text_status": "public", "keywords": "gravitational waves; numerical relativity; pseudospectral methods", "abstract": "We examine various topics involved in the creation of accurate theoretical gravitational waveforms from binary black-hole systems.
\r\n\r\nIn Chapter 2 a pseudospectral numerical code is applied to a set of analytic or near-analytic solutions to Einstein's equations which comprise a testbed for numerical-relativity codes. We then discuss methods for extracting gravitational-wave data from numerical simulations of black-hole binary systems, and introduce a practical technique for obtaining the asymptotic form of that data from finite simulation domains in Chapter 3. A formula is also developed to estimate the size of near-field effects from a compact binary. In Chapter 4 the extrapolated data is then compared to post-Newtonian (PN) approximations. We compare the phase and amplitude of the numerical waveform to a collection of Taylor approximants, cross-validating the numerical and PN waveforms, and investigating the regime of validity of the PN waveforms. Chapter 5 extends that comparison to include Pad\u00e9 and effective-one-body models, and investigates components of the PN models. In each case, a careful accounting is made of errors. Finally, we construct a long post-Newtonian\u2013numerical hybrid waveform and evaluate the performance of LIGO's current data-analysis methods with it. We suggest certain optimizations of those methods, including extending the range of template mass ratios to unphysical ranges for certain values of the total mass, and a simple analytic cutoff frequency for the templates which results in nearly optimal matches for both Initial and Advanced LIGO.
\r\n", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-01122009-143851", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01122009-143851", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-02-06", "doi": "10.7907/7NSM-RW43", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "lindblom@tapir.caltech.edu", "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "advisor" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "lindblom@tapir.caltech.edu", "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "chair" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "role": "member" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" }, { "email": "yanbei@caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-01-12", "thesis_defense_date": "2008-10-20", "thesis_approved_date": "2009-02-06", "gradofc_approval_date": "2009-02-05", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"ispublished": "unpub", "full_text_status": "public", "keywords": "albedo; characterization; exoplanets; instrumentation; optical polarimetry", "abstract": "A novel technique for detecting light scattered by extrasolar planets is presented that has the potential to constrain orbital inclination and planet mass. To develop this technique, I have commissioned a high precision polarimeter on the Hale 5-m telescope at Palomar Observatory. The high mass X-ray binary Cygnus X-1 has been observed, which is a proxy for extrasolar planet studies. The single scattering model of Brown et al. (1978), widely used in the literature, predicts an orbital inclination for Cygnus X-1 that is inconsistent with the lack of observed X-ray eclipses to 4\u03c3 - 5\u03c3. Previous studies have hinted at this discrepancy, but data quality was such that the confidence in such a discrepancy was not statistically significant. My observations represent the highest precision study of this object, and they illustrate the overwhelming complexity of the supergiant/black hole system. They also call into question the validity of the Brown et al. (1978) formalism, widely used by the community, for inclination estimation in binary systems.
\r\n\r\nExtrasolar planet host stars have also been observed, and precision of order one part per million has been achieved on bright targets. Precision attained on fainter host stars is of order one part in 10^5 . While scattered light from extrasolar planets has not been conclusively detected, a planetary transit in the HD 189733 system may have been observed in polarized light. Such an event is observed to be 1,000 times weaker in polarized light than in photometry, and it indicates a planetary transit of the Southern Hemisphere of the host star. Such geometric information is difficult to determine by other methods.
\r\n\r\nThe integrated polarization of the debris disk surrounding \u03b3 Ophiuchi has been observed to high precision, and the position angle of net polarization is aligned with the disk major axis as seen by the Spitzer Space Telescope. This indicates the disk is primarily composed of forward scattering dust grains larger than the wavelengths of visible light.
\r\n\r\nFinally, Neptune-mass extrasolar planets orbiting close to their host stars have been modeled to be far too warm for liquid water oceans to exist in their upper atmospheres.
", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-03032009-092300", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03032009-092300", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-05-13", "doi": "10.7907/3YVF-VE44", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-03-03", "thesis_defense_date": "2008-07-28", "thesis_approved_date": "2009-05-13", "gradofc_approval_date": "2009-05-12", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Wiktorowicz, Sloane John" }, { "id": "/id/eprint/4514", "eprint_id": 4514, "rev_number": 13, "documents": [ { "id": "/id/document/7330", "doc_id": 7330, "rev_number": 2, "files": [ { "id": "/id/file/44738", "fileid": 44738, "datasetid": "document", "objectid": 7330, "filename": "stark_thesis.pdf", "mime_type": "application/pdf", "filesize": 9478062, "mtime": "2012-12-26 03:09:22", "url": "/4514/1/stark_thesis.pdf" } ], "eprint_id": 4514, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "stark_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "stark_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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20:24:35", "status_changed": "2009-09-25 03:19:54", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "dps@astro.caltech.edu", "id": "Stark-Daniel-Paul", "name": { "family": "Stark", "given": "Daniel Paul" }, "show_email": "NO" } ] }, "title": "Observing Galaxy Formation in the First Two Billion Years", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmology; Galaxy formation; Gravitational Lensing", "abstract": "The universe evolves dramatically in its first two billion years. From the formation of the first stars and protogalaxies, to the reionization of hydrogen and the assembly of massive 1011 M\u2609 galaxies, this era contains some of the most important events in cosmic history. Current observations of this era are limited causing many of these processes to remain unconstrained. This thesis is comprised of five projects, each of which focuses on advancing the observational study of galaxies in this early era.
\r\n\r\nIn the first three chapters, we seek to constrain the star formation activity at z\u22736-10, concluding that there may be an abundant population of low luminosity galaxies at early times. If verified, this population would likely contribute significantly the ionizing photon budget required for reionization. In Chapter 5, conduct a detailed analysis of the stellar populations of galaxies between z\u22736 and 4, concluding that this period sees a significant increase in the number density of massive, UV luminous galaxies. Finally, in Chapter 6, we present a pilot study utilizing adaptive optics and gravitational lensing to study the resolved kinematics and molecular gas motions of a typical Lyman break galaxy at z~3 with exquisite detail.
\r\n\r\nThese results reveal well-ordered rotation and infer that molecular gas is being efficiently converted into stars in a remarkably compact region, suggesting that we are possibly witnessing the early growth of a disk galaxy where the current star formation is rapidly assembling a central bulge.
\r\n", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-11112008-105159", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-11112008-105159", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-12-19", "doi": "10.7907/Y1AH-J489", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "nzs@radio.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "chair" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "member" }, { "email": "George@Astro.Caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-11-11", "thesis_defense_date": "2008-06-24", "thesis_approved_date": "2008-12-19", "gradofc_approval_date": "2008-12-19", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/13771" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13771" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13771" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/52/12", "datestamp": "2009-06-02", "lastmod": "2023-05-30 22:30:44", "status_changed": "2011-11-07 21:54:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "hilke.schlichting@gmail.com", "id": "Schlichting-Hilke-Elisabeth", "name": { "family": "Schlichting", "given": "Hilke Elisabeth" }, "show_email": "YES" } ] }, "title": "Understanding the Origin of Planetary Systems: Studying the Kuiper Belt and the Dynamics of Planet Formation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Binary Formation; Dynamics; Kuiper Belt; Planet Formation; Planetesimal Accretion; Solar System", "abstract": "This thesis presents theoretical and observational studies pertaining to the early solar system, planet formation and extrasolar planets.
\r\n\r\nFirst, we explore the dynamics of protoplanet formation. We find that the growth of protoplanets may be dominated by the accretion of a planetesimal disk that forms from planetesimal-planetesimal collisions, rather than direct planetesimal impacts onto the protoplanet. This has far reaching implications for the formation of planets, their growth rate and dynamics. We focus on the implications for planetary spins: it can explain the prevalence of prograde spins of planets and asteroids in the solar system, which is commonly believed to be an accident.
\r\n\r\nSecond, we present a series of investigations of the formation of multiple systems in the Kuiper Belt. Two of our studies are concerned with the formation of comparable mass binaries. We find that in a dynamically cold Kuiper Belt, binaries become bound predominantly by dynamical friction. This leads to a binary population with mostly retrograde mutual binary orbits. In a dynamically hot Kuiper Belt three-body gravitational interactions dominate the binary formation producing a roughly equal number of prograde and retrograde binaries. We propose a new formation scenario for Haumea\u2019s collisional family. In our scenario, the family members are ejected while in orbit around Haumea rather than directly from Haumea\u2019s surface as previously proposed. Our formation scenario offers an explanation for the observed velocity dispersion among the family members which is much smaller than Haumea\u2019s escape velocity. It is consistent with detecting just one collisional family in the Kuiper Belt and aids with explaining Haumea\u2019s initial giant impact.
\r\n\r\nWe conclude with observational work that aims to detect sub-km sized Kuiper Belt objects and to measure their size-distribution. Our results provide the best constraint on the surface density of small Kuiper Belt objects to date. Our findings support the idea that small Kuiper Belt objects underwent collisional evolution that modified their size distribution. We present our first candidate occultation event and show that it is unlikely to be due to instrumental artifacts or statistical fluctuations in the data.
", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-05282009-124109", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05282009-124109", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-06-02", "doi": "10.7907/SGJJ-9V78", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "reemsari@gmail.com", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "orcid": "0000-0002-1084-3656", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "co-chair" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "member" }, { "email": "reemsari@gmail.com", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "orcid": "0000-0002-1084-3656", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-05-28", "thesis_defense_date": "2009-05-22", "thesis_approved_date": "2009-06-02", "gradofc_approval_date": "2009-06-01", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Schlichting, Hilke Elisabeth" }, { "id": "/id/eprint/4090", "eprint_id": 4090, "rev_number": 20, "documents": [ { "id": "/id/document/6766", "doc_id": 6766, "rev_number": 4, "files": [ { "id": "/id/file/41008", "fileid": 41008, "datasetid": "document", "objectid": 6766, "filename": "thesisback.pdf", "mime_type": "application/pdf", "filesize": 6452379, "mtime": "2012-12-26 03:05:19", "url": "/4090/1/thesisback.pdf" } ], "eprint_id": 4090, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis", "language": "en", "security": "public", "license": "other", "main": "thesisback.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23298" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23298" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23298" } ] } }, { "id": "/id/document/13862", "doc_id": 13862, "rev_number": 3, "files": [ { "id": "/id/file/204240", "fileid": 204240, "datasetid": "document", "objectid": 13862, "filename": "Li_Chao_2009.PDF", "mime_type": "application/pdf", "filesize": 41679, "mtime": "2016-08-22 21:17:09", "url": "/4090/2/Li_Chao_2009.PDF" } ], "eprint_id": 4090, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Li_Chao_2009.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/23298", "doc_id": 23298, "rev_number": 2, "files": [ { "id": "/id/file/41006", "fileid": 41006, "datasetid": "document", "objectid": 23298, "filename": "preview.png", "mime_type": "image/png", "hash": "9681d8f12276b908374cb7d7ff47722f", "hash_type": "MD5", "filesize": 13074, "mtime": "2012-12-26 03:05:19", "url": "/4090/3/preview.png" } ], "eprint_id": 4090, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "validuser", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6766" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6766" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6766" } ] } }, { "id": "/id/document/123984", "doc_id": 123984, "rev_number": 1, "files": [ { "id": "/id/file/369413", "fileid": 369413, "datasetid": "document", "objectid": 123984, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "85eab764390b3a58e5c7d1ff8d923102", "hash_type": "MD5", "filesize": 36618, "mtime": "2021-06-23 23:12:16", "url": "/4090/4/indexcodes.txt" } ], "eprint_id": 4090, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6766" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6766" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/6766" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/40/90", "datestamp": "2008-11-10", "lastmod": "2020-03-10 23:39:37", "status_changed": "2009-09-25 03:11:17", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "chaosli_8@hotmail.com", "id": "Li-Chao", "name": { "family": "Li", "given": "Chao" }, "show_email": "NO" } ] }, "title": "Topics in Theoretical Astrophysics", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology; gamma ray bursts; gravitational wave astronomy; macroscopic quantum mechanics", "abstract": "This thesis presents a study of various interesting problems in theoretical astrophysics, including gravitational wave astronomy, gamma ray bursts and cosmology. Chapters 2, 3 and 4 explore prospects for detecting gravitational waves from stellar-mass compact objects spiraling into intermediate-mass black holes with ground-based observatories. It is shown in chapter 2 that if the central body is not a BH but its metric is stationary, axisymmetric, reflection symmetric and asymptotically flat, then the waves will likely be triperiodic, as for a BH. Chapters 3 and 4 show that the evolutions of the waves' three fundamental frequencies and of the complex amplitudes of their spectral components encode (in principle) details of the central body's metric, the energy and angular momentum exchange between the central body and the orbit, and the time-evolving orbital elements. Chapter 5 studies a local readout method to enhance the low frequency sensitivity of detuned signal-recycling interferometers. We provide both the results of improvement in quantum noise and the implementation details in Advanced LIGO. Chapter 6 applies and generalizes causal Wiener filter to data analysis in macroscopic quantum mechanical experiments. With the causal Wiener filter method, we demonstrate that in theory we can put the test masses in the interferometer to its quantum mechanical ground states. Chapter 7 presents some analytical solutions for expanding fireballs, the common theoretical model for gamma ray bursts and soft gamma ray repeaters. We apply our results to SGR 1806-20 and rediscover the mismatch between the model and the afterglow observations. Chapter 8 discusses the reconstruction of the scalar-field potential of the dark energy. We advocate direct reconstruction of the scalar field potential as a way to minimize prior assumptions on the shape, and thus minimize the introduction of bias in the derived potential. Chapter 9 discusses gravitational lensing modifications to cosmic microwave background anisotropies and polarization, produced by a stochastic background of primordial gravitational waves between us and the last scattering surface. Chapter 10 calculates the non-Gaussian covariance of CMB B-modes of polarization.\r\n", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-10142008-155140", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10142008-155140", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-10", "doi": "10.7907/CWB8-VF13", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "advisor" }, { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" }, { "email": "asante@tapir.caltech.edu", "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "asante@tapir.caltech.edu", "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "role": "member" }, { "email": "rana@ligo.caltech.edu", "id": "Adhikari-R", "name": { "family": "Adhikari", "given": "Rana" }, "role": "member" }, { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-10-14", "thesis_defense_date": "2008-09-29", "thesis_approved_date": "2008-11-10", "gradofc_approval_date": "2008-11-06", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Li, Chao" }, { "id": "/id/eprint/4146", "eprint_id": 4146, "rev_number": 14, "documents": [ { "id": "/id/document/6845", "doc_id": 6845, "rev_number": 3, "files": [ { "id": "/id/file/41526", "fileid": 41526, "datasetid": "document", "objectid": 6845, "filename": "master.2.pdf", "mime_type": "application/pdf", "filesize": 12864721, "mtime": "2012-12-26 03:05:52", "url": "/4146/1/master.2.pdf" } ], "eprint_id": 4146, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis", "language": "en", "security": "public", "license": "other", "main": "master.2.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23377" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23377" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23377" } ] } }, { "id": "/id/document/13813", "doc_id": 13813, "rev_number": 3, "files": [ { "id": "/id/file/204258", "fileid": 204258, "datasetid": "document", "objectid": 13813, "filename": "Corder_Stuartt_Allan_2009.PDF", "mime_type": "application/pdf", "filesize": 43627, "mtime": "2016-08-22 21:17:11", "url": "/4146/2/Corder_Stuartt_Allan_2009.PDF" } ], "eprint_id": 4146, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Corder_Stuartt_Allan_2009.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/23377", "doc_id": 23377, "rev_number": 2, "files": [ { "id": "/id/file/41524", "fileid": 41524, "datasetid": "document", "objectid": 23377, "filename": "preview.png", "mime_type": "image/png", "hash": "ff0dd3b9ccab31e025230dfe4affd4ef", "hash_type": "MD5", "filesize": 16330, "mtime": "2012-12-26 03:05:52", "url": "/4146/3/preview.png" } ], "eprint_id": 4146, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6845" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6845" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6845" } ] } }, { "id": "/id/document/124024", "doc_id": 124024, "rev_number": 1, "files": [ { "id": "/id/file/369454", "fileid": 369454, "datasetid": "document", "objectid": 124024, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "a903d568d84b97c30b99aadc4752601c", "hash_type": "MD5", "filesize": 38662, "mtime": "2021-06-23 23:14:09", "url": "/4146/4/indexcodes.txt" } ], "eprint_id": 4146, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6845" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6845" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/6845" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/41/46", "datestamp": "2008-12-22", "lastmod": "2019-11-26 20:24:31", "status_changed": "2009-09-25 03:12:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "scorder@nrao.edu", "id": "Corder-Stuartt-Allan", "name": { "family": "Corder", "given": "Stuartt Allan" }, "show_email": "YES" } ] }, "title": "Optimizing Image Fidelity with Arrays", "ispublished": "unpub", "full_text_status": "public", "keywords": "beam size; holography; NGC7538S; voltage patterns", "abstract": "Through simulations, I have investigated the limitations imposed upon the image fidelity of interferometric observations by primary beam errors. Significant antenna surface and pointing errors lead to the greatest reduction in fidelity for most cases, but, when present, imaginary beam components dominate the degradation. Beam errors were addressed by optimizing the antenna surfaces and aligning the optics and then determining baseline based primary beams. Methods for applying these measured patterns to actual data were discussed. Pointing errors were reduced by improving the fit to the pointing model. Further reduction was achieved by integrating the use of optical pointing observations into standard radio observing. The greatest benefit was seen during daytime observations, but general reduction in pointing error was seen.
\r\n\r\nThe dense uv-coverage of the Combined Array for Research in Millimeter-wave Astronomy (CARMA) coupled with the techniques described above make it an ideal instrument for imaging extended regions with high fidelity. The NGC 7538 star-forming cloud contains dense peaks, many high-mass stars and associated accretion disks, and multiple outflows. I obtained CARMA images at the requisite fidelity, employing the above techniques. These mosaiced, spectral-line, and 3-mm band continuum observations provide a clearer picture of the bulk morphology of the region and the fine-scale structures within it than has hitherto been possible. For the first time in the region, infall signatures were found towards two sources, allowing comparison of the infall and outflow mass and verifying that significant accretion (>10\u22124M\u2299 yr\u22121) continues well into the stage where a massive protostar has formed. One of the sources, NGC 7538IRS1, shows one of the few definitive signatures of an inverse PCygni profile towards a massive protostar. Three outflows were found centered on sources that are separated by 10,000-20,000 AU in projection. The calculated energy injection rate provides constraints for models of outflow feedback. The NGC 7538 results demonstrate clearly the capability of CARMA to provide high quality images over wide-fields and the benefits of the techniques I developed. While work to improve CARMA image fidelity continues, the program described here lays the groundwork and should help guide further enhancements of image fidelity at CARMA and at other radio facilities.
\r\n", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-10172008-054754", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10172008-054754", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-12-22", "doi": "10.7907/Q7H2-2P58", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "chair" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "role": "member" }, { "email": "wright@astro.berkeley.edu", "id": "Wright-M", "name": { "family": "Wright", "given": "Melvyn" }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-10-17", "thesis_defense_date": "2008-08-29", "thesis_approved_date": "2008-12-22", "gradofc_approval_date": "2008-12-22", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Corder, Stuartt Allan" }, { "id": "/id/eprint/4187", "eprint_id": 4187, "rev_number": 12, "documents": [ { "id": "/id/document/6887", "doc_id": 6887, "rev_number": 2, "files": [ { "id": "/id/file/41840", "fileid": 41840, "datasetid": "document", "objectid": 6887, "filename": "elina_brobeck_thesis.pdf", "mime_type": "application/pdf", "filesize": 6632848, "mtime": "2012-12-26 03:06:10", "url": "/4187/1/elina_brobeck_thesis.pdf" } ], "eprint_id": 4187, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "elina_brobeck_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "elina_brobeck_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23418" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23418" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23418" } ] } }, { "id": "/id/document/23418", "doc_id": 23418, "rev_number": 2, "files": [ { "id": "/id/file/41838", "fileid": 41838, "datasetid": "document", "objectid": 23418, "filename": "preview.png", "mime_type": "image/png", "hash": "2e1e39747429f9d237cee068155583f9", "hash_type": "MD5", "filesize": 16388, "mtime": "2012-12-26 03:06:10", "url": "/4187/2/preview.png" } ], "eprint_id": 4187, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6887" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6887" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6887" } ] } }, { "id": "/id/document/124043", "doc_id": 124043, "rev_number": 1, "files": [ { "id": "/id/file/369473", "fileid": 369473, "datasetid": "document", "objectid": 124043, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "8dcf90b9a2e31c0453e375cba748e9c0", "hash_type": "MD5", "filesize": 32294, "mtime": "2021-06-23 23:15:43", "url": "/4187/3/indexcodes.txt" } ], "eprint_id": 4187, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6887" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6887" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/6887" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/41/87", "datestamp": "2009-04-27", "lastmod": "2021-11-05 22:56:20", "status_changed": "2009-09-25 03:13:07", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "elina@alum.mit.edu", "id": "Brobeck-Elina", "name": { "family": "Brobeck", "given": "Elina" }, "show_email": "YES" } ] }, "title": "Measurement of Ultra-High Energy Cosmic Rays with CHICOS", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmic rays; UHECRs", "abstract": "The California HIgh school Cosmic ray ObServatory (CHICOS) is a ground-based scintillator array designed to measure the extended air showers of ultra-high energy cosmic rays. The goal of the project is to gain insight into the origin of ultra-high energy cosmic rays by measuring the energy spectrum and the distribution of arrival directions.
\r\n\r\nThe CHICOS array has been in operation since 2003. It consists of 77 pairs of scintillator dectectors deployed at schools in the San Fernando and San Gabriel valleys near Los Angeles, and is designed to observe cosmic ray air showers at energies of 10^18 eV and above. In addition, the Chiquita subarray is designed to observe smaller showers in the energy range of 1016 - 1019 eV.
\r\n\r\nWe present new descriptions of the air shower lateral distribution function and time distribution function, which have been derived from AIRES-generated simulated air showers. The new functions are specific to the CHICOS altitude and allow for a maximum likelihood shower reconstruction method, which is more appropriate to the CHICOS data than the \u03c72 minimization method. We present several analyses of the accuracy of the reconstruction software in the energy ranges available to the Chiquita and CHICOS arrays.
\r\n\r\nThe energy spectrum between 1017 eV and 1019 eV has been measured by the Chiquita subarray. At the lowest energy range, it is found to agree with previous measurements, while the measured flux falls below previous experiments for energies greater than approximately 1017.5 eV. The CHICOS energy spectrum above 1018.4 eV is found to agree with previous results published by AGASA. However, we do not observe the cutoff in the spectrum at 1020 eV reported more recently by the Auger and HiRes Collaborations.
\r\n\r\nA correlation analysis between CHICOS data and nearby active galactic nuclei (AGN) was performed. No excess of cosmic rays was observed in the vicinity of nearby AGN. The maximum correlation was observed for cosmic ray events with E > 1020 eV and for AGN with z < 0.009, with Pchance = 21%. This is consistent with random correlations from an isotropic distribution, a result also found by HiRes, but in disagreement with Auger.
\r\n", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-10192008-143041", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10192008-143041", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0244899" }, { "agency": "NSF", "grant_number": "PHY-0102502" }, { "agency": "Weingart Foundation" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-04-27", "doi": "10.7907/9YH6-N064", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "bmck@krl.caltech.edu", "id": "McKeown-R-D", "name": { "family": "McKeown", "given": "Robert D." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "chair" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" }, { "email": "bmck@krl.caltech.edu", "id": "McKeown-R-D", "name": { "family": "McKeown", "given": "Robert D." }, "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-10-19", "thesis_defense_date": "2008-09-18", "thesis_approved_date": "2009-04-27", "gradofc_approval_date": "2009-04-24", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Brobeck, Elina" }, { "id": "/id/eprint/2746", "eprint_id": 2746, "rev_number": 18, "documents": [ { "id": "/id/document/5057", "doc_id": 5057, "rev_number": 3, "files": [ { "id": "/id/file/29489", "fileid": 29489, "datasetid": "document", "objectid": 5057, "filename": "master.pdf", "mime_type": "application/pdf", "filesize": 5975623, "mtime": "2012-12-26 02:54:03", "url": "/2746/1/master.pdf" } ], "eprint_id": 2746, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "master.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21607" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21607" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21607" } ] } }, { "id": "/id/document/13800", "doc_id": 13800, "rev_number": 3, "files": [ { "id": "/id/file/203796", "fileid": 203796, "datasetid": "document", "objectid": 13800, "filename": "Cenko_Stephen_Bradley_2009.PDF", "mime_type": "application/pdf", "filesize": 42340, "mtime": "2016-08-22 21:16:18", "url": "/2746/2/Cenko_Stephen_Bradley_2009.PDF" } ], "eprint_id": 2746, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Cenko_Stephen_Bradley_2009.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/21607", "doc_id": 21607, "rev_number": 2, "files": [ { "id": "/id/file/29487", "fileid": 29487, "datasetid": "document", "objectid": 21607, "filename": "preview.png", "mime_type": "image/png", "hash": "fe1e8993499b353af6c1107fbd9a8ea0", "hash_type": "MD5", "filesize": 16838, "mtime": "2012-12-26 02:54:03", "url": "/2746/3/preview.png" } ], "eprint_id": 2746, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5057" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5057" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5057" } ] } }, { "id": "/id/document/123136", "doc_id": 123136, "rev_number": 1, "files": [ { "id": "/id/file/368543", "fileid": 368543, "datasetid": "document", "objectid": 123136, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "566552ce8911feeaedf350c66157cb97", "hash_type": "MD5", "filesize": 42382, "mtime": "2021-06-23 22:22:29", "url": "/2746/4/indexcodes.txt" } ], "eprint_id": 2746, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5057" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5057" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5057" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/27/46", "datestamp": "2008-07-30", "lastmod": "2020-03-10 19:27:54", "status_changed": "2009-09-25 02:44:05", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "brad.cenko@nasa.gov", "id": "Cenko-Stephen-Bradley", "name": { "family": "Cenko", "given": "Stephen Bradley" }, "orcid": "0000-0003-1673-970X", "show_email": "NO" } ] }, "title": "The Energetics and Environments of Swift Gamma-Ray Bursts", "ispublished": "unpub", "full_text_status": "public", "keywords": "astrophysics; GRB; Swift gamma-ray bursts", "abstract": "For their short durations, gamma-ray bursts (GRBs) are the most electromagnetically luminous objects in the universe. In this thesis, I uses the fascinating objects, both as signposts, indicating the presence of an ultra-relativistic (Lorentz factor ~ 100-1000) outflow from a newly born stellar mass black hole, and as lighthouses, illuminating the circumburst (r ~ 1 pc) and inter-stellar (r ~ 1 kpc) media along the line of sight.
\r\n\r\nIn Part I, I describe my efforts to automate the Palomar 60 inch telescope (P60), the primary instrument on which much of this thesis is based. Designed to capitalize on NASA's recently launched Swift Gamma-Ray Burst Explorer, P60 now routinely provides moderately fast (t <~ 3 min) and sustained (R <~ 23 mag) observations of GRB afterglows and other optical transients.
\r\n\r\nPart II focuses on the geometry and energetics of some of the best-sampled events in the Swift era. I find both GRB050820A and GRB060418 are an order of magnitude more energetic than pre-Swift events, with a total energy release in excess of 10^52 erg. Both GRBs are therefore members of an emerging class of \"hyper-energetic\" GRBs, suggesting a much broader energy distribution than previously thought and challenging current massive star progenitor models.
\r\n\r\nFinally, in Part III I study the environments of long-duration GRBs. The massive star progenitors should leave an imprint on the GRB environment, both on the pc scale as a wind from mass loss of the outer envelope, and on the kpc scale from the dense, dusty disk where massive stars form. Interestingly, I demonstrate that GRB070125 exploded in a halo environment, suggesting at least some massive stars form far away from the disk of their host. By comparing the X-ray and optical light curves from a sample of 29 GRBs, I find nearly half show evidence for suppressed optical emission. I attribute this to dust absorption in the host galaxy, consistent with a massive star origin for long-duration GRBs.
", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-06272008-153145", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06272008-153145", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-07-30", "doi": "10.7907/SNRD-BR66", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "advisor" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "chair" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-06-27", "thesis_defense_date": "2008-06-04", "thesis_approved_date": "2008-07-30", "gradofc_approval_date": "2008-07-22", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Cenko, Stephen Bradley" }, { "id": "/id/eprint/3016", "eprint_id": 3016, "rev_number": 19, "documents": [ { "id": "/id/document/5405", "doc_id": 5405, "rev_number": 3, "files": [ { "id": "/id/file/203956", "fileid": 203956, "datasetid": "document", "objectid": 5405, "filename": "law_citthesis.pdf", "mime_type": "application/pdf", "filesize": 5468960, "mtime": "2016-08-22 21:16:28", "url": "/3016/1/law_citthesis.pdf" } ], "eprint_id": 3016, "pos": 1, "format": "application/pdf", "format_desc": "law_citthesis.pdf", "language": "en", "security": "internal", "license": "other", "main": "law_citthesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5406" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5406" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5406" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/30/16", "datestamp": "2008-08-13", "lastmod": "2021-11-05 22:56:49", "status_changed": "2009-09-25 02:49:44", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "dlaw@stsci.edu", "id": "Law-David-Richard-Astrophysics", "name": { "family": "Law", "given": "David Richard" }, "orcid": "0000-0002-9402-186X", "show_email": "NO" } ] }, "title": "The Kiloparsec-Scale Structure and Kinematics of High-Redshift Star-Forming Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: kinematics & dynamics; galaxies: structure", "abstract": "We study the spatially resolved properties of star-forming galaxies at redshift z ~ 2 - 3 on scales ~ 1 kpc using a combination of morphological and kinematic analyses in an effort to characterize the major mechanisms of galaxy formation in the young universe. Using a sample of 216 galaxies which have been spectroscopically confirmed to lie between redshifts z = 1.8 - 3.4 in the GOODS-N field we demonstrate that rest-UV morphology (as seen by the Hubble Space Telescope) is statistically uncorrelated with physical properties such as star formation rate and is therefore unable to support the hypothesis that the prevalence of irregular morphologies indicates a high major merger fraction. Further, we present a sample of 13 galaxies observed with the OSIRIS integral field spectrograph and the Keck laser-guide star adaptive optics system which demonstrate the prevalence of high velocity dispersions ~ 80 km/s and generally little in the way of spatially resolved velocity gradients, inconsistent with favored rotating disk models. We discuss the implications of these results for galaxy formation models, including gas accretion via cold flows and gravitational instability of early gas-rich galactic disks. There is some evidence for a trend towards stronger rotational signatures in galaxies with more massive stellar populations. ", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-08042008-124002", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08042008-124002", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-08-13", "doi": "10.7907/QNV4-9V14", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "chair" }, { "email": "abenson@its.caltech.edu", "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew J." }, "orcid": "0000-0001-5501-6008", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-04", "thesis_defense_date": "2008-07-30", "thesis_approved_date": "2008-08-13", "gradofc_approval_date": "2008-08-11", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"2008-10-21", "lastmod": "2019-11-26 20:24:24", "status_changed": "2009-09-25 02:58:35", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kmd@astro.ufrj.br", "id": "Men\u00e9ndez-Delmestre-Kar\u00edn", "name": { "family": "Men\u00e9ndez-Delmestre", "given": "Kar\u00edn" }, "orcid": "0000-0003-3153-5123", "show_email": "NO" } ] }, "title": "The Luminous, the Massive and the Dusty: A Near- to Mid-Infrared Spectroscopic Study of Submillimeter Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "high-redshift galaxies; Keck NIRSPEC; Keck OSIRIS; Spitzer IRS; submillimeter galaxies", "abstract": "Submillimeter (submm) surveys have uncovered a population of dust-enshrouded ultra-luminous galaxies that are inconspicuous in deep surveys at shorter wavelengths. Inferred to have high star-formation rates (up to more than 1000 Msun/yr), submm-selected galaxies (SMGs) contribute significantly to the global star-formation rate density at z~2-3 and are thus critical players in building up stars in galaxies. Many SMGs have been shown to display X-ray, optical and near-infrared (IR) signatures of active galactic nuclei (AGN), prompting the question: how significant is the AGN contribution to their total luminosity? Central to understanding SMGs is the study of the nature of their power source, their internal dynamics, their SFRs and their masses. We study mid-IR and near-IR spectra of SMGs to investigate these aspects.
\r\n\r\nWe have obtained the largest sample of 24 SMGs to date with the mid-IR Spitzer Infrared Spectrograph (IRS) at z ~ 0.65 - 3.2. Broad PAH emission features -- typically associated to intense star-formation -- are almost ubiquitous in the sample and the composite spectrum is well fit by a combination of a starburst component with an additional power law representing less than a 35% AGN contribution to the bolometric luminosity. We find weak silicate absorption in contrast to local ultra-luminous IR galaxies (ULIRGs), suggesting that the mid-IR visible star formation in SMGs occurs in a more extended component.
\r\n\r\nWe also study the near-IR emission of SMGs with the OH-Suppressing Infrared Imaging Spectrograph (OSIRIS), together with the Keck Laser-Guide Star Adaptive Optics system, to investigate the distribution and dynamics of the ionized gas. The two-dimensional insight of these observations allow us to distinguish and quantify the compact AGN emission, which allows us to refine estimates of dynamical masses, SFRs and gas masses for the population. With a spatially-resolved spectroscopic insight into the kpc-scale structure of these galaxies, we find that the H-alpha emission in SMGs extends over scales ~4-17 kpc, setting SMGs apart from local ULIRGs, where intense emission is confined to the central 1 kpc.
\r\n", "date": "2009", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-170617", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-170617", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-21", "doi": "10.7907/J1R4-5F20", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "chair" }, { "email": "abenson@caltech.edu", "id": "Benson-A-J", "name": { "family": "Benson", "given": "Andrew J." }, "role": "member" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "member" }, { "email": "lee@ipac.caltech.edu", "id": "Armus-L", "name": { "family": "Armus", "given": "Lee" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "2008-08-26", "thesis_approved_date": "2008-10-21", "gradofc_approval_date": "2008-10-08", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2009", "author_list": "Men\u00e9ndez-Delmestre, Kar\u00edn" }, { "id": "/id/eprint/1428", "eprint_id": 1428, "rev_number": 17, "documents": [ { "id": "/id/document/2165", "doc_id": 2165, "rev_number": 2, "eprint_id": 1428, "pos": 1, "format": "application/pdf", "format_desc": "chen2008thesis-astron.bib", "language": "en", "security": "internal", "license": "other", "main": "chen2008thesis-astron.bib", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/2166", "doc_id": 2166, "rev_number": 2, "eprint_id": 1428, "pos": 2, "format": "application/pdf", "format_desc": "chen2008thesis-engine.bib", "language": "en", "security": "internal", "license": "other", "main": "chen2008thesis-engine.bib", "media_duration": "0", "media_aspect_ratio": "0", 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"family": "Chen", "given": "Chi Ming Hubert" }, "show_email": "NO" } ] }, "title": "Development of Hard X-ray Imaging Detectors for the High Energy Focusing Telescope", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cadmium zinc telluride radiation detectors; Galaxies magnetic fields; Radiation detector circuits; Radiation mechanisms inverse Compton scattering", "abstract": "The High Energy Focusing Telescope (HEFT) is a balloon-borne instrument carrying one of the first focusing telescopes for the hard X-ray band (20\u201370 keV). It makes use of tungsten-silicon multilayer coatings to extend the reflectivity of nested grazing-incidence mirrors beyond 10 keV. It also carries novel semiconductor pixel detectors on its focal planes to match the capabilities of the multilayer mirrors. After a decade of research and development, we achieve with HEFT an angular resolution of 1.5 arcminutes in half-power diameter, and an energy resolution of 1.0 keV full width at half maximum at 60 keV. We launched HEFT for a 25-hour balloon flight in May, 2005; the instrument performed within specification, and observed Cyg X-1, the Crab Nebula, and other celestial hard X-ray sources.
\r\n\r\nIn this thesis, I lay out the scientific motivations for HEFT, and give an overview of the experiment. I report on our detector development effort in depth, and document the balloon flight of 2005. I also describe a study of two relic radio sources, 0917+75 and 1401\u221233, with data from the soft X-ray XMM-Newton observatory. With a hard X-ray focusing telescope like HEFT, one can improve the sensitivity and extend the scope of such studies to other classes of objects.
\r\n", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-04202008-135222", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04202008-135222", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-20", "doi": "10.7907/A2DS-N675", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "chair" }, { "email": "brad@krl.caltech.edu", "id": "Filippone-B-W", "name": { "family": "Filippone", "given": "Bradley W." }, "role": "member" }, { "email": "jonas@submm.caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-04-20", "thesis_defense_date": "2008-01-10", "thesis_approved_date": "2008-05-20", "gradofc_approval_date": "2008-05-19", "thesis_awards": "Everhart Distinguished Graduate Student Lecturer Award, 2008.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Chen, Chi Ming Hubert" }, { "id": "/id/eprint/1782", "eprint_id": 1782, "rev_number": 14, "documents": [ { "id": "/id/document/2903", "doc_id": 2903, "rev_number": 2, "files": [ { "id": "/id/file/17660", "fileid": 17660, "datasetid": "document", "objectid": 2903, "filename": "cit_thesis.pdf", "mime_type": "application/pdf", "filesize": 3931142, "mtime": "2012-12-26 02:41:59", "url": "/1782/1/cit_thesis.pdf" } ], "eprint_id": 1782, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "cit_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "cit_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19626" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19626" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19626" } ] } }, { "id": "/id/document/16458", "doc_id": 16458, "rev_number": 3, "files": [ { "id": "/id/file/201721", "fileid": 201721, "datasetid": "document", "objectid": 16458, "filename": "Schaller_Emily_Lauren_2008.PDF", "mime_type": "application/pdf", "filesize": 45783, "mtime": "2016-08-22 21:15:06", "url": "/1782/2/Schaller_Emily_Lauren_2008.PDF" } ], "eprint_id": 1782, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Schaller_Emily_Lauren_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/19626", "doc_id": 19626, "rev_number": 2, "files": [ { "id": "/id/file/17658", "fileid": 17658, "datasetid": "document", "objectid": 19626, "filename": "preview.png", "mime_type": "image/png", "hash": "04bd69a3974f6776673323e8c206d2ce", "hash_type": "MD5", "filesize": 16184, "mtime": "2012-12-26 02:41:59", "url": "/1782/3/preview.png" } ], "eprint_id": 1782, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2903" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2903" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2903" } ] } }, { "id": "/id/document/121246", "doc_id": 121246, "rev_number": 1, "files": [ { "id": "/id/file/366638", "fileid": 366638, "datasetid": "document", "objectid": 121246, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "f07f6f2d8ba6e429a015497f4b436b75", "hash_type": "MD5", "filesize": 22253, "mtime": "2021-06-23 21:21:13", "url": "/1782/4/indexcodes.txt" } ], "eprint_id": 1782, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2903" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2903" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2903" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/82", "datestamp": "2008-05-22", "lastmod": "2020-03-04 21:57:23", "status_changed": "2009-09-25 02:15:14", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "e.schaller@baeri.org", "id": "Schaller-Emily-Lauren", "name": { "family": "Schaller", "given": "Emily Lauren" }, "show_email": "YES" } ] }, "title": "I. Seasonal Changes in Titan\u2019s Cloud Activity. II. Volatile Ices on Outer Solar System Objects", "ispublished": "unpub", "full_text_status": "public", "keywords": "meteorology; Titan; transneptunian objects", "abstract": "This thesis presents studies in two distinct areas of observational planetary astronomy: studies of Saturn's moon Titan's seasonally varying tropospheric clouds, and studies of the surface compositions of Kuiper belt objects.
\r\n\r\nI. Understanding Titan's methane-based hydrological cycle and interpreting how and when the fluvial surface features seen by the Cassini Spacecraft were formed requires frequent long-term observations of Titan's clouds. Using nearly 100 adaptive optics images from the Keck and Gemini Telescopes from 2002-2006, we mapped the locations, frequencies, and magnitudes of Titan's clouds. We also developed a near-nightly cloud-monitoring program with the NASA Infrared Telescope Facility (IRTF). Nightly whole-disk infrared spectroscopy with IRTF allows us to determine Titan's total fractional cloud coverage, magnitudes, and altitudes, complementing and providing context for the relatively infrequent Cassini flybys. Taken together, the observations presented in this thesis have shown a striking seasonal change in the behavior of Titan's clouds as Titan has moved from southern summer solstice (October 2002) toward vernal equinox (August 2009) and indicate that seasonally varying insolation appears, to first order, to control Titan's cloud locations (Schaller et al. 2006a & 2006b).
\r\n\r\nII. Unlike Pluto and Eris, the vast majority of Kuiper belt objects (KBOs) are too small and too hot to retain volatile ices like CH4, N2, and CO on their surfaces to the present day. As a result, their infrared spectra are either dominated by involatile water ice or dark spectrally featureless material. To understand the dichotomy between volatile-rich and volatile-free surfaces in the outer solar system, we constructed a model of atmospheric escape of volatile ices over the age of the solar system (Schaller & Brown 2007a). We predicted that Quaoar, an object about half the size of Pluto, should be just capable of retaining methane ice to the present day. We observed Quaoar with the Keck Telescope, used Hapke theory to model its spectrum, and found that it contains a small amount of methane on its surface, indicating that it is a transition object between the dominant volatile-poor small KBOs and the few volatile-rich KBOs such as Pluto and Eris (Schaller & Brown 2007b).
", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-05132008-173841", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05132008-173841", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-22", "doi": "10.7907/YXFP-V230", "alt_title": { "items": [ "Volatile Ices on Outer Solar System Objects" ] }, "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-13", "thesis_defense_date": "2008-04-28", "thesis_approved_date": "2008-05-22", "gradofc_approval_date": "2008-05-21", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Schaller, Emily Lauren" }, { "id": "/id/eprint/1663", "eprint_id": 1663, "rev_number": 11, "documents": [ { "id": "/id/document/2640", "doc_id": 2640, "rev_number": 2, "files": [ { "id": "/id/file/16202", "fileid": 16202, "datasetid": "document", "objectid": 2640, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 7671079, "mtime": "2012-12-26 02:40:30", "url": "/1663/1/thesis.pdf" } ], "eprint_id": 1663, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19379" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19379" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19379" } ] } }, { "id": "/id/document/16133", "doc_id": 16133, "rev_number": 3, "files": [ { "id": "/id/file/201600", "fileid": 201600, "datasetid": "document", "objectid": 16133, "filename": "Kumar_Shwetank_2008.PDF", "mime_type": "application/pdf", "filesize": 44176, "mtime": "2016-08-22 21:15:01", "url": "/1663/2/Kumar_Shwetank_2008.PDF" } ], "eprint_id": 1663, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Kumar_Shwetank_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/19379", "doc_id": 19379, "rev_number": 2, "files": [ { "id": "/id/file/16200", "fileid": 16200, "datasetid": "document", "objectid": 19379, "filename": "preview.png", "mime_type": "image/png", "hash": "960908a030774dac56c0a5b82c0b0da8", "hash_type": "MD5", "filesize": 17315, "mtime": "2012-12-26 02:40:30", "url": "/1663/3/preview.png" } ], "eprint_id": 1663, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2640" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2640" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2640" } ] } }, { "id": "/id/document/121049", "doc_id": 121049, "rev_number": 1, "files": [ { "id": "/id/file/366438", "fileid": 366438, "datasetid": "document", "objectid": 121049, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "f656e348024382e69d0628a23d8faee1", "hash_type": "MD5", "filesize": 24750, "mtime": "2021-06-23 21:14:52", "url": "/1663/4/indexcodes.txt" } ], "eprint_id": 1663, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2640" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2640" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2640" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/16/63", "datestamp": "2008-05-20", "lastmod": "2020-03-10 23:27:56", "status_changed": "2009-09-25 02:11:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "shwetank.kumar@gmail.com", "id": "Kumar-Shwetank", "name": { "family": "Kumar", "given": "Shwetank" }, "show_email": "YES" } ] }, "title": "Submillimeter Wave Camera Using A Novel Photon Detector Technology", "ispublished": "unpub", "full_text_status": "public", "keywords": "bandpass filters; superconducting resonators", "abstract": "Cryogenic photon detectors can be used to make extremely sensitive cameras for submillimeter astronomy. Current detector technologies already have sensitivities limited by the noise due to photon arrival statistics. To further improve the sensitivity and mapping speed of experiments for a wide field survey, focal planes containing tens of thousands of pixels are required. Unfortunately, the current technologies use discrete and massive components which are not easy to integrate into large arrays. This thesis presents a 16-pixel, two-color, submillimeter-wave, prototype camera developed at Caltech and the Jet Propulsion Laboratory using a novel photon detector technology. The camera also uses new designs for other constituent elements \u2013 the antenna, transmission line feednetwork, and bandpass filters \u2013 to implement the sub-millimeter pixels. These designs allow integration of the entire camera onto a single chip and conclusively address the problem of scalability while maintaining the sensitivity and noise performance of the current technologies. This thesis explains the design of each of these components and presents the results from experiments conducted to test their performance. Results from the 'first light', obtained by mounting the prototype camera onto the Caltech Submillimeter Observatory (CSO), are also presented.
\r\n\r\nWe have also studied the temperature and power dependence of the resonance frequency, quality factor, and frequency noise of the superconducting niobium thin-film coplanar waveguide (CPW) resonators in order to understand the factors affecting the noise performance of our photon detectors. These experiments were carried out at temperatures well below the superconducting transition (Tc = 9.2 K) in an attempt to understand the source of the excess frequency noise of superconducting resonators which form the sensing element of our photon detectors. The noise decreases by nearly two orders of magnitude as the temperature is increased from 120 to 1200 mK, while the variation of the resonance frequency with temperature over this range agrees well with the standard two-level systems (TLS) model for amorphous dielectrics. These results support the hypothesis that TLS are responsible for the noise in superconducting microresonators and have important implications for resonator applications such as qubits and photon detectors.
\r\n", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-05072008-075138", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05072008-075138", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-20", "doi": "10.7907/F58T-SV45", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "rutledge@caltech.edu", "id": "Rutledge-D-B", "name": { "family": "Rutledge", "given": "David B." }, "role": "chair" }, { "email": "etcher@caltech.edu", "id": "Scherer-A", "name": { "family": "Scherer", "given": "Axel" }, "role": "member" }, { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" }, { "email": "mwb@caltech.edu", "id": "Bockrath-M-W", "name": { "family": "Bockrath", "given": "Marc William" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-07", "thesis_defense_date": "2007-12-13", "thesis_approved_date": "2008-05-20", "gradofc_approval_date": "2008-05-19", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Kumar, Shwetank" }, { "id": "/id/eprint/324", "eprint_id": 324, "rev_number": 13, "documents": [ { "id": "/id/document/483", "doc_id": 483, "rev_number": 3, "files": [ { "id": "/id/file/3083", "fileid": 3083, "datasetid": "document", "objectid": 483, "filename": "final_thesis_version_jan24.pdf", "mime_type": "application/pdf", "filesize": 4390861, "mtime": "2012-12-26 02:28:55", "url": "/324/1/final_thesis_version_jan24.pdf" } ], "eprint_id": 324, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Full thesis", "language": "en", "security": "public", "license": "other", "main": "final_thesis_version_jan24.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17309" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17309" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17309" } ] } }, { "id": "/id/document/16012", "doc_id": 16012, "rev_number": 3, "files": [ { "id": "/id/file/199995", "fileid": 199995, "datasetid": "document", "objectid": 16012, "filename": "Hainline_Laura_Jeannine_2008.PDF", "mime_type": "application/pdf", "filesize": 44598, "mtime": "2016-08-22 21:14:00", "url": "/324/2/Hainline_Laura_Jeannine_2008.PDF" } ], "eprint_id": 324, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Hainline_Laura_Jeannine_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/17309", "doc_id": 17309, "rev_number": 2, "files": [ { "id": "/id/file/3081", "fileid": 3081, "datasetid": "document", "objectid": 17309, "filename": "preview.png", "mime_type": "image/png", "hash": "5bd329078990de1d12360d68baf51fc3", "hash_type": "MD5", "filesize": 15105, "mtime": "2012-12-26 02:28:55", "url": "/324/3/preview.png" } ], "eprint_id": 324, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/483" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/483" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/483" } ] } }, { "id": "/id/document/119829", "doc_id": 119829, "rev_number": 1, "files": [ { "id": "/id/file/365198", "fileid": 365198, "datasetid": "document", "objectid": 119829, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "fd45d70345a9848d5943cf5769d0acbc", "hash_type": "MD5", "filesize": 30421, "mtime": "2021-06-23 20:22:08", "url": "/324/4/indexcodes.txt" } ], "eprint_id": 324, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/483" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/483" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/483" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/03/24", "datestamp": "2008-02-21", "lastmod": "2019-12-03 22:30:59", "status_changed": "2009-09-25 01:34:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ljh@astro.caltech.edu", "id": "Hainline-Laura-Jeannine", "name": { "family": "Hainline", "given": "Laura Jeannine" } } ] }, "title": "Multi-Wavelength Properties of Submillimeter-Selected Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxies; galaxy formation; high redshift", "abstract": "The resolution of the cosmic far-infrared background at long wavelengths has uncovered a population of high-redshift, highly infrared-luminous galaxies that indicate that a significant amount of highly obscured star formation occurred in the early history of the Universe, which has not been taken into account in studies of the cosmic star formation and mass assembly histories. Since such studies are important tests of hierarchical galaxy formation models in a cold dark matter- dominated universe, it is vital that the contribution of these luminous submillimeter-selected galaxies to the buildup of stellar mass in the Universe be understood and included when testing galaxy formation models. Progress in understanding the nature of submillimeter-selected galaxies has been slow, however, due to the faintness of the population outside of the submillimeter bands and the coarse resolution of the single-dish submillimeter surveys in which the galaxies were discovered. The slow progress has at least two important consequences: (1) there is still much that is unknown about submillimeterselected galaxies at all wavelengths, so the properties of and evolutionary predictions for the population are often inferred by making analogies to local galaxies of similar luminosity and assuming the high-redshift galaxies represent a uniform population of galaxies; and (2) the relationships of the submillimeter-selected galaxies to other high-redshift galaxy populations selected at other wavelengths remain poorly understood.
\r\n\r\nIn this work we capitalize on recently-available observing resources of the Spitzer Space Telescope, at near- and mid-infrared wavelengths, and the Green Bank Telescope, at 1 cm, to improve the characterization of the largest representative sample of submillimeter-selected galaxies with spectroscopic redshifts. We combine our new data with data from the literature at a variety of wavelengths to place new constraints on the fundamental properties of gas mass, stellar mass, infrared luminosity, and spectral energy distribution, and use our new constraints to test a variety of assumptions which have been used in the past to predict and infer characteristics of submillimeter-selected galaxies. We also use our new data to compare different populations of high-redshift galaxies selected at different wavelengths in an effort to understand the relationships between the different types of galaxies.
\r\n\r\nFirst, we use observations of CO rotational line emission with the Green Bank Telescope to constrain the cold gas mass and gas conditions in several submillimeter-selected galaxies. We obtain the first detection of CO(1\u21920) emission from a submillimeter-selected galaxy, finding that the CO(4\u21923)/CO(1\u21920) brightness temperature ratio of ~ 0.26 suggests n(H\u2082) > 3 \u2212 10 \u00d7 10\u00b2 cm\u207b\u00b3 and the presence of sub-thermally excited gas. The integrated line flux implies a cold molecular gas mass 4 times larger than the mass predicted from the CO(4\u21923) line, assuming a brightness temperature ratio of 1.0, suggesting that extrapolating molecular gas masses from J upper \u2265 3 transitions of CO, which is the primary method of estimating molecular gas masses of high-z galaxies in the literature, leads to considerable uncertainties.
\r\n\r\nNext, we use deep imaging with the Multiband Imaging Photometer for Spitzer (MIPS) on the Spitzer Space Telescope of the spectroscopic sample of radio-detected submillimeter-selected galaxies of Chapman et al. (2005) to derive new estimates of the infrared luminosity for these objects. Our Spitzer data constrain the Wien side of the infrared spectral energy distribution peak of high-redshift submillimeter-selected galaxies, and thus are extremely important to determine the contribution of hot dust emission to the total infrared luminosity. We find that most submillimeter-selected galaxies do not have dominant contributions from hot dust at rest-frame mid-infrared wavelengths. We also find that the spectral energy distribution of the nearest ultraluminous infrared galaxy, Arp 220, is significantly different on average from most high-z submillimeter-selected galaxies and is thus a poor template with which to predict properties of submillimeter-selected galaxies even though it has been often used in the past. Using our new infrared luminosity estimates constrained by multiple infrared and submillimeter data points, we show that submillimeter-selected galaxies display a relatively tight, almost linear correlation between total infrared luminosity and radio luminosity, which is not largely different from the far-infrared\u2013radio correlation of local galaxies selected by the Infrared Astronomical Satellite (IRAS).
\r\n\r\nWe examine the rest-frame ultraviolet through near-infrared spectral energy distributions of the same sample of radio-detected submillimeter-selected galaxies with spectroscopic redshifts, obtained using measurements from imaging with the Infrared Array Camera (IRAC) on Spitzer in combination with observed-frame optical and near-infrared data from the literature. We find from these spectral energy distributions, which trace the stellar light from a galaxy in the absence of an active nucleus, that submillimeter-selected galaxies suffer significant extinction at rest-frame optical wavelengths, and that both stars and dust emission contribute to the near-infrared luminosity in many z > 2 submillimeter-selected galaxies. We estimate stellar masses for the individual galaxies in the sample using restframe H-band luminosities interpolated from the observed spectral energy distributions, obtaining a median stellar mass for the sample of 6 \u2212 7 \u00d7 10\u00b9\u2070 Msun. By comparing our stellar mass estimates to molecular gas and dynamical mass estimates for 13 individual submillimeter-selected galaxies in our sample observed in CO emission lines, we determine that the molecular gas fraction in submillimeter-selected galaxies declines with increasing stellar mass, which is suggestive of an evolutionary trend. If the molecular gas masses for the 13 galaxies for which gas mass estimates are available are typical of the entire radiodetected submillimeter-selected galaxy population, then a typical lower limit to the total baryonic mass of submillimeter-selected galaxies is ~ 10\u00b9\u00b9 Msun, and these galaxies are unlikely to significantly increase their stellar mass in the current epoch of activity which is the source of their enormous infrared luminosity.
\r\n\r\nLastly, we compare the IRAC and MIPS properties of submillimeter-selected galaxies and their stellar masses to those of high-redshift ultraviolet- and optically-selected galaxies, 24 \u03bcm-selected galaxies, and powerful radio galaxies. In the IRAC bands, submillimeter-selected galaxies are brighter and redder than ultraviolet-selected galaxies, suggesting they have higher dust content, higher stellar mass, a higher contribution from an active nucleus, or some combination of these factors. The near-infrared colors of submillimeterselected galaxies are most similar to those of high-z radio galaxies, objects which are known to contain powerful, obscured active nuclei. However, submillimeter-selected galaxies are fainter in the MIPS 24 \u03bcm band than high-z radio galaxies, suggesting that the dust in the submillimeter-selected galaxies is not heated to such high temperatures as in the radio sources. We find that the typical stellar mass of submillimeter-selected galaxies is larger by a factor of 3\u20134 than that of high-redshift ultraviolet-selected galaxies, roughly similar to the typical stellar mass of optically-selected high-z galaxies, and lower than the typical stellar mass of powerful high-z radio galaxies. These comparisons suggest that submillimeter-selected galaxies are among the more massive galaxies of their epoch, but not necessarily the most massive, as has been suggested in the literature. However, systematic errors in the stellar masses of any of the high-redshift galaxy samples of a factor of a few, which are certainly possible, can alter this conclusion.
", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-01242008-093655", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01242008-093655", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-02-21", "doi": "10.7907/Q4DB-K461", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-01-24", "thesis_defense_date": "2007-11-02", "thesis_approved_date": "2008-02-21", "gradofc_approval_date": "2008-02-01", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Hainline, Laura Jeannine" }, { "id": "/id/eprint/5055", "eprint_id": 5055, "rev_number": 20, "documents": [ { "id": "/id/document/8012", "doc_id": 8012, "rev_number": 3, "files": [ { "id": "/id/file/49317", "fileid": 49317, "datasetid": "document", "objectid": 8012, "filename": "jmb_thesis.pdf", "mime_type": "application/pdf", "filesize": 4892114, "mtime": "2012-12-26 03:14:19", "url": "/5055/1/jmb_thesis.pdf" } ], "eprint_id": 5055, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "jmb_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "jmb_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/24522" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/24522" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/24522" } ] } }, { "id": "/id/document/15733", "doc_id": 15733, "rev_number": 3, "files": [ { "id": "/id/file/204495", "fileid": 204495, "datasetid": "document", "objectid": 15733, "filename": "Brown_Joanna_Margaret_2008.PDF", "mime_type": "application/pdf", "filesize": 43645, "mtime": "2016-08-22 21:17:43", "url": "/5055/2/Brown_Joanna_Margaret_2008.PDF" } ], "eprint_id": 5055, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Brown_Joanna_Margaret_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/24522", "doc_id": 24522, "rev_number": 2, "files": [ { "id": "/id/file/49315", "fileid": 49315, "datasetid": "document", "objectid": 24522, "filename": "preview.png", "mime_type": "image/png", "hash": "036c79b0773f16e404b246626fd4297c", "hash_type": "MD5", "filesize": 15130, "mtime": "2012-12-26 03:14:19", "url": "/5055/3/preview.png" } ], "eprint_id": 5055, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "validuser", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/8012" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/8012" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/8012" } ] } }, { "id": "/id/document/124713", "doc_id": 124713, "rev_number": 1, "files": [ { "id": "/id/file/370143", "fileid": 370143, "datasetid": "document", "objectid": 124713, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "54ed3aee2b8361aa79cd2c4fa080458b", "hash_type": "MD5", "filesize": 24369, "mtime": "2021-06-23 23:51:12", "url": "/5055/4/indexcodes.txt" } ], "eprint_id": 5055, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/8012" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/8012" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/8012" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/50/55", "datestamp": "2008-01-15", "lastmod": "2023-11-08 00:16:43", "status_changed": "2009-09-25 03:31:47", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "joannabrown@cfa.harvard.edu", "id": "Brown-Joanna-Margaret", "name": { "family": "Brown", "given": "Joanna Margaret" }, "show_email": "NO" } ] }, "title": "Childhood to Adolescence: Dust and Gas Clearing in Protoplanetary Disks", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy; planet formation; star formation", "abstract": "Disks are ubiquitous around young stars. Over time, disks dissipate, revealing planets that formed hidden by their natal dust. Since direct detection of young planets at small orbital radii is currently impossible, other tracers of planet formation must be found. One sign of disk evolution, potentially linked to planet formation, is the opening of a gap or inner hole in the disk. In this thesis, I have identified and characterized several cold disks with large inner gaps but retaining massive primordial outer disks. While cold disks are not common, with ~5% of disks showing signs of inner gaps, they provide proof that at least some disks evolve from the inside-out. These large gaps are equivalent to dust clearing from inside the Earth's orbit to Neptune's orbit or even the inner Kuiper belt. Unlike more evolved systems like our own, the central star is often still accreting and a large outer disk remains.
\r\n\r\nI identified four cold disks in Spitzer 5-40 \u00b5m spectra and modeled these disks using a 2-D radiative transfer code to determine the gap properties. Outer gap radii of 20-45 AU were derived. However, spectrophotometric identification is indirect and model-dependent. To validate this interpretation, I observed three disks with a submillimeter interferometer and obtained the first direct images of the central holes. The images agree well with the gap sizes derived from the spectrophotometry. One system, LkH&alpha 330, has a very steep outer gap edge which seems more consistent with gravitational perturbation rather than gradual processes, such as grain growth and settling. Roughly 70% of cold disks show CO v=1&rarr 0 gas emission from the inner 1 AU and therefore are unlikely to have evolved due to photoevaporation. The derived rotation temperatures are significantly lower for the cold disks than disks without gaps. Unresolved (sub)millimeter photometry shows that cold disks have steeper colors, indicating that they are optically thin at these wavelengths, unlike their classical T Tauri star counterparts. The gaps are cleared of most ~100 \u00b5m sized grains as well as the ~10 \u00b5m sized grains visible in the mid-infrared as silicate emission features.
\r\n", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-12182007-120046", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-12182007-120046", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-01-15", "doi": "10.7907/560K-TZ76", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "co-chair" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-12-18", "thesis_defense_date": "2007-11-19", "thesis_approved_date": "2008-01-15", "gradofc_approval_date": "2008-01-14", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Brown, Joanna Margaret" }, { "id": "/id/eprint/3237", "eprint_id": 3237, "rev_number": 11, "documents": [ { "id": "/id/document/5738", "doc_id": 5738, "rev_number": 3, "files": [ { "id": "/id/file/33968", "fileid": 33968, "datasetid": "document", "objectid": 5738, "filename": "DetectionAndExploration.pdf", "mime_type": "application/pdf", "filesize": 4999008, "mtime": "2012-12-26 02:58:24", "url": "/3237/1/DetectionAndExploration.pdf" } ], "eprint_id": 3237, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Full thesis", "language": "en", "security": "public", "license": "other", "main": "DetectionAndExploration.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22280" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22280" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22280" } ] } }, { "id": "/id/document/16339", "doc_id": 16339, "rev_number": 3, "files": [ { "id": "/id/file/204031", "fileid": 204031, "datasetid": "document", "objectid": 16339, "filename": "O'Donovan_Francis_Thomas_2008.PDF", "mime_type": "application/pdf", "filesize": 43507, "mtime": "2016-08-22 21:16:37", "url": "/3237/2/O'Donovan_Francis_Thomas_2008.PDF" } ], "eprint_id": 3237, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "O'Donovan_Francis_Thomas_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/22280", "doc_id": 22280, "rev_number": 2, "files": [ { "id": "/id/file/33966", "fileid": 33966, "datasetid": "document", "objectid": 22280, "filename": "preview.png", "mime_type": "image/png", "hash": "8a5b9c81fd873998a785fe99658ac2d9", "hash_type": "MD5", "filesize": 17332, "mtime": "2012-12-26 02:58:24", "url": "/3237/3/preview.png" } ], "eprint_id": 3237, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5738" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5738" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5738" } ] } }, { "id": "/id/document/123491", "doc_id": 123491, "rev_number": 1, "files": [ { "id": "/id/file/368906", "fileid": 368906, "datasetid": "document", "objectid": 123491, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "ba82e367fe6d6824ced008239ffd122c", "hash_type": "MD5", "filesize": 30087, "mtime": "2021-06-23 22:41:42", "url": "/3237/4/indexcodes.txt" } ], "eprint_id": 3237, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5738" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5738" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5738" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/37", "datestamp": "2007-09-05", "lastmod": "2023-05-30 22:31:48", "status_changed": "2009-09-25 02:55:02", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ftod@caltech.edu", "id": "O'Donovan-Francis-Thomas", "name": { "family": "O'Donovan", "given": "Francis Thomas" }, "orcid": "0000-0002-4858-6106", "show_email": "NO" } ] }, "title": "The Detection and Exploration of Planets from the Trans-Atlantic Exoplanet Survey", "ispublished": "unpub", "full_text_status": "public", "keywords": "exoplanets; extrasolar planets; planetary systems; stars; transiting; transits", "abstract": "I present the discovery of three transiting planets (TrES-2, TrES-3, and TrES-4) of nearby bright stars made with the ten-centimeter telescope Sleuth as part of the Trans-atlantic Exoplanet Survey (TrES). TrES-2 is the first transiting exoplanet detected in the field of view of NASA\u2019s Kepler mission. Of the 20 known transiting exoplanets, TrES-3 has the second shortest period, facilitating the study of orbital decay and atmospheric evaporation. Its visible/infrared brightness makes TrES-3 an ideal target for observations to determine the atmospheric composition. TrES-4 has the largest radius and lowest density of the known transiting planets. These three planets have radii larger than that of Jupiter, and the radius of TrES-4 significantly exceeds predictions from models of hot Jupiters, indicating a possible lack of an energy source in these models.
\r\n\r\nI present the results of Spitzer observations of TrES-2. I reject tidal dissipation of eccentricity as an explanation for the inflated radius, and examine the spectrum for evidence of atmospheric absorption.
\r\n\r\nI have monitored 19 fields each containing 6,000\u201336,000 stars for evidence of transits. I discuss the rejection of six of my candidate transiting systems from an early field that represent examples of the 67 astrophysical false positives that I encountered in Sleuth data. These six false positives highlight the benefit of a multisite survey such as TrES, and also of comprehensive follow-up of transit candidates. As a further example, I present the candidate GSC 03885-00829 from Sleuth data that was revealed to be a blend of a bright F dwarf and a fainter K-dwarf eclipsing binary. This candidate proved nontrivial to reject, requiring multicolor follow-up photometry to produce evidence of the true binary nature of this candidate.
\r\n\r\nThe yield of planets from transit surveys is not yet well constrained or understood. There are numerous factors that affect the predictions such as the amount of correlated photometric noise present in the data. Here I present an analysis of my ability to recover fake transits in TrES data. I examined both the automated transit-search algorithm and my own visual identification process. I find the recovery rate of my visual analysis to be 87% for those transit candidates that had a sufficiently high signal-to-noise ratio to be flagged by my transit-search algorithm and readily identifiable by eye.
", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-08272007-043911", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08272007-043911", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-09-05", "doi": "10.7907/585M-JF91", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "dcharbon@cfa.harvard.edu", "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "dcharbon@cfa.harvard.edu", "id": "Charbonneau-D", "name": { "family": "Charbonneau", "given": "David" }, "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-08-27", "thesis_defense_date": "2007-07-31", "thesis_approved_date": "2007-09-05", "gradofc_approval_date": "2007-08-30", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "O'Donovan, Francis Thomas" }, { "id": "/id/eprint/3182", "eprint_id": 3182, "rev_number": 9, "documents": [ { "id": "/id/document/5646", "doc_id": 5646, "rev_number": 2, "files": [ { "id": "/id/file/33384", "fileid": 33384, "datasetid": "document", "objectid": 5646, "filename": "thesis_final.pdf", "mime_type": "application/pdf", "filesize": 4753615, "mtime": "2012-12-26 02:57:47", "url": "/3182/1/thesis_final.pdf" } ], "eprint_id": 3182, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis_final.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis_final.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22189" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22189" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22189" } ] } }, { "id": "/id/document/16280", "doc_id": 16280, "rev_number": 3, "files": [ { "id": "/id/file/204011", "fileid": 204011, "datasetid": "document", "objectid": 16280, "filename": "Moran_Sean_M_2008.PDF", "mime_type": "application/pdf", "filesize": 44548, "mtime": "2016-08-22 21:16:35", "url": "/3182/2/Moran_Sean_M_2008.PDF" } ], "eprint_id": 3182, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Moran_Sean_M_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/22189", "doc_id": 22189, "rev_number": 2, "files": [ { "id": "/id/file/33382", "fileid": 33382, "datasetid": "document", "objectid": 22189, "filename": "preview.png", "mime_type": "image/png", "hash": "ecf19a822fa8638d0be9fb1610eb47d7", "hash_type": "MD5", "filesize": 19421, "mtime": "2012-12-26 02:57:47", "url": "/3182/3/preview.png" } ], "eprint_id": 3182, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5646" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5646" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5646" } ] } }, { "id": "/id/document/123426", "doc_id": 123426, "rev_number": 1, "files": [ { "id": "/id/file/368839", "fileid": 368839, "datasetid": "document", "objectid": 123426, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "9cf42ad94bd5e3d3840d067434e71acc", "hash_type": "MD5", "filesize": 36653, "mtime": "2021-06-23 22:38:52", "url": "/3182/4/indexcodes.txt" } ], "eprint_id": 3182, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5646" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5646" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5646" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/82", "datestamp": "2007-09-05", "lastmod": "2019-12-03 22:30:55", "status_changed": "2009-09-25 02:53:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "smoran@cfa.harvard.edu", "id": "Moran-Sean-Michael", "name": { "family": "Moran", "given": "Sean Michael" }, "orcid": "0000-0002-9194-5071", "show_email": "YES" } ] }, "title": "Understanding the Physical Processes Driving Galaxy Evolution in Clusters: A Case Study of Two z ~ 0.5 Galaxy Clusters", "ispublished": "unpub", "full_text_status": "public", "keywords": "GALEX", "abstract": "Clusters of galaxies represent the largest laboratories in the universe for testing the incredibly chaotic physics governing the collapse of baryons into the stars, galaxies, groups, and diffuse clouds that we see today. Within the cluster environment, there are a wide variety of physical processes that may be acting to transform galaxies.
\r\n\r\nIn this thesis, we combine extensive Keck spectroscopy with wide-field HST imaging to perform a detailed case study of two intermediate redshift galaxy clusters, Cl 0024+1654 (z=0.395) and MS 0451-03 (z=0.540). Leveraging a comprehensive multiwavelength data set that spans the X-ray to infrared, and with spectral-line measurements serving as the key to revealing both the recent star-formation histories and kinematics of infalling galaxies, we aim to shed light on the environmental processes that could be acting to transform galaxies in clusters.
\r\n\r\nWe adopt a strategy to make maximal use of our HST-based morphologies by splitting our sample of cluster galaxies according to morphological type, characterizing signs of recent evolution in spirals and early types separately. This approach proves to be powerful in identifying galaxies that are currently being altered by an environmental interaction: early-type galaxies that have either been newly transformed or prodded back into an active phase, and spiral galaxies where star formation is being suppressed or enhanced all stand out in our sample.
\r\n\r\nWe begin by using variations in the early-type galaxy population as indicators of recent activity. Because ellipticals and S0s form such a homogeneous class in the local universe, we are sensitive to even very subtle signatures of recent and current environmental interactions. This study has yielded two key results: By constructing the Fundamental Plane (FP) of Cl 0024, we observe that elliptical and S0 galaxies exhibit a high scatter in their FP residuals, which occurs only among galaxies in the cluster core, suggesting a turbulent assembly history for Cl 0024 early types. Near the Virial radius of Cl 0024, we observe a number of compact, intermediate-mass ellipticals undergoing a burst of star formation or weak AGN activity, indicated by strong [O II] emission; their locations may mark the minimum radius at which merging is effective in each cluster.
\r\n\r\nWhile E+S0 galaxies do prove to be sensitive indicators of environmental interaction, it is the spiral galaxies that, of course, host the bulk of star formation within and around these clusters. We therefore probe for kinematic disturbances in spiral disks by measuring resolved rotation curves from optical emission lines, and constructing the Tully-Fisher relation for spirals across Cl 0024 and MS 0451. We find that the cluster Tully-Fisher relation exhibits significantly higher scatter than the field relation. In probing for the origin of this difference, we find that the central mass densities of star-forming spirals exhibit a sharp break near the cluster Virial radius, with spirals in the cluster outskirts exhibiting significantly lower densities. We argue that these results considered together demonstrate that cluster spirals are kinematically disturbed by their environment, likely due to galaxy-galaxy interactions (harassment).
\r\n\r\nWe then discuss our most powerful method of tracking galaxy evolution across Cl 0024 and MS 0451: identifying and studying \"transition galaxies\"-galaxies whose stellar populations or dynamical states indicate a recent or ongoing change in morphology or star formation rate. Such galaxies are often revealed by star formation histories that seem to be at odds with the galaxy morphologies: for example, spiral galaxies with no signs of star formation, or elliptical galaxies that do show signs of star formation.
\r\n\r\nWe identify and study one such class of objects, the \"passive spirals\" in Cl 0024. These objects exhibit no emission lines in their spectra, suggesting a lack of star formation, yet are surprisingly detected in the UV, revealing the presence of young stars. By modeling the different temporal sensitivities of UV and spectroscopic data to recent activity, we show that star formation in Cl 0024 passive spirals has decayed on timescales of less than 1 Gyr, consistent with the action of \"gas starvation\".
\r\n\r\nWe then build on and link together our previous indications of galaxy evolution at work, aiming to piece together a more comprehensive picture of how cluster galaxies are affected by their environment at intermediate redshift. To accomplish this, we document what we believe to be the first direct evidence for the transformation of spirals into S0s: through an analysis of their stellar populations and recent star formation rates, we link the passive spiral galaxies in both clusters to their eventual end states as newly generated cluster S0 galaxies. Differences between the two clusters in both the timescales and spatial location of this conversion process allow us to evaluate the relative importance of several proposed physical mechanisms that could be responsible for the transformation. Combined with other diagnostics that are sensitive to either ICM-driven galaxy evolution or galaxy-galaxy interactions, we describe a self-consistent picture of galaxy evolution in clusters.
\r\n\r\nWe find that spiral galaxies within infalling groups have already begun a slow process of conversion into S0s primarily via gentle galaxy-galaxy interactions that act to quench star formation. The fates of spirals upon reaching the core of the cluster depend heavily on the cluster ICM, with rapid conversion of all remaining spirals into S0s via ram-pressure stripping in clusters where the ICM is dense. In the presence of a less-dense ICM, the conversion continues at a slower pace, with galaxy-galaxy interactions continuing to play a role along with \"starvation\" by the ICM. We conclude that the buildup of the local S0 population through the transformation of spiral galaxies is a heterogeneous process that nevertheless proceeds robustly across a variety of different environments from cluster outskirts to cores.
", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-08212007-151300", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08212007-151300", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-09-05", "doi": "10.7907/C7Q1-DF25", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "george@astro.caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-08-21", "thesis_defense_date": "2007-08-01", "thesis_approved_date": "2007-09-05", "gradofc_approval_date": "2007-08-30", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Moran, Sean Michael" }, { "id": "/id/eprint/5130", "eprint_id": 5130, "rev_number": 12, "documents": [ { "id": "/id/document/8122", "doc_id": 8122, "rev_number": 2, "files": [ { "id": "/id/file/50022", "fileid": 50022, "datasetid": "document", "objectid": 8122, "filename": "Sayers_thesis_20071231.pdf", "mime_type": "application/pdf", "filesize": 8379682, "mtime": "2012-12-26 03:15:06", "url": "/5130/1/Sayers_thesis_20071231.pdf" } ], "eprint_id": 5130, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Sayers_thesis_20071231.pdf", "language": "en", "security": "public", "license": "other", "main": "Sayers_thesis_20071231.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/24627" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/24627" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/24627" } ] } }, { "id": "/id/document/16457", "doc_id": 16457, "rev_number": 3, "files": [ { "id": "/id/file/204528", "fileid": 204528, "datasetid": "document", "objectid": 16457, "filename": "Sayers_Jack_2008.PDF", "mime_type": "application/pdf", "filesize": 40837, "mtime": "2016-08-22 21:17:48", "url": "/5130/2/Sayers_Jack_2008.PDF" } ], "eprint_id": 5130, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Sayers_Jack_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/24627", "doc_id": 24627, "rev_number": 2, "files": [ { "id": "/id/file/50020", "fileid": 50020, "datasetid": "document", "objectid": 24627, "filename": "preview.png", "mime_type": "image/png", "hash": "e2c1b0667baecf0ca7f76352652457d2", "hash_type": "MD5", "filesize": 9204, "mtime": "2012-12-26 03:15:06", "url": "/5130/3/preview.png" } ], "eprint_id": 5130, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/8122" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/8122" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/8122" } ] } }, { "id": "/id/document/124803", "doc_id": 124803, "rev_number": 1, "files": [ { "id": "/id/file/370233", "fileid": 370233, "datasetid": "document", "objectid": 124803, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "de6e6e6842dfd9cb5b9b11c862a3a91a", "hash_type": "MD5", "filesize": 36973, "mtime": "2021-06-23 23:54:54", "url": "/5130/4/indexcodes.txt" } ], "eprint_id": 5130, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/8122" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/8122" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/8122" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/51/30", "datestamp": "2008-01-16", "lastmod": "2020-03-10 19:21:59", "status_changed": "2009-09-25 03:33:51", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jack@caltech.edu", "id": "Sayers-Jack", "name": { "family": "Sayers", "given": "Jack" }, "orcid": "0000-0002-8213-3784", "show_email": "YES" } ] }, "title": "A Search for Cosmic Microwave Background Anisotropies on Arcminute Scales", "ispublished": "unpub", "full_text_status": "public", "keywords": "atmospheric noise; bolometers; CMB; cosmology; galaxy clusters; Sunyaev-Zeldovich", "abstract": "This thesis describes the results of two sets of observations made in 2003 and 2004 using Bolocam from the Caltech Submillimeter Observatory (CSO), along with a description of the design and performance of the instrument. Bolocam is a large format camera consisting of 144 bolometers with an eight arcminute field of view at the CSO, and can be operated non-simultaneously at 1.1, 1.4, or 2.1 mm. All of the data described in this thesis was collected at 2.1 mm, where the individual beams are approximately one arcminute in size. The observations were made over a total of seventy-nine nights, and consisted of surveys of two science fields, Lynx and the Subaru/XMM Deep Field (SDS1), covering a total area of approximately 1 square degree. The noise properties of the maps are extremely uniform, with RMS variations in coverage of approximately 1.5% for twenty arcsecond map pixels. The point source sensitivity of the maps is approximately 100 \u03bcKCMB per beam. Fluctuations in emission from the atmosphere limited the sensitivity of our measurements, and several algorithms designed to remove these fluctuations are described. These algorithms also removed astronomical flux, and simulations were used to determine the effect of this attenuation on a CMB power spectrum. Assuming a flat CMB band power in C\u2113, our data corresponds to an effective angular multipole of \u2113eff = 5700, with a FWHM\u2113 = 2800. At these scales the CMB power spectrum is expected to be dominated by anisotropies induced by the Sunyaev-Zel'dovich effect (SZE), and have a reasonably flat spectrum. Our data is consistent with a band power of C\u2113 = 0 \u03bcK2CMB1, and an upper limit of C\u2113 <\t755 \u03bcK2CMB at a confidence level of 90%. From this result we find that \u03c38 < 1.55 at a confidence level of 90%.\r\n", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-12232007-013248", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-12232007-013248", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-01-16", "doi": "10.7907/2Q9Q-JA33", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "chair" }, { "email": "ael@astro.caltech.edu", "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew E." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "scf@theory.caltech.edu", "id": "Frautschi-S-C", "name": { "family": "Frautschi", "given": "Steven C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-12-23", "thesis_defense_date": "2007-12-05", "thesis_approved_date": "2008-01-16", "gradofc_approval_date": "2008-01-14", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"dir": "disk0/00/00/30/90", "datestamp": "2007-08-31", "lastmod": "2023-05-30 22:16:11", "status_changed": "2009-09-25 02:51:09", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "cls@astro.caltech.edu", "id": "Slesnick-Catherine-Louise", "name": { "family": "Slesnick", "given": "Catherine Louise" }, "show_email": "NO" } ] }, "title": "1-10 Myr-Old Low Mass Stars and Brown Dwarfs in Nearby Star Forming Regions", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy; brown dwarfs; circumstellar disks; IMF; star formation", "abstract": "My thesis research has focused primarily on identifying and characterizing pre-main sequence stars in nearby star-forming regions. To this end, I carried out wide-field (~150-250 deg\u00b2) optical photometric and spectroscopic surveys in and near the star forming regions of Taurus and Upper Scorpius.
\r\n\r\nIn Taurus, the aim of my optical photometric/spectroscopic survey was specifically to probe for a population of intermediate-age pre-main sequence stars outside of the young subclusters that are known to contain most of the young Taurus population. From this work I found tens of young (~1-3 Myr) and intermediate-age (~5-10 Myr) stars both near the known Taurus population and to the east, but relatively few pre-main sequence stars of any age to the west. I argued that the new pre-main sequence stars identified far from Taurus can not have originated from the vicinity of the 1-2 Myr-old subclusters and I proposed instead that they comprise a new, previously undiscovered region of recent star formation.
\r\n\r\nIn USco, the aim of my optical photometric/spectroscopic survey was to probe beyond previously explored regions to identify large numbers of 5 Myr-old low mass stars. From the spectroscopic data I have discovered 145 low mass members of USco. Using Monte Carlo simulations I showed that, taking into account known observational errors, the observed age dispersion for the low mass population in USco is consistent with all stars forming in a single burst ~5 Myr ago. I also derived the first spectroscopic mass function for USco that extends into the substellar regime and compared results to similar mass functions derived for stars in four other young clusters and associations.
", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-08102007-161741", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08102007-161741", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-08-31", "doi": "10.7907/D7XM-E815", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "chair" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "member" }, { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "member" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-08-10", "thesis_defense_date": "2007-07-31", "thesis_approved_date": "2007-08-31", "gradofc_approval_date": "2007-08-30", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Slesnick, Catherine Louise" }, { "id": "/id/eprint/3526", "eprint_id": 3526, "rev_number": 13, "documents": [ { "id": "/id/document/6089", "doc_id": 6089, "rev_number": 3, "files": [ { "id": "/id/file/36351", "fileid": 36351, "datasetid": "document", "objectid": 6089, "filename": "SuyuThesisNewStyle.pdf", "mime_type": "application/pdf", "filesize": 7743174, "mtime": "2012-12-26 03:00:41", "url": "/3526/1/SuyuThesisNewStyle.pdf" } ], "eprint_id": 3526, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis", "language": "en", "security": "public", "license": "other", "main": "SuyuThesisNewStyle.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22629" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22629" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22629" } ] } }, { "id": "/id/document/16544", "doc_id": 16544, "rev_number": 3, "files": [ { "id": "/id/file/204089", "fileid": 204089, "datasetid": "document", "objectid": 16544, "filename": "Suyu_Sherry_H_2008.PDF", "mime_type": "application/pdf", "filesize": 42396, "mtime": "2016-08-22 21:16:47", "url": "/3526/2/Suyu_Sherry_H_2008.PDF" } ], "eprint_id": 3526, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Suyu_Sherry_H_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/22629", "doc_id": 22629, "rev_number": 2, "files": [ { "id": "/id/file/36349", "fileid": 36349, "datasetid": "document", "objectid": 22629, "filename": "preview.png", "mime_type": "image/png", "hash": "c8c16b65bf8c022ebb54d4fd12a59da6", "hash_type": "MD5", "filesize": 18226, "mtime": "2012-12-26 03:00:41", "url": "/3526/3/preview.png" } ], "eprint_id": 3526, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6089" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6089" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6089" } ] } }, { "id": "/id/document/123674", "doc_id": 123674, "rev_number": 1, "files": [ { "id": "/id/file/369098", "fileid": 369098, "datasetid": "document", "objectid": 123674, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "cbac74d85ae0a25c135c67b09d7787bb", "hash_type": "MD5", "filesize": 27548, "mtime": "2021-06-23 22:52:12", "url": "/3526/4/indexcodes.txt" } ], "eprint_id": 3526, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6089" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6089" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/6089" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/26", "datestamp": "2007-09-17", "lastmod": "2020-03-10 23:39:06", "status_changed": "2009-09-25 03:00:09", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "suyu@mpa-garching.mpg.de", "id": "Suyu-Sherry-Hsuan", "name": { "family": "Suyu", "given": "Sherry Hsuan" }, "orcid": "0000-0001-5568-6052", "show_email": "NO" } ] }, "title": "Dissecting the Gravitational Lens B1608+656: Implications for the Hubble Constant", "ispublished": "unpub", "full_text_status": "public", "keywords": "distance scale; galaxies: individual (B1608+656); gravitational lensing; methods: data analysis", "abstract": "Strong gravitational lens systems provide a tool for probing galaxy mass distributions (independent of their light profiles) and for measuring cosmological parameters. In a strong lens system, the background source intensity distribution is multiply imaged. If the source intensity is time varying, then the multiple images of the variable source are delayed in time relative to each other due to the different light travel time along the multiple light paths. One can use lens systems to measure the Hubble constant by obtaining the relative time delays between the multiple images and modeling the lens potential. B1608+656 is a quadruply imaged gravitational lens system with a spatially extended source intensity distribution and two interacting galaxy lenses. This system is unique in that the three relative time delays between the four images were measured accurately with errors of only a few percent, and it thus provides an opportunity to measure the Hubble constant with high precision. The extended source intensity distribution in B1608+656 provides additional constraints on the lens potential, though simultaneous determination of the source intensity and lens potential distribution is needed. The presence of dust and interacting galaxy lenses further complicate this system. We present a comprehensive analysis in a Bayesian framework that takes into account the extended source intensity distribution, interacting galaxy lenses, and the presence of dust for reconstructing the lens potential. Using the deep HST ACS observations on B1608+656, the resulting statistical uncertainty on H_0 associated with the lens modeling is limited by the uncertainty in the best time delay measurement (~3%). The dominant systematic error on H_0 is due to the effects of the environment on B1608+656 (mass-sheet degeneracy). By using the measured velocity dispersion of the lens galaxies and considering the mass structures along the line of sight to B1608+656, we place constraints on the external convergence associated with galaxy groups and mass structure along the line of sight. The resulting Hubble constant from B1608+656 is H_0 = 72 \u00b1 2 (stat.) \u00b1 4 (syst.) km s^-1 Mpc^-1.\r\n", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-09132007-122424", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09132007-122424", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-09-17", "doi": "10.7907/MQS2-Y860", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "rdb3@stanford.edu", "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "advisor" }, { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "rdb3@stanford.edu", "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "co-chair" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-09-13", "thesis_defense_date": "2007-06-14", "thesis_approved_date": "2007-09-17", "gradofc_approval_date": "2007-09-13", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Suyu, Sherry Hsuan" }, { "id": "/id/eprint/1783", "eprint_id": 1783, "rev_number": 13, "documents": [ { "id": "/id/document/2904", "doc_id": 2904, "rev_number": 2, "files": [ { "id": "/id/file/17669", "fileid": 17669, "datasetid": "document", "objectid": 2904, "filename": "cit_thesis.pdf", "mime_type": "application/pdf", "filesize": 5868356, "mtime": "2012-12-26 02:42:00", "url": "/1783/1/cit_thesis.pdf" } ], "eprint_id": 1783, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "cit_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "cit_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19627" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19627" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19627" } ] } }, { "id": "/id/document/13951", "doc_id": 13951, "rev_number": 3, "files": [ { "id": "/id/file/201722", "fileid": 201722, "datasetid": "document", "objectid": 13951, "filename": "Barkume_Kristina_Marie_2008.PDF", "mime_type": "application/pdf", "filesize": 43201, "mtime": "2016-08-22 21:15:06", "url": "/1783/2/Barkume_Kristina_Marie_2008.PDF" } ], "eprint_id": 1783, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Barkume_Kristina_Marie_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/19627", "doc_id": 19627, "rev_number": 2, "files": [ { "id": "/id/file/17667", "fileid": 17667, "datasetid": "document", "objectid": 19627, "filename": "preview.png", "mime_type": "image/png", "hash": "0a0b981f565cc6e99f6348aab6dfbdb6", "hash_type": "MD5", "filesize": 14270, "mtime": "2012-12-26 02:41:59", "url": "/1783/3/preview.png" } ], "eprint_id": 1783, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2904" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2904" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2904" } ] } }, { "id": "/id/document/121247", "doc_id": 121247, "rev_number": 1, "files": [ { "id": "/id/file/366639", "fileid": 366639, "datasetid": "document", "objectid": 121247, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "14cd4f8a79de6a099de5b02a022fd623", "hash_type": "MD5", "filesize": 24502, "mtime": "2021-06-23 21:21:16", "url": "/1783/4/indexcodes.txt" } ], "eprint_id": 1783, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2904" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2904" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2904" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/83", "datestamp": "2008-05-20", "lastmod": "2020-03-04 21:56:51", "status_changed": "2009-09-25 02:15:15", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "barkume@gmail.com", "id": "Barkume-Kristina-Marie", "name": { "family": "Barkume", "given": "Kristina Marie" }, "show_email": "NO" } ] }, "title": "Surface Properties of Kuiper Belt Objects and Centaurs", "ispublished": "unpub", "full_text_status": "public", "keywords": "Centaurs; Kuiper Belt Objects; Small Solar System Bodies", "abstract": "The outer solar system is inhabited by a population of small solar system bodies called Kuiper belt Objects (KBOs) and Centaurs. I present a survey of visible and near infrared (NIR) spectra of the brightest KBOs and Centaurs. The visible spectra of 19 KBOs were obtained at Palomar Observatory. At the W.M. Keck Observatory, NIR spectra were obtained for 33 KBOs and 12 Centaurs. This data marks a significant leap in the available spectra, allowing for the population to be studied as whole.
\r\n\r\nThe spectra reveal that most KBOs are covered with a material with characteristics similar to irradiate ices rich in complex organic compounds. Water ice is also observed on some KBOs and Centaurs, though its abundance is variable across the samples. A two end member mixing model is found to describe the NIR spectral properties well, but poorly fits the visible-NIR data. This suggests that the non-water ice component is heterogeneous across the KBO and Centuar populations. To characterize the non-ice component better, the visible spectra are analyzed for signatures of both organic and mineralogical features. No evidence is found for the presence of minerals, but the spectra suggest complex organics are a dominant spectral component. The abundance of water is shown to directly correlate with diameter for KBOs, but not Centaurs, suggesting it is controlled by geophysical processes on KBOs.
\r\n\r\nThe analysis of these spectra has revealed an unusual population of KBOs that are now identified as mantle fragments from the large KBO 2003 EL61. The collision that spun-up 2003 EL61, formed its satellite system, and ejected the mantle fragments into the Kuiper belt is discussed. The unusual spectral properties of 2003 EL61, its brightest satellite, and the fragments are examined. Analysis suggests that the surfaces of all these objects can be composed of nearly pure water ice, suggesting that their volatile organic inventory has been lost. The discovery of crystalline water ice on these small KBOs suggests that crystallization is not an indication of recent surface activity as was previously suggested.
\r\n", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-05132008-202158", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05132008-202158", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-20", "doi": "10.7907/EQY1-NM23", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "email": "mbrown@caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "member" }, { "email": "oa@gps.caltech.edu", "id": "Aharonson-O", "name": { "family": "Aharonson", "given": "Oded" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-13", "thesis_defense_date": "2007-12-17", "thesis_approved_date": "2008-05-20", "gradofc_approval_date": "2008-05-19", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Barkume, Kristina Marie" }, { "id": "/id/eprint/2779", "eprint_id": 2779, "rev_number": 46, "documents": [ { "id": "/id/document/5097", "doc_id": 5097, "rev_number": 5, "files": [ { "id": "/id/file/29777", "fileid": 29777, "datasetid": "document", "objectid": 5097, "filename": "01mle_frontmatter.pdf", "mime_type": "application/pdf", "filesize": 121987, "mtime": "2012-12-26 02:54:19", "url": "/2779/1/01mle_frontmatter.pdf" } ], "eprint_id": 2779, "pos": 1, "placement": 2, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "01mle_frontmatter.pdf", "language": "en", "security": "public", "license": "other", "main": "01mle_frontmatter.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { 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], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/27/79", "datestamp": "2007-08-07", "lastmod": "2019-12-03 22:30:48", "status_changed": "2009-09-25 02:44:42", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "menoch@astro.caltech.edu", "id": "Enoch-Melissa-Lanae", "name": { "family": "Enoch", "given": "Melissa Lanae" }, "show_email": "NO" } ] }, "title": "Molecular Clouds and Star Formation: A Multiwavelength Study of Perseus, Serpens, and Ophiuchus", "ispublished": "unpub", "full_text_status": "public", "keywords": "bolometer arrays; millimeter continuum; molecular clouds; protostars; star formation", "abstract": "In this thesis I utilize large-scale millimeter and mid- to far-infrared surveys to address a number of outstanding questions regarding the formation of low mass stars in molecular clouds. Continuum \u03bb = 1.1 mm maps completed with Bolocam at a resolution of 31\" cover the largest areas observed to date at millimeter or submillimeter wavelengths in three molecular clouds: 7.5 deg\u00b2 in Perseus (140 pc\u00b2 at the adopted distance of d = 250 pc), 10.8 deg\u00b2 (50 pc\u00b2 at d = 125 pc) in Ophiuchus, and 1.5 deg\u00b2 (30 pc\u00b2 at d = 125 pc) in Serpens. These surveys are sensitive to dense substructures with mean density n \u2273 2 - 3 x 10\u2074 cm\u207b\u00b3. A total of 122 cores are detected in Perseus, 44 in Ophiuchus, and 35 in Serpens above mass detection limits of 0.1 - 0.2 Msun. Combining with Spitzer mid- and far-infrared maps from the c2d Legacy program provides wavelength coverage from \u03bb = 1.25-1100 \u03bcm, and enables the assembly of an unbiased, complete sample of the youngest star forming objects in three environments. This sample includes 108 prestellar cores, 43 Class 0 sources and 94 Class I sources.
\r\n\r\nThe approximately equal number of starless cores and embedded protostars in each cloud implies a starless core lifetime of 2 - 4 x 10\u2075 yr, only a few free-fall timescales. This timescale, considerably shorter than the timescale predicted by the classic scenario of magnetic field support in which core evolution is moderated by ambipolar diffusion, suggests that turbulence is the dominant process controlling the formation and evolution of dense cores. However, dense cores in all three clouds are found only at high cloud column densities, where AV\u2273 7 mag, and the fraction of cloud mass in these cores is less than 10%, indicating that magnetic fields must play some role as well. Measured angular deconvolved sizes of the majority of starless cores are consistent with relatively flattened radial density profiles, or with Bonnor-Ebert spheres. The prestellar core mass distribution (CMD) has a slope of \u03b1 = -2.5 \u00b1 0.2 for M > 0.8 Msun, remarkably similar to recent measurements of the slope of the stellar initial mass function: \u03b1 = -2.3 to -2.8. While this result does not rule out the importance of feedback or competitive accretion, it provides support for the hypothesis that stellar masses are determined during the core formation process.
\r\n\r\nThe lifetime of the Class 0 phase is estimated to be 1 - 2 x 10\u2075 yr in Perseus and Serpens, or approximately half that of the Class I phase, arguing against a very rapid early accretion phase. In Ophiuchus the fraction of Class 0 sources is much smaller, consistent with previous measurements of a short (~ 10\u2074 yr) Class 0 phase in that cloud. A large population of low luminosity Class I sources that cannot be explained by constant or monotonically decreasing accretion rates is observed in each cloud. This result strongly suggest that accretion during the Class I phase is episodic, with sources spending approximately 25% of the Class I lifetime in a quiescent state.
\r\n\r\nFinally, I investigate the environmental dependence of star formation by comparing the dense core populations of the three clouds. Cores are found at considerably higher cloud column densities in Ophiuchus than in Perseus or Serpens; more than 75% of cores occur at visual extinctions of AV\u2273 8 mag in Perseus, AV\u2273 15 mag in Serpens, and AV\u2273 20 - 23 mag in Ophiuchus. Cloud CMDs are well characterized by power-law fits above their empirically derived 50% completeness limits, resulting in slopes of \u03b1 = -2.1 \u00b1 0.1 in Perseus, \u03b1 = -2.1 \u00b1 0.3 in Ophiuchus, and \u03b1 = -1.6 \u00b1 0.2 in Serpens. Measured slopes for Perseus and Ophiuchus broadly agree with turbulent fragmentation, but the relative shapes of the observed cloud CMDs are inconsistent with detailed simulations of the dependence of CMD shape on Mach number.
", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-06292007-134316", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06292007-134316", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "suggestions": "Released to public view 10042017", "deposited_by": "Imported from ETD-db", "deposited_on": "2007-08-07", "doi": "10.7907/25QK-5K72", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "chair" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "role": "member" }, { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "role": "member" }, { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "role": "member" }, { "email": "golwala@astro.caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-06-29", "thesis_defense_date": "2007-06-08", "thesis_approved_date": "2007-08-07", "gradofc_approval_date": "2007-08-06", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Enoch, Melissa Lanae" }, { "id": "/id/eprint/2530", "eprint_id": 2530, "rev_number": 16, "documents": [ { "id": "/id/document/4789", "doc_id": 4789, "rev_number": 4, "files": [ { "id": "/id/file/27666", "fileid": 27666, "datasetid": "document", "objectid": 4789, "filename": "thesismain_0610.pdf", "mime_type": "application/pdf", "filesize": 4323316, "mtime": "2012-12-26 02:52:23", "url": "/2530/1/thesismain_0610.pdf" } ], "eprint_id": 2530, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis", "language": "en", "security": "public", "license": "other", "main": "thesismain_0610.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"datestamp": "2008-06-11", "lastmod": "2020-03-10 23:27:45", "status_changed": "2009-09-25 02:39:56", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jiansong.gao@nist.gov", "id": "Gao-Jiansong", "name": { "family": "Gao", "given": "Jiansong" }, "orcid": "0000-0001-9972-6220", "show_email": "YES" } ] }, "title": "The Physics of Superconducting Microwave Resonators", "ispublished": "unpub", "full_text_status": "public", "keywords": "background limited detection; conformal mapping", "abstract": "Over the past decade, low temperature detectors have brought astronomers revolutionary new observational capabilities and led to many great discoveries. Although a single low temperature detector has very impressive sensitivity, a large detector array would be much more powerful and are highly demanded for the study of more difficult and fundamental problems in astronomy. However, current detector technologies, such as transition edge sensors and superconducting tunnel junction detectors, are difficult to integrate into a large array.
\r\n\r\nThe microwave kinetic inductance detector (MKID)is a promising new detector technology invented at Caltech and JPL which provides both high sensitivity and an easy solution to the detector integration. It senses the change in the surface impedance of a superconductor as incoming photons break Cooper pairs, by using high-Q superconducting microwave resonators capacitively coupled to a common feedline. This architecture allows thousands of detectors to be easily integrated through passive frequency domain multiplexing.
\r\n\r\nIn this thesis, we explore the rich and interesting physics behind these superconducting microwave resonators. The first part of the thesis discusses the surface impedance of a superconductor, the kinetic inductance of a superconducting coplanar waveguide, and the circuit response of a resonator. These topics are related with the responsivity of MKIDs. The second part presents the study of the excess frequency noise that is universally observed in these resonators. The properties of the excess noise, including power, temperature, material, and geometry dependence, have been quantified. The noise source has been identified to be the two-level systems in the dielectric material on the surface of the resonator. A semi-empirical noise model has been developed to explain the power and geometry dependence of the noise, which is useful to predict the noise for a specified resonator geometry. The detailed physical noise mechanism, however, is still not clear.
\r\n\r\nWith the theoretical results of the responsivity and the semi-empirical noise model established in this thesis, a prediction of the detector sensitivity (noise equivalent power) and an optimization of the detector design are now possible.
\r\n", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-06092008-235549", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06092008-235549", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-06-11", "doi": "10.7907/RAT0-VM75", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "chair" }, { "email": "jpe@caltech.edu", "id": "Eisenstein-J-P", "name": { "family": "Eisenstein", "given": "James P." }, "role": "member" }, { "email": "mwb@caltech.edu", "id": "Bockrath-M-W", "name": { "family": "Bockrath", "given": "Marc William" }, "role": "member" }, { "email": "pbellan@caltech.edu", "id": "Bellan-P-M", "name": { "family": "Bellan", "given": "Paul Murray" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-06-09", "thesis_defense_date": "2008-05-28", "thesis_approved_date": "2008-06-11", "gradofc_approval_date": "2008-06-10", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Gao, Jiansong" }, { "id": "/id/eprint/2208", "eprint_id": 2208, "rev_number": 17, "documents": [ { "id": "/id/document/4051", "doc_id": 4051, "rev_number": 3, "files": [ { "id": "/id/file/23630", "fileid": 23630, "datasetid": "document", "objectid": 4051, "filename": "bjnaylor-thesis.bib", "mime_type": "", "filesize": 58631, "mtime": "2012-12-26 02:48:17", "url": "/2208/1/bjnaylor-thesis.bib" } ], "eprint_id": 2208, "pos": 1, "placement": 2, "format": "other", "format_desc": "bjnaylor-thesis.bib", "language": "en", "security": "public", "license": "other", "main": "bjnaylor-thesis.bib", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/4052", "doc_id": 4052, "rev_number": 4, "files": [ { "id": "/id/file/23634", 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indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4052" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4052" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4052" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/22/08", "datestamp": "2008-06-02", "lastmod": "2020-03-10 23:28:08", "status_changed": "2009-09-25 02:30:35", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "bret.j.naylor@jpl.nasa.gov", "id": "Naylor-Bret-Justin", "name": { "family": "Naylor", "given": "Bret Justin" }, "show_email": "NO" } ] }, "title": "Broadband Millimeter-Wave Spectroscopy with Z-Spec: An Unbiased Molecular-Line Survey of the Starburst Galaxy M82", "ispublished": "unpub", "full_text_status": "public", "keywords": "interstellar medium", "abstract": "Z-Spec is a broadband, millimeter-wave, direct-detection spectrometer based on a novel waveguide grating architecture. It is designed to fully cover the wide one-millimeter atmospheric window with a frequency range of 186 to 307 GHz at a resolution of ~ 250. The design goal is the detection of rotational and fine structure lines from the distant population of galaxies that make up the far-infrared background. Its large instantaneous bandwidth enables detection of multiple transitions of carbon monoxide and a relatively rapid determination of redshift. The grating design is based on the Rowland architecture but is much more compact because of the use of a parallel-plate waveguide propagation medium. Z-Spec uses 160 silicon nitride micromesh bolometers and is cooled to less than 100 mK to achieve background-limited performance. Moreover, Z-Spec serves as a technology demonstration of a technique that is uniquely suited to far-infrared extragalactic spectroscopy from space.
\r\n\r\nZ-Spec's capabilities enable wide-coverage, unbiased line surveys of nearby galaxies. Searches for molecular lines outside our own galaxy have typically been targeted at specific transitions of particular molecules. The brightest sources of extra-galactic molecular lines come from galaxies with physical conditions very different from those found in the Milky Way. Unbiased searches for spectral lines can discover transitions and molecules that are unexpected. A three-pointing study of the prototypical starburst galaxy M82 was performed with Z-Spec at the Caltech Submillimeter Observatory. The survey detected eleven bright lines in the center of the Z-Spec band, of which four had not been previously detected. Two of the new detections are for molecules that had been detected at lower frequencies (HNC 3 - 2 and C2H 3 - 2) and the other two are potentially transitions of SO2, for which only upper limits on lower frequency transitions were previously available. Several detected molecules are analyzed using a large-velocity-gradient (LVG) radiative-transfer model and indicate significant regions of high-density molecular gas along the major axis of M82.
", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-05282008-104041", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05282008-104041", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-06-02", "doi": "10.7907/Y6TP-5E10", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "jonas@submm.caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jonas@submm.caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "politzer@theory.caltech.edu", "id": "Politzer-H-D", "name": { "family": "Politzer", "given": "Hugh David" }, "role": "member" }, { "email": "golwala@astro.caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "member" }, { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-28", "thesis_defense_date": "2007-08-21", "thesis_approved_date": "2008-06-02", "gradofc_approval_date": "2008-05-30", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Naylor, Bret Justin" }, { "id": "/id/eprint/1825", "eprint_id": 1825, "rev_number": 13, "documents": [ { "id": "/id/document/2991", "doc_id": 2991, "rev_number": 2, "files": [ { "id": "/id/file/18125", "fileid": 18125, "datasetid": "document", "objectid": 2991, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 3493601, "mtime": "2012-12-26 02:42:26", "url": "/1825/1/thesis.pdf" } ], "eprint_id": 1825, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19701" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19701" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19701" } ] } }, { "id": "/id/document/15843", "doc_id": 15843, "rev_number": 3, "files": [ { "id": "/id/file/201819", "fileid": 201819, "datasetid": "document", "objectid": 15843, "filename": "Christopher_Micol_Huw_2008.PDF", "mime_type": "application/pdf", "filesize": 40464, "mtime": "2016-08-22 21:15:10", "url": "/1825/2/Christopher_Micol_Huw_2008.PDF" } ], "eprint_id": 1825, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Christopher_Micol_Huw_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/19701", "doc_id": 19701, "rev_number": 2, "files": [ { "id": "/id/file/18123", "fileid": 18123, "datasetid": "document", "objectid": 19701, "filename": "preview.png", "mime_type": "image/png", "hash": "164ea0302f5779465bba870df7fa98eb", "hash_type": "MD5", "filesize": 13826, "mtime": "2012-12-26 02:42:26", "url": "/1825/3/preview.png" } ], "eprint_id": 1825, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2991" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2991" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2991" } ] } }, { "id": "/id/document/121315", "doc_id": 121315, "rev_number": 1, "files": [ { "id": "/id/file/366707", "fileid": 366707, "datasetid": "document", "objectid": 121315, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "d7e1db259077c3bfd069d1a6b4db3b9d", "hash_type": "MD5", "filesize": 24919, "mtime": "2021-06-23 21:23:42", "url": "/1825/4/indexcodes.txt" } ], "eprint_id": 1825, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2991" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2991" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2991" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/18/25", "datestamp": "2008-05-22", "lastmod": "2023-05-30 22:31:30", "status_changed": "2009-09-25 02:16:18", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "christop@post.harvard.edu", "id": "Christopher-Micol-Huw", "name": { "family": "Christopher", "given": "Micol Huw" }, "show_email": "NO" } ] }, "title": "Young, Massive Star Clusters in the Antennae", "ispublished": "unpub", "full_text_status": "public", "keywords": "interacting galaxies; LRIS; NIRSPEC", "abstract": "While massive star clusters have been detected in almost every galaxy with appreciable star formation, they are most prevalent in interacting and merging galaxies. As many as 95% of these clusters will ultimately be disrupted, often in the first 10 Myr, but those clusters that do survive may be the progenitors of globular clusters. Many questions exist regarding these massive clusters and the processes that lead to their formation and disruption, including the uniformity of these processes within a galaxy and between galaxies with different degrees of cluster formation (e.g., quiescent spirals, starbursts, and merging systems). To address these questions, we present a detailed spectroscopic survey of young, massive star clusters in the Antennae, one of the best examples of cluster formation in a merging galaxy.
\r\n\r\nUsing near-infrared imaging, we selected a sample of 117 clusters to observe with a combination of near-infrared and optical spectroscopy at the W.M. Keck Observatory. These clusters were chosen to sample the major star-forming regions within the Antennae. This is the largest spectroscopic survey of young massive star clusters in any merging galaxy.
\r\n\r\nComparing the equivalent widths of hydrogen recombination lines and CO absorption bandheads to the population synthesis models of Starburst99, we measure the age of each cluster. More than half of the clusters show the simultaneous presence of hydrogen recombination lines and CO bandheads, which is not predicted by an instantaneous burst model of cluster formation. We determine that cluster formation is better modeled by a 5 Myr duration constant rate burst of star formation, which we apply to our cluster measurements. We find the vast majority of clusters have ages between 7 and 12 Myr, with a few younger clusters. Comparing cluster ages with predictions of the temporal evolution of cluster luminosity, we find the lack of older (>12 Myr) clusters (and to a lesser extent younger (<7 Myr) clusters) is not a selection effect but a true deficit. Variation in cluster ages exists with location in the Antennae, with the youngest clusters found in the overlap region where the disks of the two galaxies coincide. We interpret these age variations as an indication that cluster disruption rates differ by location within the Antennae.
\r\n\r\nCluster masses are measured by comparing the extinction-corrected K-band luminosity with model luminosity predictions. We find most cluster masses are between 105 and 106 M\u2609 with a median cluster mass around 3.5 x 105 M\u2609. Substantial variation exists in masses between different regions, with the overlap region having the most massive clusters on average. These mass differences can be interpreted as size-of-sample effects and our results are consistent with a uniform cluster initial mass function throughout the Antennae.
\r\n\r\nImproved spatial resolution CO (1-0) observations of the Antennae show that younger clusters coincide with areas of enhanced molecular gas concentration and, not surprisingly, also have on average higher extinctions. From two metallicity tracers, we find cluster metallicities consistent with solar values. Based on CO bandhead and SiI equivalent widths in the near-infrared spectra, we uncover strong evidence of a substantial population of M2--M4 supergiants in many of the older clusters.
\r\n", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-05152008-141502", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05152008-141502", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "suggestions": "mchristopher@mtsac.edu", "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-22", "doi": "10.7907/QP4P-SD67", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "schweizer@ociw.edu", "id": "Schweizer-F", "name": { "family": "Schweizer", "given": "Francois" }, "role": "member" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673", "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-15", "thesis_defense_date": "2008-03-21", "thesis_approved_date": "2008-05-22", "gradofc_approval_date": "2008-05-21", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Christopher, Micol Huw" }, { "id": "/id/eprint/926", "eprint_id": 926, "rev_number": 13, "documents": [ { "id": "/id/document/1418", "doc_id": 1418, "rev_number": 2, "files": [ { "id": "/id/file/8852", "fileid": 8852, "datasetid": "document", "objectid": 1418, "filename": "MandelThesis.pdf", "mime_type": "application/pdf", "filesize": 3813528, "mtime": "2012-12-26 02:33:44", "url": "/926/1/MandelThesis.pdf" } ], "eprint_id": 926, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "MandelThesis.pdf", "language": "en", "security": "public", "license": "other", "main": "MandelThesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18214" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18214" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18214" } ] } }, { "id": "/id/document/16233", "doc_id": 16233, "rev_number": 3, "files": [ { "id": "/id/file/200691", "fileid": 200691, "datasetid": "document", "objectid": 16233, "filename": "Mandel_Ilya_2008.PDF", "mime_type": "application/pdf", "filesize": 42863, "mtime": "2016-08-22 21:14:27", "url": "/926/2/Mandel_Ilya_2008.PDF" } ], "eprint_id": 926, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Mandel_Ilya_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/18214", "doc_id": 18214, "rev_number": 2, "files": [ { "id": "/id/file/8850", "fileid": 8850, "datasetid": "document", "objectid": 18214, "filename": "preview.png", "mime_type": "image/png", "hash": "6bda1e822ca15d538fe15a01217e0eb7", "hash_type": "MD5", "filesize": 17714, "mtime": "2012-12-26 02:33:44", "url": "/926/3/preview.png" } ], "eprint_id": 926, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1418" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/1418" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1418" } ] } }, { "id": "/id/document/120350", "doc_id": 120350, "rev_number": 1, "files": [ { "id": "/id/file/365733", "fileid": 365733, "datasetid": "document", "objectid": 120350, "filename": "indexcodes.txt", "mime_type": "text/x-c", "hash": "ab09c3bd36e2b12737d1cb05bc58283d", "hash_type": "MD5", "filesize": 37487, "mtime": "2021-06-23 20:45:13", "url": "/926/4/indexcodes.txt" } ], "eprint_id": 926, "pos": 4, "placement": 4, "mime_type": "text/x-c", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1418" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1418" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/1418" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/09/26", "datestamp": "2008-04-02", "lastmod": "2020-03-10 23:39:04", "status_changed": "2009-09-25 01:50:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "Ilya.Mandel@monash.edu", "id": "Mandel-Ilya", "name": { "family": "Mandel", "given": "Ilya" }, "orcid": "0000-0002-6134-8946", "show_email": "NO" } ] }, "title": "The Three Ss of Gravitational-Wave Astronomy: Sources, Signals, Searches", "ispublished": "unpub", "full_text_status": "public", "keywords": "black hole spin; black holes; extreme mass ratio inspirals; gravitational waves; intermediate mass ratio inspirals; LIGO; LISA; periodic standing wave approximation", "note": "Title varies slightly in 2008 Commencement Program: The Three S\u2019s of Gravitational-Wave Astronomy: Sources, Signals, Searches.", "abstract": "As gravitational wave astronomy prepares for the first detections of gravitational waves from compact-object binary inspirals, theoretical work is required on the study of (i) gravitational-wave sources, (ii) the signals emitted by those sources, and (iii) the searches for those signals in detector data. This thesis describes work on all three fronts. (i) We discuss intermediate-mass-ratio inspirals (IMRIs) of black holes or neutron stars into intermediate-mass black holes (IMBHs) that could be detected with Advanced LIGO. We analyze different mechanisms of IMRI formation and compute IMRI event rates of up to tens of events per year for Advanced LIGO. We study the spin evolution of IMBHs that grow through a series of minor mergers. We explore how a deviation of an IMRI's central body from a Kerr black hole influences geodesics, including the possibility of chaotic orbital dynamics. We also address the scientific consequences of extreme-mass-ratio inspiral (EMRI) detections by LISA for astrophysics and general relativity, and the difficulties associated with detecting and analyzing EMRI signals. (ii) We study the periodic standing-wave approximation (PSWA), which can potentially provide accurate waveforms in the last inspiral cycles of a comparable-mass black-hole binary. Using a simple model, we find that the solution to Einstein's equations for inspiraling black holes can be recovered to a high accuracy by the addition a perturbative radiation-reaction field to the standing-wave, noninspiraling solution. (iii) We demonstrate the utility of searching for and analyzing tracks in time-frequency spectrograms of a gravitational-wave signal as a means of estimating the parameters of a massive black-hole binary inspiral, as observed by LISA.", "date": "2008", "date_type": "degree", "id_number": "CaltechETD:etd-03112008-012506", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03112008-012506", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-04-02", "doi": "10.7907/GABY-T236", "alt_title": { "items": [ "The Three S\u2019s of Gravitational-Wave Astronomy: Sources, Signals, Searches" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "role": "member" }, { "email": "Curt.J.Cutler@jpl.nasa.gov", "id": "Cutler-C-J", "name": { "family": "Cutler", "given": "Curt J." }, "role": "member" }, { "email": "esp@caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-03-11", "thesis_defense_date": "2007-06-28", "thesis_approved_date": "2008-04-02", "gradofc_approval_date": "2008-04-02", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2008", "author_list": "Mandel, Ilya" }, { "id": "/id/eprint/807", "eprint_id": 807, "rev_number": 12, "documents": [ { "id": "/id/document/1208", "doc_id": 1208, "rev_number": 3, "files": [ { "id": "/id/file/7592", "fileid": 7592, "datasetid": "document", "objectid": 1208, "filename": "thesis_main.pdf", "mime_type": "application/pdf", "filesize": 5878517, "mtime": "2012-12-26 02:32:34", "url": "/807/1/thesis_main.pdf" } ], "eprint_id": 807, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis_main.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18009" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18009" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18009" } ] } }, { "id": "/id/document/16284", "doc_id": 16284, "rev_number": 3, "files": [ { "id": "/id/file/200516", "fileid": 200516, "datasetid": "document", "objectid": 16284, "filename": "Morris_Brad_2007.PDF", "mime_type": "application/pdf", "filesize": 42722, "mtime": "2016-08-22 21:14:21", "url": "/807/2/Morris_Brad_2007.PDF" } ], "eprint_id": 807, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Morris_Brad_2007.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/18009", "doc_id": 18009, "rev_number": 2, "files": [ { "id": "/id/file/7590", "fileid": 7590, "datasetid": "document", "objectid": 18009, "filename": "preview.png", "mime_type": "image/png", "hash": "aa8576dd9ad69ec560c7fa3c2270a580", "hash_type": "MD5", "filesize": 15286, "mtime": "2012-12-26 02:32:34", "url": "/807/3/preview.png" } ], "eprint_id": 807, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1208" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/1208" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1208" } ] } }, { "id": "/id/document/120206", "doc_id": 120206, "rev_number": 1, "files": [ { "id": "/id/file/365584", "fileid": 365584, "datasetid": "document", "objectid": 120206, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "ee7da25abbebdc1f09f88b708f6f5806", "hash_type": "MD5", "filesize": 25661, "mtime": "2021-06-23 20:40:04", "url": "/807/4/indexcodes.txt" } ], "eprint_id": 807, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1208" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1208" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/1208" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/08/07", "datestamp": "2007-02-28", "lastmod": "2021-01-15 23:35:15", "status_changed": "2009-09-25 01:46:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Morris-Bradford-S", "name": { "family": "Morris", "given": "Bradford S." }, "show_email": "NO" } ] }, "title": "Charge-Exchange Collision Dynamics and Ion Engine Grid Geometry Optimization", "ispublished": "unpub", "full_text_status": "public", "keywords": "differential cross-section; electric propulsion; ion engine; NSTAR; sputtering", "abstract": "The development of a new three-dimensional model for determining the absolute energy distribution of ions at points corresponding to spacecraft surfaces to the side of an ion engine is presented. The ions resulting from elastic collisions, both charge-exchange (CEX) and direct, between energetic primary ions and thermal neutral xenon atoms are accounted for. Highly resolved energy distributions of CEX ions are found by integration over contributions from all points in space within the main beam formed by the primary ions.
\r\n\r\nThe sputtering rate due to impingement of these ions on a surface is calculated. The CEX ions that obtain significant energy (10 eV or more) in the collision are responsible for the majority of the sputtering, though this can depend on the specific material being sputtered. In the case of a molybdenum surface located 60 cm to the side of a 30 cm diameter grid, nearly 90% of the sputtering is due to the 5% of ions with the highest collision exit energies. Previous models that do not model collision energetics cannot predict this. The present results agree with other models and predict that the majority of the ion density is due to collisions where little to no energy is transferred.
\r\n\r\nThe sputtering model is combined with a grid-structure model in an optimization procedure where the sputtering rate at specified locations is minimized by adjustment of parameters defining the physical shape of the engine grids. Constraints are imposed that require that the deflection of the grid under a specified load does not exceed a maximum value, in order to ensure survivability of the grids during launch. To faciliate faster execution of the calculations, simplifications based on the predicted behavior of the CEX ions are implemented. For diametrically opposed sputtering locations, a rounded barrel-vault shape reduces the expected sputtering rate by up to 30% in comparison to an NSTAR-shaped grid.
", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-02282007-154751", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-02282007-154751", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "GALCIT", "Astronomy Department", "Explosion Dynamics Laboratory" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-02-28", "doi": "10.7907/W996-M220", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Shepherd-J-E", "name": { "family": "Shepherd", "given": "Joseph E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "joseph.e.shepherd@caltech.edu", "id": "Shepherd-J-E", "name": { "family": "Shepherd", "given": "Joseph E." }, "role": "chair" }, { "email": "leonard@caltech.edu", "id": "Leonard-A", "name": { "family": "Leonard", "given": "Anthony" }, "role": "member" }, { "email": "fecfly@caltech.edu", "id": "Culick-F-E-C", "name": { "family": "Culick", "given": "Fred E. C." }, "role": "member" }, { "email": "ravi@caltech.edu", "id": "Ravichandran-G", "name": { "family": "Ravichandran", "given": "Guruswami" }, "role": "member" }, { "email": "lee.k.johnson@jpl.nasa.gov", "id": "Johnson-L-K", "name": { "family": "Johnson", "given": "Lee K." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-02-28", "thesis_defense_date": "2006-09-22", "thesis_approved_date": "2007-02-28", "review_status": "approved", "option_major": { "items": [ "aeronautics" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Morris, Bradford S." }, { "id": "/id/eprint/2071", "eprint_id": 2071, "rev_number": 15, "documents": [ { "id": "/id/document/3745", "doc_id": 3745, "rev_number": 3, "files": [ { "id": "/id/file/21983", "fileid": 21983, "datasetid": "document", "objectid": 3745, "filename": "main.pdf", "mime_type": "application/pdf", "filesize": 76292754, "mtime": "2012-12-26 02:46:40", "url": "/2071/1/main.pdf" } ], "eprint_id": 2071, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "main.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20411" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20411" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20411" } ] } }, { "id": "/id/document/3746", "doc_id": 3746, "rev_number": 4, "files": [ { "id": "/id/file/202459", "fileid": 202459, "datasetid": "document", "objectid": 3746, "filename": "permission.txt", "mime_type": "text/plain", "filesize": 2415, "mtime": "2016-08-22 21:15:31", "url": "/2071/2/permission.txt" } ], "eprint_id": 2071, "pos": 2, "format": "text/plain", "format_desc": "permission.txt for ApJ papers", "language": "en", "security": "internal", "license": "other", "main": "permission.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "copyright" }, { "id": "/id/document/16503", "doc_id": 16503, "rev_number": 3, "files": [ { "id": "/id/file/202460", "fileid": 202460, "datasetid": "document", "objectid": 16503, "filename": 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"security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3745" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3745" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3745" } ] } }, { "id": "/id/document/122034", "doc_id": 122034, "rev_number": 1, "files": [ { "id": "/id/file/367428", "fileid": 367428, "datasetid": "document", "objectid": 122034, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "7334ad7b3a68c6a86dbce5f0875e1969", "hash_type": "MD5", "filesize": 947, "mtime": "2021-06-23 21:44:33", "url": "/2071/6/indexcodes.txt" } ], "eprint_id": 2071, "pos": 6, "placement": 6, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3746" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3746" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3746" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/20/71", "datestamp": "2007-05-31", "lastmod": "2020-04-15 23:50:12", "status_changed": "2009-09-25 02:25:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "asoderberg@cfa.harvard.edu", "id": "Soderberg-Alicia-Margarita", "name": { "family": "Soderberg", "given": "Alicia Margarita" }, "show_email": "NO" } ] }, "title": "The Many Facets of Cosmic Explosions", "ispublished": "unpub", "full_text_status": "public", "keywords": "gamma-ray bursts; supernovae", "abstract": "Over the past few years, long-duration gamma-ray bursts (GRBs) including the subclass of X-ray flashes (XRFs) have been revealed to be a rare variety of Type Ibc supernova (SN Ibc). While all these events result from the death of massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those of ordinary Type Ibc SNe by many orders of magnitude. The observed diversity of stellar death corresponds to large variations in the energy, velocity and geometry of the explosion ejecta. Using multi-wavelength (radio, optical, X-ray) observations of the nearest GRBs, XRFs, and SNe Ibc, I show that GRBs and XRFs couple at least 1048 erg to relativistic material while SNe Ibc typically couple less than 1048 erg to their fastest (albeit non-relativistic) outflows. Specifically, I find that less than 3% of local SNe Ibc show any evidence for association with a GRB or XRF. Interestingly, this dichotomy is not echoed by the properties of their optical SN emission, dominated by the radioactive decay of Nickel-56; I find that GRBs, XRFs, and SNe Ibc show significant overlap in their optical peak luminosity and photospheric velocities. Recently, I identified a new class of GRBs and XRFs that are under-luminous in comparison with the statistical sample of GRBs. Owing to their faint high energy emission, these sub-energetic bursts are only detectable nearby (z < 0.1) and are likely 10 times more common than cosmological GRBs. In comparison with local SNe Ibc and typical GRBs/XRFs, these explosions are intermediate in terms of both volumetric rate and energetics. Yet the essential physical process that causes a dying star to produce a GRB, XRF, or sub-energetic burst, and not just a SN, remains a crucial open question. Progress requires a detailed understanding of ordinary SNe Ibc which will be facilitated with the launch of wide-field optical surveys in the near future.", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-05252007-140338", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05252007-140338", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-31", "doi": "10.7907/5f1t-7f27", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "chair" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-25", "thesis_defense_date": "2007-05-18", "thesis_approved_date": "2007-05-31", "gradofc_approval_date": "2007-05-30", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Soderberg, Alicia Margarita" }, { "id": "/id/eprint/2206", "eprint_id": 2206, "rev_number": 12, "documents": [ { "id": "/id/document/4049", "doc_id": 4049, "rev_number": 2, "files": [ { "id": "/id/file/23614", "fileid": 23614, "datasetid": "document", "objectid": 4049, "filename": "Thesis.pdf", "mime_type": "application/pdf", "filesize": 1347453, "mtime": "2012-12-26 02:48:16", "url": "/2206/1/Thesis.pdf" } ], "eprint_id": 2206, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "Thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20673" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20673" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20673" } ] } }, { "id": "/id/document/15717", "doc_id": 15717, "rev_number": 3, "files": [ { "id": "/id/file/202767", "fileid": 202767, "datasetid": "document", "objectid": 15717, "filename": "Bondarescu_Mihai_2007.PDF", "mime_type": "application/pdf", "filesize": 43033, "mtime": "2016-08-22 21:15:41", "url": "/2206/2/Bondarescu_Mihai_2007.PDF" } ], "eprint_id": 2206, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Bondarescu_Mihai_2007.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/20673", "doc_id": 20673, "rev_number": 2, "files": [ { "id": "/id/file/23612", "fileid": 23612, "datasetid": "document", "objectid": 20673, "filename": "preview.png", "mime_type": "image/png", "hash": "f244b68791a0684439d73eccb4d4bed8", "hash_type": "MD5", "filesize": 12924, "mtime": "2012-12-26 02:48:16", "url": "/2206/3/preview.png" } ], "eprint_id": 2206, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4049" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4049" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4049" } ] } }, { "id": "/id/document/122323", "doc_id": 122323, "rev_number": 1, "files": [ { "id": "/id/file/367721", "fileid": 367721, "datasetid": "document", "objectid": 122323, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "d8c26395f88e786f5278e3fea3163b36", "hash_type": "MD5", "filesize": 22836, "mtime": "2021-06-23 21:54:23", "url": "/2206/4/indexcodes.txt" } ], "eprint_id": 2206, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4049" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4049" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4049" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/22/06", "datestamp": "2007-05-31", "lastmod": "2020-03-04 22:06:42", "status_changed": "2009-09-25 02:30:34", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mihai7@gmail.com", "id": "Bondarescu-Mihai", "name": { "family": "Bondarescu", "given": "Mihai" }, "orcid": "0000-0001-8631-0146", "show_email": "YES" } ] }, "title": "Topics in General Relativity", "ispublished": "unpub", "full_text_status": "public", "keywords": "embedding; gravitational waves; LIGO; Mesa", "abstract": "This thesis is based on three of the five research projects I have worked on during my graduate student years. Each of these projects resulted in a paper a chapter of this thesis is based on. Two other papers I published during my stay at Caltech are not included, as they are not related to the research reported here.
\r\n\r\nAfter a brief introduction in the first chapter, in chapter two I discuss a simple way to greatly reduce tilt instability in Advanced LIGO by changing the mirror shape from nearly-flat previously considered mesa beams to nearly a nearly concentric shape that would provide the beam characteristics without the tilt instability. I also propose a family of hyperboloidal beams that join the nearly-flat and nearly-concentric mesa beams in a continuous manner.
\r\n\r\nIn chapter three I report the results of a recent search for the lowest value of thermal noise that can be achieved in LIGO by changing the mirror shape. I discuss in detail the beam properties and point out some of the characteristics of an advanced LIGO that uses these beams. Such an instrument, if built, would have an event rate roughly three times higher than an advanced LIGO using the Mesa beams introduced in chapter 2.
\r\n\r\nChapter four, which is also the last chapter of this thesis, is based on a Numerical Relativity project. I compute embeddings of general two-dimensional surfaces with spherical topology in flat 3D space using a minimization algorithm. The minimization problem is similar to the one solved in chapter three, albeit in a somewhat different setting.
", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-05282007-231321", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05282007-231321", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-31", "doi": "10.7907/2DKM-A388", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "barish_b@ligo.caltech.edu", "id": "Barish-B-C", "name": { "family": "Barish", "given": "Barry C." }, "role": "co-advisor" }, { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "barish_b@ligo.caltech.edu", "id": "Barish-B-C", "name": { "family": "Barish", "given": "Barry C." }, "role": "chair" }, { "email": "preskill@theory.caltech.edu", "id": "Preskill-J-P", "name": { "family": "Preskill", "given": "John P." }, "role": "member" }, { "email": "wise@theory.caltech.edu", "id": "Wise-M-B", "name": { "family": "Wise", "given": "Mark B." }, "role": "member" }, { "email": "yanbei.chen@aei.mpg.de", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-28", "thesis_defense_date": "2007-05-21", "thesis_approved_date": "2007-05-31", "gradofc_approval_date": "2007-05-30", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Bondarescu, Mihai" }, { "id": "/id/eprint/5243", "eprint_id": 5243, "rev_number": 20, "documents": [ { "id": "/id/document/8378", "doc_id": 8378, "rev_number": 3, "files": [ { "id": "/id/file/51955", "fileid": 51955, "datasetid": "document", "objectid": 8378, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 4705947, "mtime": "2012-12-26 03:16:50", "url": "/5243/1/thesis.pdf" } ], "eprint_id": 5243, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/8641" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/8641" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/8641" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/52/43", "datestamp": "2006-08-03", "lastmod": "2020-03-10 22:59:06", "status_changed": "2009-11-11 00:13:11", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yang-Min", "name": { "family": "Yang", "given": "Min" }, "show_email": "NO" } ] }, "title": "Submillimeter Surveys of Galaxy Samples", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxy; infrared; interstellar dust", "abstract": "This thesis aims to gain a better understanding of dusty galaxies by studying the thermal emission of interstellar dust at submillimeter (submm) wavelengths. We conduct 350\u03bcm observations of two galaxy samples selected based on entirely different criteria, using the Submillimeter High Angular Resolution Camera II (SHARC-II, Dowell et al. 2003) at the 10.4m Caltech Submillimeter Observatory (CSO).
\r\n\r\nThe first galaxy sample consists of 18 luminous infrared galaxies (LIGs) in the local Universe (0.003 \u2264 z \u2264 0.042). We estimate the global properties in this galaxy sample; dust temperature (Td = 38.6 \u00b1 7.7 K), emissivity index (\u03b2 = 1.6 \u00b1 0.3), far-infrared (FIR) luminosity (Lfir = 1011.2\u00b10.6 L\u2609}) and dust mass (Md = 107.4\u00b10.6 M\u2609). Guided by theoretical considerations and laboratory measurements, we derive a Td-\u03b2 inverse correlation for the local LIG sample; Td = [5.03 x 109]1/4.46 + \u03b2.
\r\n\r\nThe second galaxy sample consists of 36 ultraluminous infrared galaxies (ULIGs) at moderate redshifts (0.1 < z < 1.0), out of which 28 galaxies are detected. The newly acquired 350\u03bcm data, in combination with the pre-existing IRAS 60\u03bcm and 100\u03bcm data, leads to meaningful estimates of the global properties in these galaxies for the first time; Td = 40.9 \u00b1 6.9K, Lfir = 1012.2\u00b10.5 L\u2609, Md = 108.3\u00b10.3 M\u2609 and intense starburst activity (SFR = 102.5\u00b10.5 L\u2609 yr-1). There is strong circumstantial evidence that the Td-\u03b2 inverse correlation observed in the local LIG sample remains valid in ULIGs at moderate redshifts. We find that the FIR-radio correlation observed in local star-forming galaxies continues to hold for ULIGs over the redshift range of 0.1 < z < 1.0 and dust heating originates predominantly from star formation. Lfir and Td derived for dusty galaxy samples over a wide range of redshifts show significant scatter, due to differing selection biases and variations in dust mass and grain properties. We argue that the observed Td, as a large-scale SED parameter, is linked to the global star formation efficiency (SFE) and the spatial extent characteristic of dominant star formation in a galaxy.
", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-08012006-120712", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08012006-120712", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-08-03", "doi": "10.7907/ZTAY-AM05", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "email": "awb@phobos.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "bts@mop.caltech.edu", "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" }, { "email": "jonas@caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-08-01", "thesis_defense_date": "2006-07-31", "thesis_approved_date": "2006-08-03", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "option_minor": { "items": [ "socsci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Yang, Min" }, { "id": "/id/eprint/2340", "eprint_id": 2340, "rev_number": 10, "documents": [ { "id": "/id/document/4434", "doc_id": 4434, "rev_number": 2, "files": [ { "id": "/id/file/25570", "fileid": 25570, "datasetid": "document", "objectid": 4434, "filename": "gdb_thesis_double.pdf", "mime_type": "application/pdf", "filesize": 3279344, "mtime": "2012-12-26 02:50:15", "url": "/2340/1/gdb_thesis_double.pdf" } ], "eprint_id": 2340, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "gdb_thesis_double.pdf", "language": "en", "security": "public", "license": "other", "main": "gdb_thesis_double.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21002" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21002" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21002" } ] } }, { "id": "/id/document/13960", "doc_id": 13960, "rev_number": 3, "files": [ { "id": "/id/file/203214", "fileid": 203214, "datasetid": "document", "objectid": 13960, "filename": "Becker_George_D_2007.PDF", "mime_type": "application/pdf", "filesize": 42150, "mtime": "2016-08-22 21:15:55", "url": "/2340/2/Becker_George_D_2007.PDF" } ], "eprint_id": 2340, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Becker_George_D_2007.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/21002", "doc_id": 21002, "rev_number": 2, "files": [ { "id": "/id/file/25568", "fileid": 25568, "datasetid": "document", "objectid": 21002, "filename": "preview.png", "mime_type": "image/png", "hash": "a31e633d685b99349fd79072b2c9010a", "hash_type": "MD5", "filesize": 10809, "mtime": "2012-12-26 02:50:15", "url": "/2340/3/preview.png" } ], "eprint_id": 2340, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4434" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4434" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4434" } ] } }, { "id": "/id/document/122704", "doc_id": 122704, "rev_number": 1, "files": [ { "id": "/id/file/368102", "fileid": 368102, "datasetid": "document", "objectid": 122704, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "0f5c962fccc0e98f54f04ac0661de5c1", "hash_type": "MD5", "filesize": 28565, "mtime": "2021-06-23 22:04:45", "url": "/2340/4/indexcodes.txt" } ], "eprint_id": 2340, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4434" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4434" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4434" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/23/40", "datestamp": "2007-06-01", "lastmod": "2023-05-30 22:32:20", "status_changed": "2009-09-25 02:35:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "george.becker@ucr.edu", "id": "Becker-George-Dana", "name": { "family": "Becker", "given": "George Dana" }, "orcid": "0000-0003-2344-263X", "show_email": "YES" } ] }, "title": "A High-Resolution Study of the High-Redshift Intergalactic Medium", "ispublished": "unpub", "full_text_status": "public", "keywords": "intergalactic medium; quasar absorption lines; quasars; reionization", "abstract": "We present a study of the structure and evolution of the high-redshift intergalactic medium (IGM) using a variety of approaches based on high-resolution quasar spectra. We first use the cross-correlation of transmitted flux towards two pairs of quasars with moderate angular separation to demonstrate that filamentary structures in the IGM at z = 4 are partially coherent on roughly 1 Mpc scales. We then measure the ionization state of the high-redshift IGM using three techniques: a search for low-ionization metal lines at z > 5, an analysis of the evolution of Lyman-alpha optical depths over 2 < z < 6, and a measurement of the UV background at 4 < z < 5 using the quasar proximity effect. We identify an excess of O I systems towards the z = 6.4 quasar SDSS J1148+5251, but do not detect a \"forest\" of O I lines elsewhere that would strongly indicate the end of reionization at z = 6. Using a large sample of quasars spanning 2.0 < z < 6.4, we show that a standard Lyman-alpha optical depth distribution that assumes an isothermal IGM and uniform ionizing background produces poor fits to the observed flux distributions unless large corrections are made to the quasar continua. In contrast, an empirical lognormal optical depth distribution fits the data at all redshifts. A simple evolution of the lognormal distribution accounts for the observed mean Lyman-alpha and Lyman-beta transmitted fluxes over 1.6 < z < 6.2, which further suggests that no sudden change in the intergalactic medium such as reionization is occurring at z = 6. We measure the metagalactic UV background at 4 < z < 5 using the quasar proximity effect in a sample of 16 quasars. We combine accurate redshifts from Mg II emission and other indicators with a new method for estimating the size of a quasar's proximity region to demonstrate that the relative sizes of the proximity regions are generally consistent with the expected trend in quasar luminosity. Our estimate of the background H I ionization rate at z = 4-5 is consistent with little or no evolution from z > 2.", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-05312007-141523", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05312007-141523", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-06-01", "doi": "10.7907/TND7-F429", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "chair" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "mr@ociw.edu", "id": "Rauch-M", "name": { "family": "Rauch", "given": "Michael" }, "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" }, { "email": "esp@astro.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-31", "thesis_defense_date": "2006-07-24", "thesis_approved_date": "2007-06-01", "gradofc_approval_date": "2007-05-31", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Becker, George Dana" }, { "id": "/id/eprint/2073", "eprint_id": 2073, "rev_number": 15, "documents": [ { "id": "/id/document/3748", "doc_id": 3748, "rev_number": 2, "files": [ { "id": "/id/file/21999", "fileid": 21999, "datasetid": "document", "objectid": 3748, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 1949530, "mtime": "2012-12-26 02:46:41", "url": "/2073/1/thesis.pdf" } ], "eprint_id": 2073, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"creators": { "items": [ { "email": "owen@tapir.caltech.edu", "id": "Owen-Robert-Philip", "name": { "family": "Owen", "given": "Robert Philip" }, "show_email": "NO" } ] }, "title": "Topics in Numerical Relativity: The Periodic Standing-Wave Approximation, the Stability of Constraints in Free Evolution, and the Spin of Dynamical Black Holes", "ispublished": "unpub", "full_text_status": "public", "keywords": "approximate Killing vectors; binary black holes; constraint damping; constraint projection; hyperbolic systems", "abstract": "This thesis concerns numerical relativity, the attempt to study Einstein's theory of gravitation using numerical discretization. The goal of the field, the study of gravitational dynamics in cases where symmetry reduction or perturbation theory are not possible, finally seems to be coming to fruition, at least for the archetypal problem of the inspiral and coalescence of binary black hole systems. This thesis presents three episodes that each bear some relationship to this story.
\r\n\r\nChapters 2 and 3 present previously published work in collaboration with Richard Price and others on the so-called periodic standing-wave (PSW) approximation for binary inspiral. The approximation is to balance outgoing radiation with incoming radiation, stabilizing the orbit and making the problem stationary in a rotating frame. Chapters 2 and 3 apply the method to the problem of co-orbiting charges coupled to a nonlinear scalar field in three dimensions.
\r\n\r\nChapters 4, 5, and 6 concern the stability of constraint fields in conventional numerical relativity simulations. Chapter 4 (also previously published work, in collaboration with the Caltech numerical relativity group, along with Michael Holst and Lawrence Kidder) presents a method for immediately correcting violations of constraints after they have arisen. Chapters 5 and 6 present methods to \"damp\" away constraint violations dynamically in two specific contexts. Chapter 5 (previously published work in collaboration with the Caltech numerical relativity group and Lawrence Kidder) presents a first-order linearly degenerate symmetric hyperbolic representation of Einstein's equations in generalized harmonic gauge. A representation is presented that stabilizes all constraints, including those that appear when the system is written in first-order form. Chapter 6 presents a generalization of the Kidder-Scheel-Teukolsky evolution systems that provides much-improved stability. This is investigated with numerical simulations of a single black hole spacetime.
\r\n\r\nFinally, chapter 7 presents work in progress to implement code to calculate the spin of black holes in numerical simulations. This requires a well-defined generalization of the concept of \"rotation generators\" on topological two-spheres that may not have any true Killing vectors. I present a new method for defining these fields, and results of a numerical code that computes them.
", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-05252007-143511", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05252007-143511", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-31", "doi": "10.7907/464A-4Y76", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "advisor" }, { "id": "Price-R", "name": { "family": "Price", "given": "Richard" }, "role": "advisor" }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lindblom@tapir.caltech.edu", "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "chair" }, { "email": "Curt.J.Cutler@jpl.nasa.gov", "id": "Cutler-C-J", "name": { "family": "Cutler", "given": "Curt J." }, "role": "member" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" }, { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-25", "thesis_defense_date": "2007-05-17", "thesis_approved_date": "2007-05-31", "gradofc_approval_date": "2007-05-30", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Owen, Robert Philip" }, { "id": "/id/eprint/2508", "eprint_id": 2508, "rev_number": 10, "documents": [ { "id": "/id/document/4763", "doc_id": 4763, "rev_number": 2, "files": [ { "id": "/id/file/27479", "fileid": 27479, "datasetid": "document", "objectid": 4763, "filename": "eckart_thesis.pdf", "mime_type": "application/pdf", "filesize": 5622271, "mtime": "2012-12-26 02:52:13", "url": "/2508/1/eckart_thesis.pdf" } ], "eprint_id": 2508, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "eckart_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "eckart_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21318" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21318" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21318" } ] } }, { "id": "/id/document/15921", "doc_id": 15921, "rev_number": 3, "files": [ { "id": "/id/file/203530", "fileid": 203530, "datasetid": "document", "objectid": 15921, "filename": "Eckart_Megan_Elizabeth_2007.PDF", "mime_type": "application/pdf", "filesize": 40952, "mtime": "2016-08-22 21:16:08", "url": "/2508/2/Eckart_Megan_Elizabeth_2007.PDF" } ], "eprint_id": 2508, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Eckart_Megan_Elizabeth_2007.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/21318", "doc_id": 21318, "rev_number": 2, "files": [ { "id": "/id/file/27477", "fileid": 27477, "datasetid": "document", "objectid": 21318, "filename": "preview.png", "mime_type": "image/png", "hash": "1d906710e63b0c578937c68f9558daaf", "hash_type": "MD5", "filesize": 16310, "mtime": "2012-12-26 02:52:13", "url": "/2508/3/preview.png" } ], "eprint_id": 2508, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4763" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4763" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4763" } ] } }, { "id": "/id/document/123006", "doc_id": 123006, "rev_number": 1, "files": [ { "id": "/id/file/368408", "fileid": 368408, "datasetid": "document", "objectid": 123006, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "7b46220ab376c37de8d8414b6f97ac94", "hash_type": "MD5", "filesize": 53207, "mtime": "2021-06-23 22:14:54", "url": "/2508/4/indexcodes.txt" } ], "eprint_id": 2508, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4763" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4763" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4763" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/25/08", "datestamp": "2007-07-03", "lastmod": "2020-03-10 19:29:02", "status_changed": "2009-09-25 02:39:22", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "megan.e.eckart@nasa.gov", "id": "Eckart-Megan-Elizabeth", "name": { "family": "Eckart", "given": "Megan Elizabeth" }, "orcid": "0000-0003-3894-5889", "show_email": "YES" } ] }, "title": "Measurements of X-Ray Selected AGN and Novel Superconducting X-Ray Detectors", "ispublished": "unpub", "full_text_status": "public", "keywords": "active galactic nuclei; Chandra surveys; low temperature detectors; microwave kinetic inductance detectors; Spitzer AGN; X-ray background surveys", "abstract": "Major astrophysical advances typically come through combining new observational approaches with new technologies. This thesis involves work on both fronts, combining observational work using data from the Chandra X-ray Observatory and Keck Observatory with novel superconducting detector development to further technology for future observatories.
\r\n\r\nThe subject of the first part of this thesis is the Serendipitous Extragalactic X-ray Source Identification (SEXSI) program, a survey using Chandra data selected to probe the dominant contributors to the 2-10 keV cosmic X-ray background. SEXSI covers more than 2 square degrees of sky and employs optical photometric and spectroscopic followup of sources discovered in archival Chandra fields. The resulting sample consists of 1034 hard X-ray-selected sources with R-band optical-followup imaging, and optical spectroscopy for 477 of the sources, filling the gap between wide-area, shallow surveys and the deep, pencil-beam surveys. The vast majority of the 2-10 keV-selected sample are AGN with redshifts between 0.1 and 3. We discuss results from our survey, including the spectroscopic properties of hard X-ray sources and the relationship between X-ray and optical properties of our sources. In addition, we present infrared data from the Spitzer Space Telescope that cover a subset of the Chandra fields, which allows us to explore the relative strengths of Chandra and Spitzer as black-hole finders.
\r\n\r\nThe second part of this thesis focuses on microwave kinetic inductance detectors (MKIDs), a superconducting detector technology that has breakthrough potential for providing megapixel imagers with several eV energy resolution for use in future X-ray missions. These detectors utilize simple, thin-film lithographed microwave resonators as photon detectors in a multiplexed readout approach. X-ray absorption in a superconductor creates quasiparticle excitations, with number proportional to the X-ray energy. The surface impedance of a superconductor changes with the quasiparticle density, and if operated at T << Tc, extremely small changes in the surface impedance can be measured using the thin-film resonant circuit and microwave readout techniques. This provides a sensitive detector with excellent energy resolution.
\r\n\r\nMKIDs offer the advantage over many other cryogenic detector technologies that they can be easily multiplexed by coupling many resonators to a single microwave transmission line. In addition, the readout electronics can be operated at room temperature, a significant advantage for space applications. The practical application of MKIDs for photon detection requires a method of efficiently coupling the photon energy to the MKID. To this end we have been studying MKIDs in a strip detector architecture. The second part of this thesis presents our results using strip detectors with tantalum absorbers coupled to aluminum MKIDs.
", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-06072007-130804", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06072007-130804", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-07-03", "doi": "10.7907/SZAB-0Y07", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "role": "member" }, { "email": "golwala@caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-06-07", "thesis_defense_date": "2007-05-22", "thesis_approved_date": "2007-07-03", "gradofc_approval_date": "2007-06-29", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Eckart, Megan Elizabeth" }, { "id": "/id/eprint/1915", "eprint_id": 1915, "rev_number": 16, "documents": [ { "id": "/id/document/3292", "doc_id": 3292, "rev_number": 3, "files": [ { "id": "/id/file/19631", "fileid": 19631, "datasetid": "document", "objectid": 3292, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 1937126, "mtime": "2012-12-26 02:44:07", "url": "/1915/1/thesis.pdf" } ], "eprint_id": 1915, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19984" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19984" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19984" } ] } }, { "id": "/id/document/19984", "doc_id": 19984, "rev_number": 2, "files": [ { "id": "/id/file/19629", "fileid": 19629, "datasetid": "document", "objectid": 19984, "filename": "preview.png", "mime_type": "image/png", "hash": "097214a4b11cae1605037d410527e19c", "hash_type": "MD5", "filesize": 12625, "mtime": "2012-12-26 02:44:07", "url": "/1915/2/preview.png" } ], "eprint_id": 1915, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "validuser", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3292" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3292" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3292" } ] } }, { "id": "/id/document/121592", "doc_id": 121592, "rev_number": 1, "files": [ { "id": "/id/file/366984", "fileid": 366984, "datasetid": "document", "objectid": 121592, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "95c4974790d55ffdacea6423d3c3a217", "hash_type": "MD5", "filesize": 33574, "mtime": "2021-06-23 21:30:33", "url": "/1915/3/indexcodes.txt" } ], "eprint_id": 1915, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3292" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3292" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3292" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/19/15", "datestamp": "2007-07-05", "lastmod": "2020-03-10 23:39:05", "status_changed": "2009-09-25 02:19:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fang-Hua", "name": { "family": "Fang", "given": "Hua" }, "show_email": "NO" } ] }, "title": "Topics in Gravitational Physics: Tidal Coupling in Gravitational Wave Searches and Mach\u2019s Principle", "ispublished": "unpub", "full_text_status": "public", "keywords": " tidal couplilng; frame dragging; gravitational waves", "abstract": "The gravitational waves emitted by a compact object inspirling into a massive central body (e.g., a massive black hole) contain exquisite information about the spacetime geometry around that body and the tidal interaction (energy and angular momentum transfer) between the body and the inspiraling object's orbit. The first part (chapter 2--4) of this thesis studies several topics in the frame work of gravitation-wave search. In chapter 2 (in collaboration with G. Lovelace), we study the tidal interaction between a non-rotating black hole and circularly orbiting moon. Our analysis shows that the static induced quadrupole moment of the black hole is inherently ambiguous. In chapter 3, we give a survey of initial explorations of the prospects for using Advanced LIGO to detect gravitational waves from intermediate-mass-ratio inspirals (IMRIs))---analogous to the extreme-mass-ratio inspirals (EMRIs) targeted by LISA. We describe initial estimates of the detection range and the number of IMRI wave cycles in the Advanced LIGO band. We also give a detailed analysis of Advanced LIGO's accuracy for measuring the tide-induced energy transfer between the central black hole and the orbit. In chapter 4 (in collaboration with S. Babak, J. R. Gair, K. Glampedakis, and S. Hughes), we describe a new waveform-generating scheme in the context of LISA's data analysis for EMRI waves. The result is a family of \"Numerical Kludge\" waveforms, which share remarkable agreement with the more rigorous, but more computational-intensive Teukolsky-based waveforms.
\r\n\r\nThe second part (chapter 5) of this thesis (in collaboration with K. S. Thorne) discusses another prediction from general relativity, the dragging of inertial frames, in connection with Mach's principle. We idealize our universe as a homogeneous, isotropic expanding, and slowly rotating sphere, surrounded by vacuum. We find that as the universe expands, the frame dragging weakens at its center; and that at later times inertia at the center completely breaks free of the grip of the universe's rotating matter.
", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-05212007-004257", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05212007-004257", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12834" }, { "agency": "NASA", "grant_number": "NAG5-10707" }, { "agency": "NASA", "grant_number": "NNG04GK98G" }, { "agency": "NSF", "grant_number": "PHY-0099568" }, { "agency": "NSF", "grant_number": "PHY-0601459" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "suggestions": "Released to public view 01292018 // ", "deposited_by": "Imported from ETD-db", "deposited_on": "2007-07-05", "doi": "10.7907/D99H-J577", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "cjcutler@jpl.nasa.gov", "id": "Cutler-C-J", "name": { "family": "Cutler", "given": "Curt J." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-21", "thesis_defense_date": "2007-01-09", "thesis_approved_date": "2007-07-05", "gradofc_approval_date": "2007-05-05", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "option_minor": { "items": [ "eleceng" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Fang, Hua" }, { "id": "/id/eprint/1987", "eprint_id": 1987, "rev_number": 18, "documents": [ { "id": "/id/document/3473", "doc_id": 3473, "rev_number": 3, "files": [ { "id": "/id/file/20581", "fileid": 20581, "datasetid": "document", "objectid": 3473, "filename": "thesisSubmitted.pdf", "mime_type": "application/pdf", "filesize": 2306898, "mtime": "2012-12-26 02:45:06", "url": "/1987/1/thesisSubmitted.pdf" } ], "eprint_id": 1987, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesisSubmitted.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20148" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20148" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20148" } ] } }, { "id": "/id/document/16195", "doc_id": 16195, "rev_number": 3, "files": [ { "id": "/id/file/202253", "fileid": 202253, "datasetid": "document", "objectid": 16195, "filename": "Lovelace_Geoffrey_Mark_2007.PDF", "mime_type": "application/pdf", "filesize": 42537, "mtime": "2016-08-22 21:15:24", "url": "/1987/2/Lovelace_Geoffrey_Mark_2007.PDF" } ], "eprint_id": 1987, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Lovelace_Geoffrey_Mark_2007.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/20148", "doc_id": 20148, "rev_number": 2, "files": [ { "id": "/id/file/20579", "fileid": 20579, "datasetid": "document", "objectid": 20148, "filename": "preview.png", "mime_type": "image/png", "hash": "e5ee1db7d5e3f02b9a15a1b94dc4c930", "hash_type": "MD5", "filesize": 14184, "mtime": "2012-12-26 02:45:06", "url": "/1987/3/preview.png" } ], "eprint_id": 1987, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3473" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3473" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3473" } ] } }, { "id": "/id/document/121750", "doc_id": 121750, "rev_number": 1, "files": [ { "id": "/id/file/367142", "fileid": 367142, "datasetid": "document", "objectid": 121750, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "1419b9d69d4119ec072240dc4a5aeda5", "hash_type": "MD5", "filesize": 27961, "mtime": "2021-06-23 21:34:44", "url": "/1987/4/indexcodes.txt" } ], "eprint_id": 1987, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3473" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3473" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3473" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/19/87", "datestamp": "2007-05-29", "lastmod": "2020-09-01 22:37:20", "status_changed": "2009-09-25 02:22:04", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "geoffrey4444@gmail.com", "id": "Lovelace-Geoffrey-Mark", "name": { "family": "Lovelace", "given": "Geoffrey Mark" }, "orcid": "0000-0002-7084-1070", "show_email": "YES" } ] }, "title": "Topics in Gravitational-Wave Physics", "ispublished": "unpub", "full_text_status": "public", "keywords": "Advanced LIGO; black holes; gravitational waves; initial data for binary black holes; numerical relativity; tidal coupling", "abstract": "Together with ongoing experimental efforts to detect gravitational waves, several fronts of theoretical research are presently being pursued, including second-generation detector design, data analysis, and numerical-relativity simulations of sources. This thesis presents a study in each of these topics: i) The noise in the most sensitive frequency bands in second-generation ground-based gravitational-wave interferometers is dominated by the thermal noise of the test masses. One way to reduce test-mass thermal noise is to modify shape of the laser beam so that it better averages over the thermal fluctuations. When edge effects are neglected, the test-mass thermal noise is related to the beam shape by simple scaling laws. This thesis presents a rigorous derivation of these laws, along with estimates of the errors made by neglecting edge effects. ii) An important class of gravitational-wave sources for space-based gravitational-wave interferometers is extreme-mass-ratio inspirals (EMRIs). These are binaries in which an object of a few solar masses spirals into a (typically million-solar-mass) supermassive black hole (or, if any exist, other type of massive body). Ryan (1995) proved that, under certain simplifying assumptions, the spacetime geometry is redundantly encoded in EMRI waves. One of Ryan's assumptions was negligible tidal coupling. After first finding that only the time-varying part of the induced tide is unambiguously defined when the central body is a black hole, this thesis extends Ryan's theorem by showing that both the spacetime geometry and details of the tidal coupling are encoded in EMRI waves. iii) Merging black holes with comparable masses are important sources of gravitational waves for ground-based detectors. The gravitational waves near the time of merger can only be predicted by numerically solving the Einstein equations. Initial data in numerical simulations must contain the desired physical content but also satisfy the Einstein constraint equations. But conventional binary-black-hole initial data has physical flaws: a nonzero orbital eccentricity and an initial, unphysical pulse of spurious gravitational radiation. Using the Caltech-Cornell pseudospectral code, this thesis develops and implements methods to reduce both of these effects.
", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-05232007-115433", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05232007-115433", "related_url": { "items": [ { "description": "Article adapted for Ch.2.", "type": "doi", "url": "https://doi.org/10.1088/0264-9381/24/17/014" }, { "description": "Article adapted for Ch.3.", "type": "doi", "url": "https://doi.org/10.1103/physrevd.72.124016" }, { "description": "Article adapted for Ch.4.", "type": "doi", "url": "https://doi.org/10.1103/physrevd.77.064022" }, { "description": "Article adapted for Ch.5.", "type": "doi", "url": "https://doi.org/10.1088/0264-9381/24/12/s06" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12834" }, { "agency": "NASA", "grant_number": "NAG5-10707" }, { "agency": "NASA", "grant_number": "NNG04GK98G" }, { "agency": "NASA", "grant_number": "NNG05GG52G" }, { "agency": "NASA", "grant_number": "NNG05GG51G" }, { "agency": "NSF", "grant_number": "PNY-0099568" }, { "agency": "NSF", "grant_number": "PHY-0601459" }, { "agency": "NSF", "grant_number": "PHY-0244906" }, { "agency": "NSF", "grant_number": "DMS-0553302" }, { "agency": "NSF", "grant_number": "PHY-0312072" }, { "agency": "NSF", "grant_number": "PHY-0354631" }, { "agency": "Sherman Fairchild Foundation" }, { "agency": "Brinson Foundation" }, { "agency": "NSF", "grant_number": "PHY-0107417" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department", "LIGO" ] }, "suggestions": "glovelace@fullerton.edu", "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-29", "doi": "10.7907/94TE-3B59", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" }, { "email": "lindblom@tapir.caltech.edu", "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-23", "thesis_defense_date": "2007-05-14", "thesis_approved_date": "2007-05-29", "gradofc_approval_date": "2007-05-24", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Lovelace, Geoffrey Mark" }, { "id": "/id/eprint/444", "eprint_id": 444, "rev_number": 12, "documents": [ { "id": "/id/document/670", "doc_id": 670, "rev_number": 2, "files": [ { "id": "/id/file/4236", "fileid": 4236, "datasetid": "document", "objectid": 670, "filename": "Thesis_Li_Final.pdf", "mime_type": "application/pdf", "filesize": 6425083, "mtime": "2012-12-26 02:29:51", "url": "/444/1/Thesis_Li_Final.pdf" } ], "eprint_id": 444, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thesis_Li_Final.pdf", "language": "en", "security": "public", "license": "other", "main": "Thesis_Li_Final.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17496" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17496" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17496" } ] } }, { "id": "/id/document/16159", "doc_id": 16159, "rev_number": 3, "files": [ { "id": "/id/file/200122", "fileid": 200122, "datasetid": "document", "objectid": 16159, "filename": "Li_Liming_2007.PDF", "mime_type": "application/pdf", "filesize": 42052, "mtime": "2016-08-22 21:14:05", "url": "/444/2/Li_Liming_2007.PDF" } ], "eprint_id": 444, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Li_Liming_2007.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/17496", "doc_id": 17496, "rev_number": 2, "files": [ { "id": "/id/file/4234", "fileid": 4234, "datasetid": "document", "objectid": 17496, "filename": "preview.png", "mime_type": "image/png", "hash": "5bad739afad3978b951932c042abbcf8", "hash_type": "MD5", "filesize": 17975, "mtime": "2012-12-26 02:29:51", "url": "/444/3/preview.png" } ], "eprint_id": 444, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/670" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/670" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/670" } ] } }, { "id": "/id/document/119929", "doc_id": 119929, "rev_number": 1, "files": [ { "id": "/id/file/365298", "fileid": 365298, "datasetid": "document", "objectid": 119929, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "d565988792f13e7263083c99b9c83410", "hash_type": "MD5", "filesize": 19546, "mtime": "2021-06-23 20:27:10", "url": "/444/4/indexcodes.txt" } ], "eprint_id": 444, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/670" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/670" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/670" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/04/44", "datestamp": "2007-02-12", "lastmod": "2020-03-11 18:43:01", "status_changed": "2009-09-25 01:37:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "lli7@central.uh.edu", "id": "Li-Liming", "name": { "family": "Li", "given": "Liming" }, "orcid": "0000-0002-5257-9849", "show_email": "YES" } ] }, "title": "Dynamics of the Jovian Atmosphere from Observation and Theory", "ispublished": "unpub", "full_text_status": "public", "keywords": "Moist convection; Wave; Zonal jets", "abstract": "The atmospheric dynamics of Jupiter is studied by the Cassini observations and numerical models.
\r\n\r\nThe multi-filter imaging data sets and the global thermal maps acquired by two instruments on Cassini--the Imaging Science Subsystem (ISS) and the Cassini Composite Infrared Spectrometer (CIRS) during the Jupiter flyby, are utilized to study atmospheric activities on Jupiter including small-scale spots, the Great Red Spot (GRS), the Dark Oval (DO), the vertical structure of zonal winds, and wave propagation. These new observations enrich the library of atmospheric activities and offer more clues and constraints on theoretical studies.
\r\n\r\nA reduced-gravity quasi-geostrophic (QG) model is combined with a parameterization of moist convections based on observations, to study the interaction between moist convection and zonal jets on Jupiter and Saturn. The numerical experiments support the idea that the zonal jets get their energy from moist convective events. Strong jets in Jupiter and Saturn, which violate the barotropic stability criterion, are reproduced by assuming westward flows in the deep underlying layer. Furthermore, our simulations suggest that the width and strength of jets on Jupiter and Saturn are controlled by the classical Rhines scale and a new velocity scale determined by characteristics of moist convection.
", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-02012007-204746", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-02012007-204746", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-02-12", "doi": "10.7907/6DAY-FJ03", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "burnett@gps.caltech.edu", "id": "Burnett-D-S", "name": { "family": "Burnett", "given": "Donald S." }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "email": "mir@gps.caltech.edu", "id": "Richardson-M-I", "name": { "family": "Richardson", "given": "Mark I." }, "role": "member" }, { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-02-01", "thesis_defense_date": "2006-09-08", "thesis_approved_date": "2007-02-12", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2007", "author_list": "Li, Liming" }, { "id": "/id/eprint/3380", "eprint_id": 3380, "rev_number": 16, "documents": [ { "id": "/id/document/5910", "doc_id": 5910, "rev_number": 3, "files": [ { "id": "/id/file/35139", "fileid": 35139, "datasetid": "document", "objectid": 5910, "filename": "main.pdf", "mime_type": "application/pdf", "filesize": 14019184, "mtime": "2012-12-26 02:59:30", "url": "/3380/1/main.pdf" } ], "eprint_id": 3380, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "main.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22450" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22450" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22450" } ] } }, { "id": "/id/document/15936", "doc_id": 15936, "rev_number": 3, "files": [ { "id": "/id/file/204067", "fileid": 204067, "datasetid": "document", "objectid": 15936, "filename": "Erb_Dawn_K_2006.PDF", "mime_type": "application/pdf", "filesize": 43726, "mtime": "2016-08-22 21:16:42", "url": "/3380/2/Erb_Dawn_K_2006.PDF" } ], "eprint_id": 3380, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Erb_Dawn_K_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/22450", "doc_id": 22450, "rev_number": 2, "files": [ { "id": "/id/file/35137", "fileid": 35137, "datasetid": "document", "objectid": 22450, "filename": "preview.png", "mime_type": "image/png", "hash": "71f151ff0a8a55cc74f279bc9c7e6b93", "hash_type": "MD5", "filesize": 11743, "mtime": "2012-12-26 02:59:30", "url": "/3380/3/preview.png" } ], "eprint_id": 3380, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5910" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5910" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5910" } ] } }, { "id": "/id/document/123576", "doc_id": 123576, "rev_number": 1, "files": [ { "id": "/id/file/368998", "fileid": 368998, "datasetid": "document", "objectid": 123576, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "42d7d70bb2b07129aa1e4b9629ae16a9", "hash_type": "MD5", "filesize": 32293, "mtime": "2021-06-23 22:46:57", "url": "/3380/4/indexcodes.txt" } ], "eprint_id": 3380, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5910" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5910" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5910" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/80", "datestamp": "2005-09-12", "lastmod": "2020-03-31 22:04:14", "status_changed": "2009-09-25 02:57:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "erbd@uwm.edu", "id": "Erb-Dawn-Karuna", "name": { "family": "Erb", "given": "Dawn Karuna" }, "orcid": "0000-0001-9714-2758", "show_email": "NO" } ] }, "title": "The Properties of Star-Forming Galaxies at z ~ 2: Kinematics, Stellar Populations, and Metallicities", "ispublished": "unpub", "full_text_status": "public", "keywords": "High redshift galaxies", "abstract": "We study the properties of star-forming galaxies at redshift z ~ 2, an era in which a substantial fraction of the stellar mass in the universe formed. Using 114 near-IR spectra of the H\u03b1 and [N II] emission lines and model spectral energy distributions fit to rest-frame UV through IR photometry, we examine the galaxies' star formation properties, dynamical masses and velocity dispersions, spatially resolved kinematics, outflow properties, and metallicities as a function of stellar mass and age. While the stellar masses of the galaxies in our sample vary by a factor of ~ 500, dynamical masses from H\u03b1 velocity dispersions and indirect estimates of gas masses imply that the variation of stellar mass is due as much to the evolution of the stellar population and the conversion of gas into stars as to intrinsic differences in the total masses of the galaxies. About 10% of the galaxies are apparently young starbursts with high gas fractions, caught just as they have begun to convert large amounts of gas into stars. Using the [N II]/H\u03b1 ratio of composite spectra to estimate the average oxygen abundance, we find a monotonic increase in metallicity with stellar mass. From the estimated gas fractions, we conclude that the increase in metallicity as gas is converted to stars is more likely to explain the observed mass-metallicity relation than the loss of metals through outflows. The picture that emerges is of galaxies with a broad range in stellar population properties, from young galaxies with ages of a few tens of Myr, stellar masses M* ~ 10\u2079 M\u2299, and metallicities Z ~ 1/3 Z\u2299, to massive objects with M* ~ 10\u00b9\u00b9 M\u2299, Z ~ Z\u2299, and ages as old as the universe allows. All, however, are rapidly star-forming, power galactic-scale outflows, and have masses in gas and stars of at least ~ 10\u00b9\u2070 M\u2299, in keeping with their likely role as the progenitors of elliptical galaxies seen today.
", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-09082005-113029", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082005-113029", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/375316" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1086/422464" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-09-12", "doi": "10.7907/C5D0-7789", "alt_title": { "items": [ "The Properties of Star-Forming Galaxies at z ~ 2", "Kinematics, Stellar Populations, and Metallicities" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "kamion@tapir.caltech.edy", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-09-08", "thesis_defense_date": "2005-08-03", "thesis_approved_date": "2005-09-12", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Erb, Dawn Karuna" }, { "id": "/id/eprint/3730", "eprint_id": 3730, "rev_number": 11, "documents": [ { "id": "/id/document/6346", "doc_id": 6346, "rev_number": 3, "files": [ { "id": "/id/file/38080", "fileid": 38080, "datasetid": "document", "objectid": 6346, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 17984452, "mtime": "2012-12-26 03:02:29", "url": "/3730/1/thesis.pdf" } ], "eprint_id": 3730, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22884" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22884" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22884" } ] } }, { "id": "/id/document/13955", "doc_id": 13955, "rev_number": 3, "files": [ { "id": "/id/file/204150", "fileid": 204150, "datasetid": "document", "objectid": 13955, "filename": "Basu_Shabari_2006.PDF", "mime_type": "application/pdf", "filesize": 44091, "mtime": "2016-08-22 21:16:55", "url": "/3730/2/Basu_Shabari_2006.PDF" } ], "eprint_id": 3730, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Basu_Shabari_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/22884", "doc_id": 22884, "rev_number": 2, "files": [ { "id": "/id/file/38078", "fileid": 38078, "datasetid": "document", "objectid": 22884, "filename": "preview.png", "mime_type": "image/png", "hash": "52816b8985cd493693ab899dd6b679a2", "hash_type": "MD5", "filesize": 12590, "mtime": "2012-12-26 03:02:29", "url": "/3730/3/preview.png" } ], "eprint_id": 3730, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6346" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6346" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6346" } ] } }, { "id": "/id/document/123808", "doc_id": 123808, "rev_number": 1, "files": [ { "id": "/id/file/369236", "fileid": 369236, "datasetid": "document", "objectid": 123808, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "dd89512b0f33387c271e5191fa72703b", "hash_type": "MD5", "filesize": 29815, "mtime": "2021-06-23 22:59:53", "url": "/3730/4/indexcodes.txt" } ], "eprint_id": 3730, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6346" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6346" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/6346" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/30", "datestamp": "2005-11-09", "lastmod": "2020-03-31 19:24:01", "status_changed": "2009-09-25 03:04:18", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Basu-Shabari", "name": { "family": "Basu", "given": "Shabari" }, "show_email": "NO" } ] }, "title": "Simulations of the Martian Dust Cycle with a General Circulation Model", "ispublished": "unpub", "full_text_status": "public", "keywords": "dust cycle; general circulation model; Mars", "abstract": "The Martian seasonal dust cycle is examined with a General Circulation Model (GCM) that treats dust as a radiatively and dynamically interactive trace species. Dust injection is parameterized as being due to convective processes (such as dust devils) and model-resolved wind stresses. Multi-year Viking and Mars Global Surveyor mission air temperature data sets are used to quantitatively assess the quality of simulations. Varying the three free parameters for the two dust injection schemes (rate parameters for the two schemes and a threshold for wind-stress lifting), we find that northern spring and summer temperatures, which are observed to repeat very closely each year, can be reproduced by the model if the background dust haze is supplied by convective lifting. To obtain spontaneous and variable dust storms, dust injection due to high threshold and high rate stress lifting must be added. The convective scheme is found unable to generate a dust storm but is a good candidate for background dust (in agreement with imaging observations e.g., dust devils). Combining the convective scheme and high-threshold stress lifting, we obtain a \"best fit\" multi-year simulation, which includes simulation of both a realistic thermal state in northern spring and summer and, for the first time, the spontaneous generation of inter-annually-variable global dust storms. Our results support the idea that variable and spontaneous global dust storm behavior can emerge from a periodically forced system (the only forcing being the diurnal and seasonal cycles) when the dust injection mechanism involves an activation threshold. The general circulation model is also used to evaluate changes to the circulation and dust transport in the Martian atmosphere for simulations with a finite supply of dust on the surface. The focus is on changes to atmospheric temperatures and dust-related surface features, as these may potentially be verified by observations. In this work, the use of a finite surface dust supply increases the amount of inter-annual variability the system is capable of producing. This is due to a new set of initial conditions, in the form of available surface dust, being present at the beginning of each storm season.", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-09232005-154100", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232005-154100", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-11-09", "doi": "10.7907/BDB8-Z423", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mir@gps.caltech.edu", "id": "Richardson-M-I", "name": { "family": "Richardson", "given": "Mark I." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mir@gps.caltech.edu", "id": "Richardson-M-I", "name": { "family": "Richardson", "given": "Mark I." }, "role": "chair" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-09-23", "thesis_defense_date": "2005-09-21", "thesis_approved_date": "2005-11-09", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Basu, Shabari" }, { "id": "/id/eprint/2058", "eprint_id": 2058, "rev_number": 9, "documents": [ { "id": "/id/document/3716", "doc_id": 3716, "rev_number": 3, "files": [ { "id": "/id/file/21822", "fileid": 21822, "datasetid": "document", "objectid": 3716, "filename": "mpan.pdf", "mime_type": "application/pdf", "filesize": 4672868, "mtime": "2012-12-26 02:46:30", "url": "/2058/1/mpan.pdf" } ], "eprint_id": 2058, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "mpan.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20384" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20384" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20384" } ] } }, { "id": "/id/document/16355", "doc_id": 16355, "rev_number": 3, "files": [ { "id": "/id/file/202420", "fileid": 202420, "datasetid": "document", "objectid": 16355, "filename": "Pan_Margaret_Whei-Jie_2006.PDF", "mime_type": "application/pdf", "filesize": 43355, "mtime": "2016-08-22 21:15:30", "url": "/2058/2/Pan_Margaret_Whei-Jie_2006.PDF" } ], "eprint_id": 2058, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Pan_Margaret_Whei-Jie_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/20384", "doc_id": 20384, "rev_number": 2, "files": [ { "id": "/id/file/21820", "fileid": 21820, "datasetid": "document", "objectid": 20384, "filename": "preview.png", "mime_type": "image/png", "hash": "d83ae147a75f3dfd173f553b95f4a81d", "hash_type": "MD5", "filesize": 20567, "mtime": "2012-12-26 02:46:30", "url": "/2058/3/preview.png" } ], "eprint_id": 2058, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3716" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3716" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3716" } ] } }, { "id": "/id/document/122001", "doc_id": 122001, "rev_number": 1, "files": [ { "id": "/id/file/367395", "fileid": 367395, "datasetid": "document", "objectid": 122001, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "1517a9f05df9490fcdafbb243c0ee0f4", "hash_type": "MD5", "filesize": 18439, "mtime": "2021-06-23 21:43:19", "url": "/2058/4/indexcodes.txt" } ], "eprint_id": 2058, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3716" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3716" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3716" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/20/58", "datestamp": "2006-06-02", "lastmod": "2020-04-08 18:46:47", "status_changed": "2009-09-25 02:24:52", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pan-Margaret-Whei-Jie", "name": { "family": "Pan", "given": "Margaret Whei-Jie" }, "show_email": "NO" } ] }, "title": "Slices of Theoretical Astrophysics: Solar System Dynamics and Relativistic Explosions", "ispublished": "unpub", "full_text_status": "public", "keywords": "collisional cascades; planetary dynamics; relativistic shocks; similarity solutions", "abstract": "This thesis presents studies in two distinct areas of theoretical astrophysics: dynamics of planetary systems and relativistic fluid flows from shocks emerging from stellar envelopes. The first pertains to the early solar system, planet formation, and extrasolar planets; the second is related to extreme explosions like gamma-ray bursts and supernovae.
\r\n\r\nWe present two investigations of the dynamics and population evolution of small solar system bodies. First, we explore the dynamics of mean-motion resonances for a test particle moving in a highly eccentric long-period orbit in the restricted circular planar three-body problem --- a scenario relevant to the scattered Kuiper belt and the formation of the Oort cloud. We find an infinite number of analogues to the Lagrange points; a simple explanation for the presence and absence of asymmetric librations in particular mean-motion resonances; and a criterion for the onset of chaotic motion at large semimajor axes.
\r\n\r\nSecond, we study the size distribution of Kuiper belt objects (KBOs), which is observed to be a broken power law. We apply a simple mass conservation argument to the KBO collisional cascade to get the power-law slope for KBOs below the break; our result agrees well with observations if we assume KBOs are held together by self-gravity rather than material strength. We also explain the location and time evolution of the break in the size distribution.
\r\n\r\nWe also present investigations of the flow which results when a relativistic shock propagates through and then breaks out of a stellar envelope with a polytropic density profile. This work informs predictions of the speed of and energy carried by the relativistic ejecta in supernovae and perhaps in gamma-ray bursts. We find the asymptotic solution for the flow as the shock reaches the star's edge and find a new self-similar solution for flow of hot fluid after the shock breakout. Since the post-breakout flow acclerates by converting its thermal energy into bulk kinetic energy, the fluid in the flow eventually cools to non-relativistic temperatures. We derive a second new self-similar solution which includes the cold portions of the flow. This second solution gives an exact relation between the terminal Lorentz factor of each fluid element and the Lorentz factor it acquired upon being shocked before breakout.
", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-05252006-181025", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05252006-181025", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-06-02", "doi": "10.7907/40AE-N743", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "chair" }, { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "member" }, { "email": "nzs@radio.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "email": "pmg@tapir.caltech.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-05-25", "thesis_defense_date": "2006-05-23", "thesis_approved_date": "2006-06-02", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Pan, Margaret Whei-Jie" }, { "id": "/id/eprint/1595", "eprint_id": 1595, "rev_number": 19, "documents": [ { "id": "/id/document/2496", "doc_id": 2496, "rev_number": 3, "files": [ { "id": "/id/file/15395", "fileid": 15395, "datasetid": "document", "objectid": 2496, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 1838614, "mtime": "2012-12-26 02:39:43", "url": "/1595/1/thesis.pdf" } ], "eprint_id": 1595, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19236" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19236" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19236" } ] } }, { "id": "/id/document/16162", "doc_id": 16162, "rev_number": 3, "files": [ { "id": "/id/file/201520", "fileid": 201520, "datasetid": "document", "objectid": 16162, "filename": "Liang_Mao-Chang_2006.PDF", "mime_type": "application/pdf", "filesize": 40629, "mtime": "2016-08-22 21:14:59", "url": "/1595/2/Liang_Mao-Chang_2006.PDF" } ], "eprint_id": 1595, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Liang_Mao-Chang_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/19236", "doc_id": 19236, "rev_number": 2, "files": [ { "id": "/id/file/15393", "fileid": 15393, "datasetid": "document", "objectid": 19236, "filename": "preview.png", "mime_type": "image/png", "hash": "dea7a944e79cd49eda4cd844663b74e4", "hash_type": "MD5", "filesize": 20962, "mtime": "2012-12-26 02:39:43", "url": "/1595/3/preview.png" } ], "eprint_id": 1595, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2496" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2496" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2496" } ] } }, { "id": "/id/document/120963", "doc_id": 120963, "rev_number": 1, "files": [ { "id": "/id/file/366351", "fileid": 366351, "datasetid": "document", "objectid": 120963, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "076478cef8271ff240edff68df94929a", "hash_type": "MD5", "filesize": 32659, "mtime": "2021-06-23 21:11:19", "url": "/1595/4/indexcodes.txt" } ], "eprint_id": 1595, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2496" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2496" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2496" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/95", "datestamp": "2006-05-15", "lastmod": "2023-11-08 00:36:10", "status_changed": "2009-09-25 02:08:47", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mcl@gate.sinica.edu.tw", "id": "Liang-Mao-Chang", "name": { "family": "Liang", "given": "Mao-Chang" }, "orcid": "0000-0002-5294-9344", "show_email": "YES" } ] }, "title": "Chemical and Dynamical Processes in the Atmospheres of I. Ancient and Present-Day Earth, II. Jupiter and Galileo Satellite, III. Extrasolar \u201cHot Jupiters\u201d", "ispublished": "unpub", "full_text_status": "public", "keywords": "atmosphere; dynamics; photochemistry; planet; radiative transfer", "abstract": "When exposed to stellar UV radiation, chemical processes will be governed not only by temperature/pressure but also the spectrum of the incoming dissociative photon flux; the system will approach kinetic, or photochemical, equilibrium, instead of thermochemical equilibrium. Over the previous decades, photochemistry has proven to be a powerful tool for predicting the chemical composition in the atmospheres of solar planets and their satellites. For example, the ozone layer in our own atmosphere (stratosphere) is a photochemical product of oxygen. In this thesis, I apply a photochemical model to the study of a variety of astronomical objects: the Earth, Jupiter, the Galilean satellite Callisto, and extrasolar \"hot Jupiters\" (HD 209458b). For the Earth, a method for utilizing the isotopic composition of CO2 and N2O to monitor global changes due to these two greenhouse gases is developed. For objects other than the Earth, the model facilitates in the interpretation of data acquired by remote (telescopic) and in situ (spacecraft) measurements. The ultimate goal is to understand the conditions of chemical and physical environments in protoplanetary nebulae, which will provide clues as to the formation of planetary systems; the synthesis of organic compounds which could lead to the appearance of life; and the evolution of planetary atmospheres such as the formation of Titan's nitrogen-rich atmosphere.", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-05032006-214832", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05032006-214832", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-05-15", "doi": "10.7907/8HSF-CA03", "alt_title": { "items": [ "Ancient and Present-Day Earth", "Jupiter and Galileo Satellite", "Extrasolar \u201cHot Jupiters\u201d" ] }, "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "advisor" }, { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "orcid": "0000-0002-1084-3656", "role": "member" }, { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-05-03", "thesis_defense_date": "2005-11-07", "thesis_approved_date": "2006-05-15", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Liang, Mao-Chang" }, { "id": "/id/eprint/3229", "eprint_id": 3229, "rev_number": 12, "documents": [ { "id": "/id/document/5720", "doc_id": 5720, "rev_number": 2, "files": [ { "id": "/id/file/33871", "fileid": 33871, "datasetid": "document", "objectid": 5720, "filename": "Metchev_Thesis.pdf", "mime_type": "application/pdf", "filesize": 8334006, "mtime": "2012-12-26 02:58:16", "url": "/3229/1/Metchev_Thesis.pdf" } ], "eprint_id": 3229, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Metchev_Thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "Metchev_Thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22262" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22262" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22262" } ] } }, { "id": "/id/document/16262", "doc_id": 16262, "rev_number": 3, "files": [ { "id": "/id/file/204029", "fileid": 204029, "datasetid": "document", "objectid": 16262, "filename": "Metchev_Stanimir_Angelov_2006.PDF", "mime_type": "application/pdf", "filesize": 46542, "mtime": "2016-08-22 21:16:37", "url": "/3229/2/Metchev_Stanimir_Angelov_2006.PDF" } ], "eprint_id": 3229, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Metchev_Stanimir_Angelov_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/22262", "doc_id": 22262, "rev_number": 2, "files": [ { "id": "/id/file/33869", "fileid": 33869, "datasetid": "document", "objectid": 22262, "filename": "preview.png", "mime_type": "image/png", "hash": "3b2492e1cfbb0fb8a3da8eefa5399905", "hash_type": "MD5", "filesize": 12365, "mtime": "2012-12-26 02:58:16", "url": "/3229/3/preview.png" } ], "eprint_id": 3229, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5720" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5720" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5720" } ] } }, { "id": "/id/document/123476", "doc_id": 123476, "rev_number": 1, "files": [ { "id": "/id/file/368889", "fileid": 368889, "datasetid": "document", "objectid": 123476, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "ca21d5fe155b9d3872a9f4ec75e3215e", "hash_type": "MD5", "filesize": 51732, "mtime": "2021-06-23 22:41:09", "url": "/3229/4/indexcodes.txt" } ], "eprint_id": 3229, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5720" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5720" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5720" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/29", "datestamp": "2005-08-29", "lastmod": "2023-05-30 22:16:34", "status_changed": "2009-09-25 02:54:53", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "smetchev@uwo.ca", "id": "Metchev-Stanimir-Angelov", "name": { "family": "Metchev", "given": "Stanimir Angelov" }, "orcid": "0000-0003-3050-8203", "show_email": "YES" } ] }, "title": "Brown Dwarf Companions to Young Solar Analogs: An Adaptive Optics Survey Using Palomar and Keck", "ispublished": "unpub", "full_text_status": "public", "keywords": "adaptive optics astrometry; sub-stellar companions; sub-stellar multiplicity; ultra-cool dwarfs; young brown dwarfs", "abstract": "We present results from an adaptive optics survey conducted with the Palomar and Keck telescopes over 3 years, which measured the frequency of stellar and sub-stellar companions to Sun-like stars. The survey sample contains 266 stars in the 3-10000 million year age range at heliocentric distances between 8 and 200 parsecs and with spectral types between F5-K5. A sub-sample of 101 stars, between 3-500 million years old, were observed in deep exposures with a coronagraph to search for faint sub-stellar companions. A total of 288 candidate companions were discovered around the sample stars, which were re-imaged at subsequent epochs to determine physical association with the candidate host stars by checking for common proper motion. Benefiting from a highly accurate astrometric calibration of the observations, we were able to successfully apply the common proper motion test in the majority of the cases, including stars with proper motions as small as 20 milli-arcseconds/year.
\r\n\r\nThe results from the survey include the discovery of three new brown dwarf companions (HD 49197B, HD 203030B, and ScoPMS 214B), 43 new stellar binaries, and a triple system. The physical association of an additional, a priori-suspected, candidate sub-stellar companion to the star HII 1348 is astrometrically confirmed. The newly-discovered and confirmed young brown dwarf companions span a range of spectral types between M5 and T0.5, and will be of prime significance for constraining evolutionary models of young brown dwarfs and extra-solar planets.
\r\n\r\nBased on the 3 new detections of sub-stellar companions in the 101 star sub-sample and following a careful estimate of the survey incompleteness, a Bayesian statistical analysis shows that the frequency of 0.012-0.072 solar-mass brown dwarfs in 30-1600 AU orbits around young solar analogs is 6.8% (-4.9%, +8.3\\%; 2-sigma limits). While this is a factor of 3 lower than the frequency of stellar companions to G-dwarfs in the same orbital range, it is significantly higher than the frequency of brown dwarfs in 0-3 AU orbits discovered through precision radial velocity surveys. It is also fully consistent with the observed frequency of 0-3 AU extra-solar planets. Thus, the result demonstrates that the radial-velocity \"brown dwarf desert\" does not extend to wide separations, contrary to previous belief.
", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-08262005-170055", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08262005-170055", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-08-29", "doi": "10.7907/ZGB1-CY59", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "chair" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "rgd@astro.caltech.edu", "id": "Dekany-R-G", "name": { "family": "Dekany", "given": "Richard G." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-08-26", "thesis_defense_date": "2005-08-18", "thesis_approved_date": "2005-08-29", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Metchev, Stanimir Angelov" }, { "id": "/id/eprint/1846", "eprint_id": 1846, "rev_number": 21, "documents": [ { "id": "/id/document/3075", "doc_id": 3075, "rev_number": 2, "files": [ { "id": "/id/file/18509", "fileid": 18509, "datasetid": "document", "objectid": 3075, "filename": "nar_thesis.pdf", "mime_type": "application/pdf", "filesize": 4726628, "mtime": "2012-12-26 02:42:56", "url": "/1846/1/nar_thesis.pdf" } ], "eprint_id": 1846, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "nar_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "nar_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19776" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19776" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19776" } ] } }, { "id": "/id/document/16402", "doc_id": 16402, "rev_number": 3, "files": [ { "id": "/id/file/201866", "fileid": 201866, "datasetid": "document", "objectid": 16402, "filename": "Reddy_Naveen_Ananta_2006.PDF", "mime_type": "application/pdf", "filesize": 41073, "mtime": "2016-08-22 21:15:11", "url": "/1846/2/Reddy_Naveen_Ananta_2006.PDF" } ], "eprint_id": 1846, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Reddy_Naveen_Ananta_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/19776", "doc_id": 19776, "rev_number": 2, "files": [ { "id": "/id/file/18507", "fileid": 18507, "datasetid": "document", "objectid": 19776, "filename": "preview.png", "mime_type": "image/png", "hash": "44886a8e5ac522cb2cb694016f74d11d", "hash_type": "MD5", "filesize": 10791, "mtime": "2012-12-26 02:42:56", "url": "/1846/3/preview.png" } ], "eprint_id": 1846, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3075" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3075" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3075" } ] } }, { "id": "/id/document/121374", "doc_id": 121374, "rev_number": 1, "files": [ { "id": "/id/file/366766", "fileid": 366766, "datasetid": "document", "objectid": 121374, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "6474171c9f64cf1a89adf4112b23134c", "hash_type": "MD5", "filesize": 36882, "mtime": "2021-06-23 21:25:09", "url": "/1846/4/indexcodes.txt" } ], "eprint_id": 1846, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3075" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3075" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3075" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/18/46", "datestamp": "2006-05-22", "lastmod": "2020-02-19 23:27:06", "status_changed": "2009-09-25 02:17:29", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "naveen.reddy@ucr.edu", "id": "Reddy-Naveen-Ananta", "name": { "family": "Reddy", "given": "Naveen Ananta" }, "orcid": "0000-0001-9687-4973", "show_email": "YES" } ] }, "title": "A Multi-Wavelength Census of Star Formation at Redshift z ~ 2", "ispublished": "unpub", "full_text_status": "public", "keywords": "High redshift galaxies", "note": "Title listed in 2006 commencement program -- A Multi-Wavelength Census of Star Formation at Redshifts z Equals 2 -- differs from title listed in thesis file (PDF).", "abstract": "We examine the census of star-forming galaxies and their extinction properties at redshift z ~ 2, when a large fraction of the stellar mass in the universe formed. We find a good agreement between the X-ray, radio, and de-reddened UV estimates of the average star formation rate (SFR) for our sample of z ~ 2 galaxies of ~ 50 M\u2299 yr\u207b\u00b9, indicating that the locally calibrated SFR relations appear to be statistically valid from redshifts 1.5 \u227e z \u227e 3.0. Spitzer MIPS data are used to assess the extinction properties of individual star-forming galaxies, and we find that the rest-frame UV slope of most galaxies at z ~ 2 can be used to infer their attenuation factors, Lbol/LUV. As in the local universe, the obscuration, LFIR/LUV is strongly dependent on bolometric luminosity, and ranges in value from < 1 to ~ 1000 within the sample considered. However, the obscuration is ~ 10 times smaller at a given Lbol (or, equivalently, a similar level of obscuration occurs at luminosities ~ 10 times larger) at z ~ 2 than at z ~ 0. This trend is expected as galaxies age and their gas becomes more dust-enriched. Specific SFRs indicate wide range in the evolutionary state of galaxies at z ~ 2, from galaxies that have just begun to form stars to those that have already accumulated most of their stellar mass and are about to become, or already are, passively evolving. Finally, we examine two techniques for assessing the census of galaxies at z ~ 2. In the first, we select galaxies using optical, near-IR, and sub-mm criteria, and find a large overlap between optical and near-IR selected samples of galaxies at z ~ 2. The second technique involves reconstructing the luminosity function of z ~ 2 galaxies as determined from Monte Carlo simulations. We find that the SFR density increases between z = 4 to 2 by a factor of ~ 1.2. However, this increase is mild compared to the much steeper increase from z ~ 6 to z ~ 4, suggesting that the processes responsible for the increase in SFR density at early epochs saturate around z ~ 2.
", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-05172006-133633", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05172006-133633", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/383087" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1086/444588" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1086/503739" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "https://doi.org/10.1086/508851" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-05-22", "doi": "10.7907/9FXD-QX54", "alt_title": { "items": [ "A Multi-Wavelength Census of Star Formation at Redshifts z Equals 2" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-05-17", "thesis_defense_date": "2006-05-15", "thesis_approved_date": "2006-05-22", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Reddy, Naveen Ananta" }, { "id": "/id/eprint/2065", "eprint_id": 2065, "rev_number": 14, "documents": [ { "id": "/id/document/3734", "doc_id": 3734, "rev_number": 2, "files": [ { "id": "/id/file/21920", "fileid": 21920, "datasetid": "document", "objectid": 3734, "filename": "thesis_liu.pdf", "mime_type": "application/pdf", "filesize": 1682415, "mtime": "2012-12-26 02:46:37", "url": "/2065/1/thesis_liu.pdf" } ], "eprint_id": 2065, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis_liu.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis_liu.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20402" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20402" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20402" } ] } }, { "id": "/id/document/16186", "doc_id": 16186, "rev_number": 3, "files": [ { "id": "/id/file/202446", "fileid": 202446, "datasetid": "document", "objectid": 16186, "filename": "Liu_Junjun_2006.PDF", "mime_type": "application/pdf", "filesize": 41339, "mtime": "2016-08-22 21:15:31", "url": "/2065/2/Liu_Junjun_2006.PDF" } ], "eprint_id": 2065, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Liu_Junjun_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/20402", "doc_id": 20402, "rev_number": 2, "files": [ { "id": "/id/file/21918", "fileid": 21918, "datasetid": "document", "objectid": 20402, "filename": "preview.png", "mime_type": "image/png", "hash": "d922e1c67c3046d17f86b95e62b2f6f1", "hash_type": "MD5", "filesize": 13015, "mtime": "2012-12-26 02:46:37", "url": "/2065/3/preview.png" } ], "eprint_id": 2065, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3734" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3734" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3734" } ] } }, { "id": "/id/document/122022", "doc_id": 122022, "rev_number": 1, "files": [ { "id": "/id/file/367416", "fileid": 367416, "datasetid": "document", "objectid": 122022, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "c42006cd8b74af976886ee6c0189f456", "hash_type": "MD5", "filesize": 20361, "mtime": "2021-06-23 21:44:07", "url": "/2065/4/indexcodes.txt" } ], "eprint_id": 2065, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3734" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3734" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3734" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/20/65", "datestamp": "2006-06-01", "lastmod": "2022-08-25 00:03:15", "status_changed": "2009-09-25 02:25:22", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jliu@spacescience.org", "id": "Liu-Junjun", "name": { "family": "Liu", "given": "Junjun" }, "show_email": "NO" } ] }, "title": "Interaction of Magnetic Field and Flow in the Outer Shells of Giant Planets", "ispublished": "unpub", "full_text_status": "public", "keywords": "dynamo; giant planets; Interior; Jupiter; magnetic field; Neptune; Saturn; Uranus; wind", "abstract": "This study of the interaction of magnetic field and flow in the outer shells of giant planets consists of three parts.
\r\n\r\nPart one: The atmospheres of Jupiter and Saturn exhibit strong and stable zonal winds. Busse suggested that they might be the surface expression of deep flows on cylinders. However, the deep flow hypothesis experiences difficulty when account is taken of the electrical conductivity of molecular hydrogen as measured in shockwave experiments. The deep zonal flow of an electrically conducting fluid would produce a toroidal magnetic field, an associated poloidal electrical current, and Ohmic dissipation. In steady state, the total Ohmic dissipation cannot exceed the planet's net luminosity. If we assume that the observed zonal flow penetrates along cylinders until it is truncated to (near) zero at some spherical radius, the upper bound on Ohmic dissipation constrains this radius to be no smaller than 0.95 Jupiter radius and 0.87 Saturn radius. The truncation of the cylindrical flow in the convective envelope requires an appropriate force to break the Taylor-Proudman constraint. We have been unable to identify any plausible candidate. Thus we conclude that deep-seated cylindrical flows do not exist.
\r\n\r\nPart two: A fluid shell with sufficient electrical conductivity and azimuthal velocity shear outside of the dynamo generation region can attenuate the non-axisymmetric component of the magnetic field. However, the interaction of the axisymmetric component of the magnetic field and the zonal flow is able to reduce the magnitude of zonal flow. The dimensionless number characterizing this reduction is the Chandrasekhar number. The smaller Saturnian field may allow a larger velocity shear and a greater attenuation of the non-axisymmetric field, thereby providing a possible explanation for the nearly axisymmetric field.
\r\n\r\nPart three: Combining the study for the attenuation effect produced by the semi-conducting layer and the observation of the magnetic field by Galileo and Voyager, we find the possible outer boundary of the dynamo generation zone is at 0.86 Jupiter radius. The magnetic fields generated in the outer shell are dictated by a length scale comparable to the scale height of electrical conductivity, which is much smaller than the radius of the planet.
", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-05252006-223939", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05252006-223939", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-06-01", "doi": "10.7907/4PVM-0G30", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "advisor" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" }, { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "chair" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "orcid": "0000-0002-1084-3656", "role": "member" }, { "email": "tapio@gps.caltech.edu", "id": "Schneider-T", "name": { "family": "Schneider", "given": "Tapio" }, "orcid": "0000-0001-5687-2287", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-05-25", "thesis_defense_date": "2006-05-16", "thesis_approved_date": "2006-06-01", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "appliedmath" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Liu, Junjun" }, { "id": "/id/eprint/2007", "eprint_id": 2007, "rev_number": 14, "documents": [ { "id": "/id/document/3534", "doc_id": 3534, "rev_number": 3, "files": [ { "id": "/id/file/20898", "fileid": 20898, "datasetid": "document", "objectid": 3534, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 3217286, "mtime": "2012-12-26 02:45:26", "url": "/2007/1/thesis.pdf" } ], "eprint_id": 2007, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20206" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20206" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20206" } ] } }, { "id": "/id/document/16356", "doc_id": 16356, "rev_number": 3, "files": [ { "id": "/id/file/202293", "fileid": 202293, "datasetid": "document", "objectid": 16356, "filename": "Pan_Yi_2006.PDF", "mime_type": "application/pdf", "filesize": 41375, "mtime": "2016-08-22 21:15:25", "url": "/2007/2/Pan_Yi_2006.PDF" } ], "eprint_id": 2007, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Pan_Yi_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/20206", "doc_id": 20206, "rev_number": 2, "files": [ { "id": "/id/file/20896", "fileid": 20896, "datasetid": "document", "objectid": 20206, "filename": "preview.png", "mime_type": "image/png", "hash": "73a144b4f7dac5f86adcacf2733e4814", "hash_type": "MD5", "filesize": 13864, "mtime": "2012-12-26 02:45:26", "url": "/2007/3/preview.png" } ], "eprint_id": 2007, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3534" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3534" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3534" } ] } }, { "id": "/id/document/121812", "doc_id": 121812, "rev_number": 1, "files": [ { "id": "/id/file/367204", "fileid": 367204, "datasetid": "document", "objectid": 121812, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "748fad3d550dbce036e161cfafbec5bb", "hash_type": "MD5", "filesize": 31189, "mtime": "2021-06-23 21:36:25", "url": "/2007/4/indexcodes.txt" } ], "eprint_id": 2007, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3534" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3534" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3534" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/20/07", "datestamp": "2006-05-31", "lastmod": "2020-04-08 18:50:25", "status_changed": "2009-09-25 02:22:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ypan@tapir.caltech.edu", "id": "Pan-Yi", "name": { "family": "Pan", "given": "Yi" }, "show_email": "NO" } ] }, "title": "Topics of LIGO Physics: Template Banks for the Inspiral of Precessing, Compact Binaries, and Design of the Signal-Recycling Cavity for Advanced LIGO", "ispublished": "unpub", "full_text_status": "public", "keywords": "data analysis; false alarm; Gaussian mode", "abstract": "In the next decade, the detection of gravitational-wave signals by ground-based laser interferometric detectors (e.g., the Laser Interferometer Gravitational-Wave Observatory, or LIGO) will provide new information on the structure and dynamics of compact objects such as neutron stars (NS) and black holes (BH), both isolated and in binary systems. Efforts to detect the intrinsically weak gravitational-wave signals involve the development of high-quality detectors, the precise modeling of expected signals, and the development of efficient data analysis techniques. This thesis concerns two topics in these areas: methods to detect signals from the inspiral of precessing NS-BH and BH-BH binaries, and the design of the signal-recycling cavity for Advanced LIGO (the second generation LIGO detector).
\r\n\r\nThe detection of signals from the inspiral of precessing binaries using the standard matched filter technique, is complicated by the large number (12 at least) of parameters required to describe the complex orbital-precession dynamics of the binary and the consequent modulations of the gravitational-wave signals. To extract these signals from the noisy detector output requires a discrete bank of a huge number of signal templates that cover the 12-dimensional parameter space; and processing data with all these templates requires computational power far exceeding what is available with current technology. To solve this problem, Buonanno, Chen, and Vallisneri (BCV) proposed the use of detection template families (DTFs) --- phenomenological templates that are capable of mimicking rather accurately the inspiral waveform calculated by the post-Newtonian (PN) approach, while having a simpler functional form to reduce the computational cost. In particular, BCV proposed the so called BCV2 DTF for the precessing-binary inspiral, which has 12 parameters (most of them phenomenological). Of these, 8 are extrinsic parameters that can be searched over analytically, and only four of them are intrinsic parameters that need be searched over in a numerical one-by-one manner. The signal-matching efficiency of the BCV2 DTF has been shown to be satisfactory for signals from comparable mass BH-BH binaries.
\r\n\r\nIn Chapter 2 (in collaboration with Alessandra Buonanno, Yanbei Chen, Hideyuki Tagoshi, and Michele Vallisneri), I test the signal-matching efficiency of the BCV2 DTF for signals from a wide sample of precessing BH-BH and NS-BH binaries that covers the parameter range of interest for LIGO and other ground-based gravitational-wave detectors, and I study the mapping between the physical and phenomenological parameters. My colleagues and I calculate the template-match metric, propose the template-placement strategy in the intrinsic parameter space and estimate the number of templates needed (and thus equivalently the computational cost) to cover the parameter space. We also propose a so called BCV2P DTF that replaces the phenomenological parameters in the BCV2 DTF by physical parameters, which can be used to estimate the actual parameters of the binary that emitted any detected signal.
\r\n\r\nIn Chapters 3 and 4 (in collaboration with Alessandra Buonanno, Yanbei Chen, and Michele Vallisneri), I investigate a physical template family (PTF) suggested by BCV. This PTF uses the most accurate known waveforms for inspiraling, precessing binaries (the adiabatic PN waveforms), formulated using a new precessing convention such that five parameters become extrinsic. PTF has the obvious advantages over the DTFs of a perfect match with target signals, a lower false-alarm rate at fixed threshold, and an ability to directly estimate the physical parameters of any detected signal.
\r\n\r\nIn Chapter 3, we focus on the simpler single-spin binaries in which only four parameters out of nine remain intrinsic. We propose a two-stage scheme to search over the five extrinsic parameters quickly, and investigate the false-alarm statistics in each of the two stages. We define and calculate the metric of the full template space, and the projected metric and average metric of the intrinsic parameter subspace, and use these metrics to develop the method of template placement. Finally, we estimate that the number of templates needed to detect single-spin binary inspirals is within the reach of the current available computational power.
\r\n\r\nIn Chapter 4, we generalize the use of the single-spin PTF to double-spin binaries, based on the fact that most double-spin binaries have similar dynamics to the single-spin ones. Since the PTF in this case is, strictly speaking, only quasi-physical, we test and eventually find satisfactory signal-matching performance. We also investigate, both analytically and numerically, the difference between the single-spin and double-spin dynamics, and gain an intuition into where in the parameter space the PTF works well. We estimate the number of templates needed to cover all BH-BH and NS-BH binaries of interest to ground-based detectors, which turns out to be roughly at the limit of currently available computational power. Since the PTF is not exactly physical for double-spin binaries, it introduces systematic errors in parameter estimation. We investigate these, and find that they are either comparable to or overwhelmed by statistical errors, for events with moderate signal-to-noise ratio. BCV and I are currently systematically investigating parameter estimation with the PTF.
\r\n\r\nThe second part of this thesis concerns the design of the signal-recycling cavity for Advanced LIGO. In the planned Advanced-LIGO-detector upgrades from the first-generation LIGO, a signal-recycling mirror (SRM) is introduced at the dark output port. This SRM forms a signal-recycling cavity (SRC) with the input test masses. This signal-recycling design offers several advantages and brings new physics to LIGO. However, there is a problem in the current design of the SRC: the SRC is nearly degenerate, i.e., it does not distinguish transverse optical modes; and as a result, mode coupling due to mirror deformation will strongly reduce the optical power in the fundamental mode, and thus reduce the signal strength, which is roughly proportional to it.
\r\n\r\nIn Chapter 5, I investigate this problem using a numerical simulation of the propagation of the optical field in an Advanced LIGO interferometer. I find that if the current degenerate design for the SRC is used, there will be a serious and perhaps unattainable constraint on the magnitude of mirror deformations, in order to keep the reduction of signal-to-noise ratio below a few percent. This conclusion is consistent with previous order of magnitude estimates. This constraint poses practical difficulties on the quality of mirror polishing and the control of thermal aberration of the mirrors. Based on my simulation results, for a range of degeneracies of the SRC, I find the optimal level of degeneracy, which minimizes the reduction of signal-to-noise ratio. That optimum is nearly non-degenerate. I also discuss possible modifications to the current design that can achieve this optimal degeneracy.
", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-05242006-025220", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05242006-025220", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department", "LIGO" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-05-31", "doi": "10.7907/TJB1-PQ24", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "role": "member" }, { "email": "lindblom@tapir.caltech.edu", "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "member" }, { "email": "stan@ligo.caltech.edu", "id": "Whitcomb-S-E", "name": { "family": "Whitcomb", "given": "Stanley E." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-05-24", "thesis_defense_date": "2006-05-19", "thesis_approved_date": "2006-05-31", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Pan, Yi" }, { "id": "/id/eprint/2400", "eprint_id": 2400, "rev_number": 11, "documents": [ { "id": "/id/document/4546", "doc_id": 4546, "rev_number": 3, "files": [ { "id": "/id/file/26226", "fileid": 26226, "datasetid": "document", "objectid": 4546, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 1882028, "mtime": "2012-12-26 02:50:54", "url": "/2400/1/thesis.pdf" } ], "eprint_id": 2400, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21109" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21109" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21109" } ] } }, { "id": "/id/document/16122", "doc_id": 16122, "rev_number": 3, "files": [ { "id": "/id/file/203305", "fileid": 203305, "datasetid": "document", "objectid": 16122, "filename": "Kovacs_Attila_2006.PDF", "mime_type": "application/pdf", "filesize": 42324, "mtime": "2016-08-22 21:15:59", "url": "/2400/2/Kovacs_Attila_2006.PDF" } ], "eprint_id": 2400, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Kovacs_Attila_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/21109", "doc_id": 21109, "rev_number": 2, "files": [ { "id": "/id/file/26224", "fileid": 26224, "datasetid": "document", "objectid": 21109, "filename": "preview.png", "mime_type": "image/png", "hash": "c4da41a0691a3dc9ca7335eca0f92f58", "hash_type": "MD5", "filesize": 18712, "mtime": "2012-12-26 02:50:54", "url": "/2400/3/preview.png" } ], "eprint_id": 2400, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4546" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4546" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4546" } ] } }, { "id": "/id/document/122809", "doc_id": 122809, "rev_number": 1, "files": [ { "id": "/id/file/368208", "fileid": 368208, "datasetid": "document", "objectid": 122809, "filename": "indexcodes.txt", "mime_type": "text/x-c", "hash": "b8e9eedf46cae90554b4d33e45c913b9", "hash_type": "MD5", "filesize": 33332, "mtime": "2021-06-23 22:08:52", "url": "/2400/4/indexcodes.txt" } ], "eprint_id": 2400, "pos": 4, "placement": 4, "mime_type": "text/x-c", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4546" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4546" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4546" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/24/00", "datestamp": "2006-06-05", "lastmod": "2020-04-02 21:33:09", "status_changed": "2009-09-25 02:36:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "attila.kovacs@]cfa.harvard.edu", "id": "Kov\u00e1cs-Attila", "name": { "family": "Kov\u00e1cs", "given": "Attila" }, "show_email": "NO" } ] }, "title": "SHARC-2 350 Micron Observations of Distant Submillimeter Selected Galaxies and Techniques for the Optimal Analysis and Observing of Weak Signals", "ispublished": "unpub", "full_text_status": "public", "keywords": "1/f noise; 350 micron; CRUSH; data analysis; data collection strategies; data reduction; filtering; noise weighting; observing patterns; observing strategies; radio to far-infrared correlation; SHARC-2; submillimeter galaxies; weak signals", "abstract": "New 350 micron data constrain accurately the thermal far-infrared spectral energy distributions (SEDs) for 12 distant submillimeter selected galaxies (SMGs). The results confirm that the linear radio to far-infrared correlation, established for local infrared galaxies, holds out to high redshifts z ~ 1--3. The low correlation constant q ~ 2.14 is more indicative of star formation than AGN-fueled dust heating. The sample exhibits an apparent luminosity--temperature relation (L_FIR ~ T_d^2.89), possibly owing to selection effects. As a result, photometric redshifts in the radio or far-infrared may not be viable, but expressions may relate the observed quantities for current flux and volume limited SMG samples. These suggest that SED estimation may be possible, for objects similarly selected, based on a single radio or far-infrared flux measurement.
\r\n\r\nThe detection of these faint objects (~10 mJy at 350 micron) from the ground is complicated by a bright (~1000 Jy) and highly variable (~10 Jy RMS in 10 minutes of integration) atmosphere with a 1/f^2 noise spectrum and by instrumental 1/f noise. To reach optimum sensitivities, a careful analysis of the data is required, and well-chosen observing strategies are helpful. The principal techniques that aid the extraction of weak signals from colored noise are presented. Close to optimal analysis is implemented effectively by the CRUSH software. Both the computing and storage requirement of the implementation scales linearly with the size of the data set, making this approach superior to the computationally expensive alternatives for handling the very large data volumes expected from future instruments.
", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-06022006-123747", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06022006-123747", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-06-05", "doi": "10.7907/8ZM9-6671", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "email": "blain@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "jonas@submm.caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-06-02", "thesis_defense_date": "2006-05-19", "thesis_approved_date": "2006-06-05", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Kov\u00e1cs, Attila" }, { "id": "/id/eprint/907", "eprint_id": 907, "rev_number": 11, "documents": [ { "id": "/id/document/1391", "doc_id": 1391, "rev_number": 3, "files": [ { "id": "/id/file/8674", "fileid": 8674, "datasetid": "document", "objectid": 1391, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 4141403, "mtime": "2012-12-26 02:33:35", "url": "/907/1/thesis.pdf" } ], "eprint_id": 907, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18187" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18187" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18187" } ] } }, { "id": "/id/document/15740", "doc_id": 15740, "rev_number": 3, "files": [ { "id": "/id/file/200659", "fileid": 200659, "datasetid": "document", "objectid": 15740, "filename": "Bundy_Kevin_2006.PDF", "mime_type": "application/pdf", "filesize": 41690, "mtime": "2016-08-22 21:14:26", "url": "/907/2/Bundy_Kevin_2006.PDF" } ], "eprint_id": 907, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Bundy_Kevin_2006.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/18187", "doc_id": 18187, "rev_number": 2, "files": [ { "id": "/id/file/8672", "fileid": 8672, "datasetid": "document", "objectid": 18187, "filename": "preview.png", "mime_type": "image/png", "hash": "3b725ed813d1257e554666bf0cf76ae3", "hash_type": "MD5", "filesize": 15558, "mtime": "2012-12-26 02:33:35", "url": "/907/3/preview.png" } ], "eprint_id": 907, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1391" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/1391" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1391" } ] } }, { "id": "/id/document/120335", "doc_id": 120335, "rev_number": 1, "files": [ { "id": "/id/file/365716", "fileid": 365716, "datasetid": "document", "objectid": 120335, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "204776111787ccf439cf2d5ba0acd27b", "hash_type": "MD5", "filesize": 32600, "mtime": "2021-06-23 20:44:38", "url": "/907/4/indexcodes.txt" } ], "eprint_id": 907, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1391" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1391" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/1391" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/09/07", "datestamp": "2006-03-09", "lastmod": "2021-11-05 22:57:09", "status_changed": "2009-09-25 01:50:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kbundy@ucsc.edu", "id": "Bundy-Kevin-A", "name": { "family": "Bundy", "given": "Kevin A." }, "orcid": "0000-0001-9742-3138", "show_email": "NO" } ] }, "title": "The Mass Assembly History of Field Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "downsizing; evolution; galaxy; star formation", "abstract": "The work presented in this thesis utilizes the combination of near-IR photometry and spectroscopic redshifts to estimate the stellar masses of distant field galaxies in order to characterize their assembly history since z~1. The primary data set for this analysis comes from an extensive near-IR survey conducted at Palomar Observatory that includes over 12,000 galaxies detected in the Ks-band with DEEP2 spectroscopic redshifts in the range 0.2<z<1.5. Utilizing stellar masses estimated for this sample, little evolution is observed in the galaxy stellar mass function since z~1, indicating that the stellar content of intermediate to high-mass galaxies has largely assembled by this epoch. Significant evolution since z~1 in the characteristics of the galaxy population does take place, however. As a function of time, red early-types--already established at the highest masses at z~1--increase in abundance as star formation shifts to late-type galaxies with lower masses. This pattern is interpreted in the context of \"downsizing,\" and a new mechanism is proposed that is capable of quenching star formation in massive galaxies and driving their morphological transformation into systems with spheroidal configurations.
\r\n\r\nNew diagnostics are introduced to quantify this downsizing behavior including the quenching mass, M_Q, which traces the stellar mass scale above which star formation in galaxies is suppressed. M_Q decreases by a factor of ~5 after z~1, indicating that the quenching mechanism responsible for downsizing becomes more efficient in galaxies with lower masses as a function of time. This evolution is analyzed as a function of environmental density, and no environmental dependence is observed except in the most extreme environments, where downsizing appears to be slightly accelerated in high density regions. This weak environmental dependence suggests that the quenching mechanism for most galaxies is primarily driven by internal processes. The nature of the quenching mechanism is discussed in the context of CDM galaxy formation models, and additional motivation for this comparison is also presented in a direct study of the near-IR merger rate and an analysis of the relationship between stellar mass and dark matter in disk galaxies.
", "date": "2006", "date_type": "degree", "id_number": "CaltechETD:etd-03092006-120454", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03092006-120454", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-03-09", "doi": "10.7907/3QVQ-FH17", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "orcid": "0000-0002-1084-3656", "role": "chair" }, { "email": "acr@deimos.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "nzs@radio.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-03-09", "thesis_defense_date": "2006-02-28", "thesis_approved_date": "2006-03-09", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2006", "author_list": "Bundy, Kevin A." }, { "id": "/id/eprint/1835", "eprint_id": 1835, "rev_number": 172, "documents": [ { "id": "/id/document/3022", "doc_id": 3022, "rev_number": 23, "files": [ { "id": "/id/file/18285", "fileid": 18285, "datasetid": "document", "objectid": 3022, "filename": "aminoethanol.fit", "mime_type": "", "filesize": 313626, "mtime": "2012-12-26 02:42:39", "url": "/1835/1/aminoethanol.fit" } ], "eprint_id": 1835, "pos": 1, "placement": 24, "format": "other", "format_desc": "aminoethanol.fit -- Appendix I and ch.7", "language": "en", "security": "public", "license": "other", "main": "aminoethanol.fit", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "supplemental" }, { "id": "/id/document/3023", "doc_id": 3023, "rev_number": 20, "files": [ { "id": 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3046" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/18/35", "datestamp": "2005-05-23", "lastmod": "2023-11-08 00:16:43", "status_changed": "2009-09-25 02:16:45", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "susanna.widicus.weaver@emory.edu", "id": "WidicusWeaver-Susanna-Leigh", "name": { "family": "Widicus Weaver", "given": "Susanna Leigh" }, "orcid": "0000-0001-6015-3429", "show_email": "NO" } ] }, "title": "Rotational Spectroscopy and Observational Astronomy of Prebiotic Molecules", "ispublished": "unpub", "full_text_status": "public", "keywords": "astrochemistry; rotational spectroscopy ; molecular spectroscopy", "abstract": "It is now widely believed that prebiotic molecules were delivered to the early Earth by planetesimals and their associated interplanetary dust particles. Yet the formation pathways for these molecules are not clear. Amino acids and sugars have been found in carbonaceous chondrites, but only much simpler species have been detected in the interstellar medium (ISM). Prebiotic organics could have formed in the ISM and been directly incorporated into planetesimals, or simpler species could have formed in the ISM and then been incorporated into planetesimals, undergone further processing, and been delivered to Earth. Limits on interstellar chemistry must therefore be established through observational astronomy before potential prebiotic formation pathways can be assessed. These observations require laboratory spectroscopic investigation of the species of interest.
\r\n\r\nThis thesis is an interdisciplinary study involving laboratory rotational spectroscopy and astronomical observations of several key prebiotic molecules. The laboratory work has focused on obtaining the rotational spectra of the simplest three-carbon ketose sugar, 1,3-dihydroxyacetone, and its structural isomers methyl glycolate and dimethyl carbonate, as well as aminoethanol, the predicted interstellar precursor to alanine. The pure rotational spectral analysis of the low-lying torsional states of the simplest alpha-hydroxy aldehyde, glycolaldehyde, has also been completed. The original Balle-Flygare Fourier transform microwave spectrometer was used to obtain the microwave spectra, while both the Jet Propulsion Laboratory and Caltech direct absorption flow cell spectrometers were used for additional direct absorption millimeter and submillimeter studies.
\r\n\r\nThe results of these laboratory experiments were used to guide observational searches with the Caltech Submillimeter Observatory, the Owens Valley Millimeter Array, and the Green Bank Telescope toward the hot core sources Sgr B2(N-LMH), Orion Hot Core/Compact Ridge, and W51 e1/e2. Evidence has been found for the presence of dihydroxyacetone and methyl glycolate in Sgr B2(N-LMH).
\r\n\r\nThese results have important implications for interstellar grain surface chemistry, and proposed additions to grain surface chemical models are also discussed. Reactions involving surface radicals and molecules containing carbonyl groups can efficiently compete with the simple grain surface reactions included in previous models. Such aldehyde abstraction reactions should be considered as pathways to complex carbonyl-containing species on interstellar grain surfaces.
", "date": "2005", "date_type": "degree", "id_number": "CaltechETD:etd-05162005-153745", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05162005-153745", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-05-23", "doi": "10.7907/CN1R-H437", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jlbchamp@its.caltech.edu", "id": "Beauchamp-J-L", "name": { "family": "Beauchamp", "given": "Jesse L." }, "orcid": "0000-0001-8839-4822", "role": "chair" }, { "email": "collier@caltech.edu", "id": "Collier-C-P", "name": { "family": "Collier", "given": "C. Patrick" }, "orcid": "0000-0002-8198-793X", "role": "member" }, { "email": "dcrees@caltech.edu", "id": "Rees-D-C", "name": { "family": "Rees", "given": "Douglas C." }, "orcid": "0000-0003-4073-1185", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-05-16", "thesis_defense_date": "2005-05-02", "thesis_approved_date": "2005-05-23", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2005", "author_list": "Widicus Weaver, Susanna Leigh" }, { "id": "/id/eprint/334", "eprint_id": 334, "rev_number": 60, "documents": [ { "id": "/id/document/494", "doc_id": 494, "rev_number": 5, "files": [ { "id": "/id/file/3160", "fileid": 3160, "datasetid": "document", "objectid": 494, "filename": "00_Front_Abstract_TOC.pdf", "mime_type": "application/pdf", "filesize": 96295, "mtime": "2012-12-26 02:28:57", "url": "/334/1/00_Front_Abstract_TOC.pdf" } ], "eprint_id": 334, "pos": 1, "placement": 3, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "00_Front_Abstract_TOC.pdf", "language": "en", "security": "public", "license": "other", "main": "00_Front_Abstract_TOC.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { 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"hash_type": "MD5", "filesize": 691, "mtime": "2021-06-23 20:22:59", "url": "/334/62/indexcodes.txt" } ], "eprint_id": 334, "pos": 62, "placement": 62, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/54582" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/54582" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/54582" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/03/34", "datestamp": "2005-01-27", "lastmod": "2023-11-08 00:16:43", "status_changed": "2009-09-25 01:34:51", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "vkapinus@gmail.com", "id": "Kapinus-Vadym-A", "name": { "family": "Kapinus", "given": "Vadym A." }, "show_email": "NO" } ] }, "title": "Photophysical Properties of Protonated Aromatic Hydrocarbons", "ispublished": "unpub", "full_text_status": "public", "keywords": "anthracene; diffuse interstellar bands; photodissociation; polycyclic aromatic hydrocarbons; protonated PAHs; spectroscopy", "abstract": "Polycyclic aromatic hydrocarbons (PAHs) and their derivatives are among the likely candidates for diffuse interstellar band (DIB) carriers. In diffuse interstellar clouds molecules are expected to be ionized, and PAHs in particular are predicted to be in protonated form. Protonated PAHs are closed-shell ions with electronic transitions that are red-shifted compared to neutral PAHs.
\r\n\r\nThis thesis presents an experimental and theoretical analysis of two-, three-, and four-ring protonated PAHs. The energetics of protonated PAH isomers in their ground electronic state and the proton tunneling barriers were calculated using density functional theory. The loss of an H atom or H2 molecule from a protonation site were identified as the most favorable dissociation channels for protonated PAHs. They were found to be within a few kcal/mol of each other in energy, and about 45-60 kcal/mol above the ground state.
\r\n\r\nThe Configuration Interaction Singles (CIS) method was used to estimate the positions of the electronic transitions for protonated PAHs. Red shifts up to 150 nm were predicted for protonated naphthalene, anthracene, phenanthrene and pyrene. This places the S1 \u2190 S0 transitions of protonated PAHs well into the DIB wavelength region.
\r\n\r\nExperimentally, a robust hydrogen discharge source was designed to produce protonated PAHs. Laser photodissociation of protonated PAHs was studied with an excimer laser/reflectron time-of-flight mass spectrometer. Small protonated PAHs were found to be very photostable. Nanosecond pulse length photodissociation was multiphoton even at short wavelengths (193 nm). For protonated anthracene, the dissociation threshold was estimated to be 13 -- 15 eV, much higher than the predicted thermodynamic threshold of 2.5 -- 3.0 eV. This was attributed to intramolecular vibrational relaxation (IVR) upon electronic excitation.
\r\n\r\nCluster photodissociation was used to locate the electronic transitions of protonated anthracene between 420 and 540 nm. Clusters with water molecules were produced in a two-valve mixing discharge source. Their photodissociation spectrum was recorded using a novel hybrid cavity optical parametric oscillator. The observed absorption bands (20 nm FWHM) are too wide to account for the DIBs. This spectral broadening most likely results from rapid IVR induced by the high density of states in protonated PAHs.
", "date": "2005", "date_type": "degree", "id_number": "CaltechETD:etd-01252005-123917", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01252005-123917", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-01-27", "doi": "10.7907/3A85-DC20", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jlbchamp@its.caltech.edu", "id": "Beauchamp-J-L", "name": { "family": "Beauchamp", "given": "Jesse L." }, "orcid": "0000-0001-8839-4822", "role": "chair" }, { "email": "dad@igor.caltech.edu", "id": "Dougherty-D-A", "name": { "family": "Dougherty", "given": "Dennis A." }, "orcid": "0000-0003-1464-2461", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "email": "hgcm@its.caltech.edu", "id": "Gray-H-B", "name": { "family": "Gray", "given": "Harry B." }, "orcid": "0000-0002-7937-7876", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-01-25", "thesis_defense_date": "2004-12-14", "thesis_approved_date": "2005-01-27", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2005", "author_list": "Kapinus, Vadym A." }, { "id": "/id/eprint/2391", "eprint_id": 2391, "rev_number": 12, "documents": [ { "id": "/id/document/4536", "doc_id": 4536, "rev_number": 3, "files": [ { "id": "/id/file/26153", "fileid": 26153, "datasetid": "document", "objectid": 4536, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 2980205, "mtime": "2012-12-26 02:50:51", "url": "/2391/1/thesis.pdf" } ], "eprint_id": 2391, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21099" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21099" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21099" } ] } }, { "id": "/id/document/21099", "doc_id": 21099, "rev_number": 2, "files": [ { "id": "/id/file/26151", "fileid": 26151, "datasetid": "document", "objectid": 21099, "filename": "preview.png", "mime_type": "image/png", "hash": "3a2e8a10845b57243b3f725c10ed8647", "hash_type": "MD5", "filesize": 23495, "mtime": "2012-12-26 02:50:51", "url": "/2391/2/preview.png" } ], "eprint_id": 2391, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4536" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4536" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4536" } ] } }, { "id": "/id/document/122797", "doc_id": 122797, "rev_number": 1, "files": [ { "id": "/id/file/368195", "fileid": 368195, "datasetid": "document", "objectid": 122797, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "08bf41f363d1c0cd17d23495d7502176", "hash_type": "MD5", "filesize": 31288, "mtime": "2021-06-23 22:08:14", "url": "/2391/3/indexcodes.txt" } ], "eprint_id": 2391, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4536" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4536" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4536" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/23/91", "datestamp": "2005-06-03", "lastmod": "2020-05-22 22:17:02", "status_changed": "2009-09-25 02:36:19", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "nevin@mit.edu", "id": "Weinberg-Nevin-Nachum", "name": { "family": "Weinberg", "given": "Nevin Nachum" }, "orcid": "0000-0001-9194-2084", "show_email": "NO" } ] }, "title": "I. Ash Injection and Exposure During Radius Expansion Type I X-Ray Bursts. II. Stellar Dynamics at the Galactic Center. III. Weak Gravitational Lensing by Dark Matter Concentrations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Dark energy; Extremely Large Telescope", "abstract": "The studies presented herein are on three distinct topics in astrophysics:
\r\n\r\nI. We solve for the evolution of the vertical extent of the convective region of a neutron star atmosphere during a type I X-ray burst. The convective region is well-mixed with ashes of nuclear burning, and its extent determines the burst rise time. We show that the maximum extent of the convective region during photospheric radius expansion (PRE) bursts can be sufficiently great that some ashes of burning are: (1) ejected by the radiation-driven wind during the PRE phase and, (2) exposed at the neutron star surface following the PRE phase. We calculate the expected column density of ashes in hydrogen-like states and find that the resulting photoionization edges should be detectable with current high spectral resolution X-ray telescopes. A detection would probe the burst nuclear burning processes and might enable a measurement of the neutron star gravitational redshift.
\r\n\r\nII. We discuss physical experiments achievable via the monitoring of stellar dynamics near the massive black hole (MBH) at the Galactic center with a next-generation, extremely large telescope (ELT). We use the Markov Chain Monte Carlo method to evaluate the constraints that the monitoring of these orbits will place on the matter content at the Galactic center. We compare these future constraints with those obtained with the current data. We also describe how the monitoring of stellar proper motions can be used to probe directly the masses of isolated stellar remnants near the MBH.
\r\n\r\nIII. We calculate the abundance of dark-matter concentrations that are sufficiently overdense to produce a detectable weak-gravitational-lensing signal. Most of these overdensities are virialized halos containing identifiable X-ray and/or optical clusters. However, a significant fraction are nonvirialized, cluster-mass overdensities still in the process of gravitational collapse---these should produce significantly weaker or no X-ray emission. Our predicted abundance of such dark clusters is consistent with the abundance implied by the detection of apparent dark lenses. We also examine the prospect of using weak gravitational lenses to constrain the dark energy equation-of-state parameter.
\r\n", "date": "2005", "date_type": "degree", "id_number": "CaltechETD:etd-06022005-151603", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06022005-151603", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-06-03", "doi": "10.7907/V8PX-AE66", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-06-02", "thesis_defense_date": "2005-05-18", "thesis_approved_date": "2005-06-03", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2005", "author_list": "Weinberg, Nevin Nachum" }, { "id": "/id/eprint/3910", "eprint_id": 3910, "rev_number": 12, "documents": [ { "id": "/id/document/6564", "doc_id": 6564, "rev_number": 2, "files": [ { "id": "/id/file/39560", "fileid": 39560, "datasetid": "document", "objectid": 6564, "filename": "MazinThesis.pdf", "mime_type": "application/pdf", "filesize": 21902405, "mtime": "2012-12-26 03:03:57", "url": "/3910/1/MazinThesis.pdf" } ], "eprint_id": 3910, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "MazinThesis.pdf", "language": "en", "security": "public", "license": "other", "main": "MazinThesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23096" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23096" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23096" } ] } }, { "id": "/id/document/23096", "doc_id": 23096, "rev_number": 2, "files": [ { "id": "/id/file/39558", "fileid": 39558, "datasetid": "document", "objectid": 23096, "filename": "preview.png", "mime_type": "image/png", "hash": "c4de8eeb95b2cebecaaca87dca0d1106", "hash_type": "MD5", "filesize": 12280, "mtime": "2012-12-26 03:03:56", "url": "/3910/2/preview.png" } ], "eprint_id": 3910, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6564" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6564" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6564" } ] } }, { "id": "/id/document/123905", "doc_id": 123905, "rev_number": 1, "files": [ { "id": "/id/file/369333", "fileid": 369333, "datasetid": "document", "objectid": 123905, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "7bb6498ecdecc1706b82d317c20481d1", "hash_type": "MD5", "filesize": 30048, "mtime": "2021-06-23 23:05:32", "url": "/3910/3/indexcodes.txt" } ], "eprint_id": 3910, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6564" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6564" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/6564" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/39/10", "datestamp": "2004-10-05", "lastmod": "2020-05-22 21:13:24", "status_changed": "2009-09-25 03:07:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "bmazin@physics.ucsb.edu", "id": "Mazin-Benjamin-A", "name": { "family": "Mazin", "given": "Benjamin A." }, "show_email": "NO" } ] }, "title": "Microwave Kinetic Inductance Detectors", "ispublished": "unpub", "full_text_status": "public", "keywords": "kinetic inductance; low temperature detectors", "abstract": "Low temperature detectors have been a subject of intense interest to the scientific community over the last decade. These detectors work at very low temperatures, often well below 1 Kelvin, to minimize the noise in the measurement of photons. This leads to very powerful detectors applicable to a broad wavelength range.
\r\n\r\nSince these detectors are so sensitive even single pixels and small arrays (up to several hundred pixels) enable deeper explorations of the cosmos than ever before. Instruments based on these technologies have been used at submillimeter, optical, and X-ray wavelengths. The scientific prospects for these detectors increase as they grow in pixel count. For some applications, especially for Cosmic Microwave Background (CMB) polarization work, a large focal plane will not only increase efficiency but will also enable new and vital science.
\r\n\r\nCurrent superconducting technologies, such as Transition Edge Sensors (TESs), can currently deliver extremely high sensitivity in the submillimeter and read-noise free imaging spectroscopy at Optical/UV and X-ray wavelengths, but the largest arrays contain less that 100 pixels. In order to make real progress these arrays must contain many thousands of pixels. This is a formidable technical challenge.
\r\n\r\nThis thesis will explore a promising emerging technology called Microwave Kinetic Inductance Detectors (MKIDs). MKIDs make use of the change in the surface impedance of a superconductor as incoming photons break up Cooper pairs. This is accomplished by making the strip of superconductor part of a microwave resonant circuit, and monitoring the phase of a signal transmitted through (or past) the resonator. The primary advantage of this technology is that by using resonant circuits with high quality factors, passive frequency domain multiplexing will allow up to thousands of resonators to be read out through a single coaxial cable and a single HEMT amplifier. This eliminates the cryogenic electronics (SQUIDS) and wiring problems associated with current superconducting devices. Inexpensive and powerful room-temperature readout electronics can leverage the microwave integrated circuits developed for wireless communications.
\r\n\r\nWhen this project started four years ago MKIDs were just a concept. In this thesis I will recount the progress we have made in taking this concept and turning it into a detector technology, building on the work we published in Nature in 2003. I will demonstrate that we have overcome the major technical obstacles and shown conclusively that MKIDs work, and should provide much larger arrays than are possible with other technologies. Due to our work at Caltech and JPL, MKIDs are considered one of the leading technologies to reach the ambitious goals set for future ground and space missions. The noise performance is already good enough for sky-limited, ground-based, submillimeter astronomy.
\r\n\r\nDespite MKIDs acceptable noise performance for ground-based astronomy, there are many applications which require lower detector noise. The simple MKIDs we measure in this thesis still exhibit a noise higher than theory would predict which could limit their usefulness for some applications.
\r\n\r\nIn Chapters 7-9 we perform several experiments which identify the source of the excess noise as the substrate.
\r\n\r\nIn the course of these experiments to characterize and identify the noise, we successfully demonstrate two distinct approaches which dramatically reduce the noise excess.
", "date": "2005", "date_type": "degree", "id_number": "CaltechETD:etd-10042004-120707", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10042004-120707", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-10-05", "doi": "10.7907/GZ72-V784", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" } } ] }, "thesis_committee": { "items": [ { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "chair" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "role": "member" }, { "email": "jonas@submm.caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-10-04", "thesis_defense_date": "2004-08-18", "thesis_approved_date": "2004-10-05", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2005", "author_list": "Mazin, Benjamin A." }, { "id": "/id/eprint/372", "eprint_id": 372, "rev_number": 12, "documents": [ { "id": "/id/document/545", "doc_id": 545, "rev_number": 3, "files": [ { "id": "/id/file/3488", "fileid": 3488, "datasetid": "document", "objectid": 545, "filename": "baj_thesis_twoside.pdf", "mime_type": "application/pdf", "filesize": 4562309, "mtime": "2012-12-26 02:29:13", "url": "/372/1/baj_thesis_twoside.pdf" } ], "eprint_id": 372, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "baj_thesis_twoside.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17371" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17371" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17371" } ] } }, { "id": "/id/document/17371", "doc_id": 17371, "rev_number": 2, "files": [ { "id": "/id/file/3486", "fileid": 3486, "datasetid": "document", "objectid": 17371, "filename": "preview.png", "mime_type": "image/png", "hash": "d77034db6f728600fe187f35d682e7a5", "hash_type": "MD5", "filesize": 13346, "mtime": "2012-12-26 02:29:13", "url": "/372/2/preview.png" } ], "eprint_id": 372, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/545" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/545" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/545" } ] } }, { "id": "/id/document/119859", "doc_id": 119859, "rev_number": 1, "files": [ { "id": "/id/file/365228", "fileid": 365228, "datasetid": "document", "objectid": 119859, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "19a91cf37bd79aeb17da9c92dc359671", "hash_type": "MD5", "filesize": 23671, "mtime": "2021-06-23 20:23:48", "url": "/372/3/indexcodes.txt" } ], "eprint_id": 372, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/545" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/545" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/545" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/03/72", "datestamp": "2005-01-31", "lastmod": "2023-05-30 22:33:33", "status_changed": "2009-09-25 01:35:30", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jacoby-Bryan-Anthony", "name": { "family": "Jacoby", "given": "Bryan Anthony" }, "show_email": "NO" } ] }, "title": "Recycled Pulsars", "ispublished": "unpub", "full_text_status": "public", "keywords": "neutron stars; pulsars", "abstract": "We present the results of a large-area survey for millisecond pulsars (MSPs) at moderately high galactic latitudes with the 64 m Parkes radio telescope, along with follow-up timing and optical studies of the newly-discovered pulsars and several others. Major results include the first precise measurement of the mass of a fully recycled pulsar and measurement of orbital period decay in a double neutron star binary system allowing a test of general relativity along with improved measurements of the neutron star masses.
\r\n\r\nIn a survey of approx. 4,150 square degrees, we discovered 26 previously unknown pulsars, including 7 \"recycled\" millisecond or binary pulsars. Several of these recycled pulsars are particularly interesting: PSR J1528-3146 is in a circular orbit with a companion of at least 0.94 solar masses; it is a member of the recently recognized class of intermediate mass binary pulsar (IMBP) systems with massive white dwarf companions. We have detected optical counterparts for this and one other IMBP system; taken together with optical detections and non-detections of several similar systems, our results indicate that the characteristic age consistently overestimates the time since the end of mass accretion in these recycled systems. This result implies that the pulsar spin period at the end of the accretion phase is not dramatically shorter than the observed period as is generally assumed. PSR J1600-3053 is among the best high-precision timing pulsars known and should be very useful as part of an ensemble of pulsars used to detect very low frequency gravitational waves. PSR J1738+0333 has an optical counterpart which, although not yet well-studied, has already allowed a preliminary measurement of the system's mass ratio. The most significant discovery of this survey is PSR J1909-3744, a 2.95 ms pulsar in an extremely circular 1.5 d orbit with a low-mass white dwarf companion. Though this system is a fairly typical low-mass binary pulsar (LMBP) system, it has several exceptional qualities: an extremely narrow pulse profile and stable rotation have enabled the most precise long-term timing ever reported, and a nearly edge-on orbit gives rise to a strong Shapiro delay signature in the pulse timing data which has allowed the most precise measurement of the mass of a millisecond pulsar: 1.438 +/- 0.024 solar masses. Our accurate parallax distance measurement, d = 1.14 +0.08 / -0.07 kpc, combined with the mass of the optically-detected companion, 0.2038 +/- 0.022 solar masses, will provide an important calibration for white dwarf models relevant to other LMBP companions.
\r\n\r\nWe have measured the decay of the binary period of the double neutron star system B2127+11C in the globular cluster M15. This has allowed an improved measurement of the mass of the pulsar, 1.3584 +/- 0.0097 solar masses, and companion, 1.3544 +/- 0.0097 solar masses, as well as a test of general relativity at the 3% level. We find that the proper motions of this pulsar as well as B2127+11A and B2127+11B are consistent with each other and with one published measurement of the cluster proper motion.
\r\n\r\nWe have discovered three binary millisecond pulsars in the globular cluster M62 using the 100-m Green Bank Telescope (GBT). These pulsars are the first objects discovered with the GBT.
\r\n\r\nWe briefly describe a wide-bandwidth coherent dedispersion backend used for some of the high precision pulsar timing observations presented here.
\r\n", "date": "2005", "date_type": "degree", "id_number": "CaltechETD:etd-01272005-015012", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01272005-015012", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-01-31", "doi": "10.7907/H5DY-5J74", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "chair" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "email": "sba@astro.caltech.edu", "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "Stuart B." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-01-27", "thesis_defense_date": "2004-12-08", "thesis_approved_date": "2005-01-31", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2005", "author_list": "Jacoby, Bryan Anthony" }, { "id": "/id/eprint/2095", "eprint_id": 2095, "rev_number": 15, "documents": [ { "id": "/id/document/3795", "doc_id": 3795, "rev_number": 3, "files": [ { "id": "/id/file/22246", "fileid": 22246, "datasetid": "document", "objectid": 3795, "filename": "cv.pdf", "mime_type": "application/pdf", "filesize": 35386, "mtime": "2012-12-26 02:46:54", "url": "/2095/1/cv.pdf" } ], "eprint_id": 2095, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "cv.pdf", "language": "en", "security": "internal", "license": "other", "main": "cv.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"uri": "/id/document/3796" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3796" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/20/95", "datestamp": "2005-05-26", "lastmod": "2023-05-30 22:17:05", "status_changed": "2009-09-25 02:26:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Eisner-Joshua-Aaron", "name": { "family": "Eisner", "given": "Joshua Aaron" }, "show_email": "NO" } ] }, "title": "High Angular Resolution Studies of the Structure and Evolution of Protoplanetary Disks", "ispublished": "unpub", "full_text_status": "public", "keywords": "interferometry; planet formation; protoplanetary disks; young stars", "abstract": "Young stars are surrounded by massive, rotating disks of dust and gas, which supply a reservoir of material that may be incorporated into planets or accreted onto the central star. In this dissertation, I use high angular resolution observations at a range of wavelengths to understand the structure, ubiquity, and evolutionary timescales of protoplanetary disks.
\r\n\r\nFirst, I describe a study of Class I protostars, objects believed to be at an evolutionary stage between collapsing spherical clouds and fully-assembled young stars surrounded by protoplanetary disks. I use a Monte Carlo radiative transfer code to model new 0.9 micron scattered light images, 1.3 mm continuum images, and broadband spectral energy distributions. This modeling shows that Class I sources are probably surrounded by massive protoplanetary disks embedded in massive infalling envelopes. For the best-fitting models of the circumstellar dust distributions, I determine several important properties, including envelope and disk masses, mass infall rates, and system inclinations, and I use these results to constrain the evolutionary stage of these objects.
\r\n\r\nSecond, I discuss observations of the innermost regions of more evolved disks around T Tauri and Herbig Ae/Be stars, obtained with the Palomar Testbed and Keck Interferometers. I constrain the spatial and temperature structure of the circumstellar material at sub-AU radii, and demonstrate that lower-mass stars are surrounded by inclined disks with puffed-up inner edges 0.1-1 AU from the star. In contrast, the truncated inner disks around more massive stars may not puff-up, indicating that disk structure depends on stellar properties. I discuss the implications of these results for disk accretion, terrestrial planet formation and giant planet migration.
\r\n\r\nFinally, I put these detailed studies of disk structure into a broader context by constraining the mass distribution and evolutionary timescales of circumstellar disks. Using the Owens Valley Millimeter Array, I mapped the millimeter continuum emission toward >300 low-mass stars in the NGC 2024 and Orion Nebula clusters. These observations demonstrate that the average disk mass in each cluster is comparable to the \"minimum-mass protosolar nebula\", and that there may be disk evolution on one million year timescales.
", "date": "2005", "date_type": "degree", "id_number": "CaltechETD:etd-05262005-141109", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05262005-141109", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-05-26", "doi": "10.7907/61Y5-F650", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." } }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098" } ] }, "thesis_committee": { "items": [ { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "orcid": "0000-0002-1084-3656", "role": "chair" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "member" }, { "email": "jmc@astro.caltech.edu", "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "John M." }, "orcid": "0000-0003-2251-0602", "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-05-26", "thesis_defense_date": "2005-05-17", "thesis_approved_date": "2005-05-26", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2005", "author_list": "Eisner, Joshua Aaron" }, { "id": "/id/eprint/1971", "eprint_id": 1971, "rev_number": 15, "documents": [ { "id": "/id/document/3433", "doc_id": 3433, "rev_number": 4, "files": [ { "id": "/id/file/20361", "fileid": 20361, "datasetid": "document", "objectid": 3433, "filename": "afcv.pdf", "mime_type": "application/pdf", "filesize": 10613, "mtime": "2012-12-26 02:44:52", "url": "/1971/1/afcv.pdf" } ], "eprint_id": 1971, "pos": 1, "placement": 2, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "afcv.pdf", "language": "en", "security": "internal", "license": "other", "main": "afcv.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/3434" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3434" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3434" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/19/71", "datestamp": "2005-05-27", "lastmod": "2020-12-10 20:20:25", "status_changed": "2009-09-25 02:21:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ajf@ias.edu", "id": "Farmer-Alison-Jane", "name": { "family": "Farmer", "given": "Alison Jane" }, "show_email": "YES" } ] }, "title": "Adventures in Theoretical Astrophysics", "ispublished": "unpub", "full_text_status": "public", "keywords": "chaotic dynamics; cosmic rays; gravitational waves; Saturn electrodynamics; white dwarf searches", "abstract": "This thesis is a tour of topics in theoretical astrophysics, unified by their diversity and their pursuit of physical understanding of astrophysical phenomena.
\r\n\r\nIn the first chapter, we raise the possibility of the detection of white dwarfs in transit surveys for extrasolar Earths, and discuss the peculiarities of detecting these more massive objects.
\r\n\r\nA population synthesis calculation of the gravitational wave background from extragalactic binary stars is then presented. In this study, we establish a firm understanding of the uncertainties in such a calculation and provide a valuable reference for planning the Laser Interferometer Space Antenna mission.
\r\n\r\nThe long-established problem of cosmic ray confinement to the Galaxy is addressed in another chapter. We introduce a new wave damping mechanism, due to the presence of background turbulence, that prevents the confinement of cosmic rays by the resonant streaming instability.
\r\n\r\nWe also investigate the spokes in Saturn's B ring, an electrodynamic mystery that is being illuminated by new data sent back from the Cassini spacecraft. In particular, we present assessments of the presence of charged dust near the rings, and the size of currents and electric fields in the ring system. We make inferences from the Cassini discovery of oxygen ions above the rings. In addition, the previous leading theory for spoke formation is demonstrated to be unphysical.
\r\n\r\nIn the final chapter, we explain the wayward motions of Prometheus and Pandora, two small moons of Saturn. Previously found to be chaotic as a result of mutual interactions, we account for their behavior by analogy with a parametric pendulum. We caution that this behavior may soon enter a new regime.
", "date": "2005", "date_type": "degree", "id_number": "CaltechETD:etd-05232005-155338", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05232005-155338", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-05-27", "doi": "10.7907/JJKJ-J144", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "chair" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-05-23", "thesis_defense_date": "2005-05-13", "thesis_approved_date": "2005-05-27", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2005", "author_list": "Farmer, Alison Jane" }, { "id": "/id/eprint/4209", "eprint_id": 4209, "rev_number": 32, "documents": [ { "id": "/id/document/6930", "doc_id": 6930, "rev_number": 3, "files": [ { "id": "/id/file/42092", "fileid": 42092, "datasetid": "document", "objectid": 6930, "filename": "chapter1.pdf", "mime_type": "application/pdf", "filesize": 212024, "mtime": "2012-12-26 03:06:29", "url": "/4209/1/chapter1.pdf" } ], "eprint_id": 4209, "pos": 1, "placement": 2, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "chapter1.pdf", "language": "en", "security": "public", "license": "other", "main": "chapter1.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6936" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6936" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/6936" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/09", "datestamp": "2003-10-28", "lastmod": "2023-11-08 00:16:43", "status_changed": "2009-09-25 03:13:39", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kessler-Jacqueline-Elizabeth", "name": { "family": "Kessler", "given": "Jacqueline Elizabeth" }, "show_email": "NO" } ] }, "title": "Gas and Dust Chemistry in Planet-Forming Disks", "ispublished": "unpub", "full_text_status": "public", "keywords": "aperture-synthesis; astrochemistry; CN; CO; cosmochemistry; HCN; HCO+; Herbig Ae; interferometry; molecular line; planet formation; silicates; star formation; T-Tauri", "abstract": "As analogs to the solar nebula, circumstellar disks offer a unique opportunity to study the conditions during the star and planet formation process. Interpretation of molecular line observations is dependent on the development of extensive models of the chemistry and radiative transfer in accretion disks. In this study, several millimeter-wave molecular lines were observed toward a sample of disks encircling T Tauri and Herbig Ae stars with the Owens Valley Millimeter Array. The intent of these studies is the quantitative examination of the chemistry of the biogenic elements (C, N, O, S) in accretion disks. Toward this goal, radiative transfer models were modified for direct comparison with the observations to aid in the interpretation of molecular line emission and comparison with the predictions of chemical models, as discussed in Chapter 2. Chapter 3 presents a survey of CN, HCN, CO and HCO+ in 7 Herbig Ae and T Tauri star disks, which was performed in order to probe the effects of UV fields on disk chemistry. In this study, CN and HCO+ are found to be sensitive to the strength of the local UV field. The first interferometric studies of deuterium in disks were performed and are discussed in Chapter 4. HDO and DCN were detected toward the T Tauri disk LkCa 15 and the Herbig Ae disk HD 163296. The deuterium enrichments are similar to that of molecular clouds, hot cores, and comets, consistent with comet formation in the outer regions of disks. The distribution of HDO in LkCa 15 was found to be similar to predictions from chemical models, which suggest a steep gradient as a function of disk radius. Chapter 5 presents Keck LWS observations of the 8-13 micron silicate emission feature toward several T Tauri and Herbig Ae stars at various stages of the star formation process indicate an evolutionary trend similar to that previously seen with ISO for disks around intermediate mass stars. However, emission from crystalline silicates was only detected toward one low mass star, Hen 3-600A, possibly indicating that crystallization processes occur less frequently, or are more difficult to observe at mid-infrared wavelengths, in these disks. Finally, in Chapter 6, a summary of protoplanetary disk chemistry is presented and the future of the field is discussed.", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-10222003-092836", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10222003-092836", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-10-28", "doi": "10.7907/MGC6-WR47", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Okumura-M", "name": { "family": "Okumura", "given": "Mitchio" }, "orcid": "0000-0001-6874-1137", "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "id": "Gray-H-B", "name": { "family": "Gray", "given": "Harry B." }, "orcid": "0000-0002-7937-7876", "role": "member" }, { "id": "Marcus-R-A", "name": { "family": "Marcus", "given": "Rudolph A." }, "orcid": "0000-0001-6547-1469", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-10-22", "thesis_defense_date": "2003-08-13", "thesis_approved_date": "2003-10-28", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Kessler, Jacqueline Elizabeth" }, { "id": "/id/eprint/1771", "eprint_id": 1771, "rev_number": 15, "documents": [ { "id": "/id/document/2872", "doc_id": 2872, "rev_number": 2, "files": [ { "id": "/id/file/17498", "fileid": 17498, "datasetid": "document", "objectid": 2872, "filename": "psu_thesis.pdf", "mime_type": "application/pdf", "filesize": 4115387, "mtime": "2012-12-26 02:41:48", "url": "/1771/1/psu_thesis.pdf" } ], "eprint_id": 1771, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "psu_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "psu_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19595" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19595" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19595" } ] } }, { "id": "/id/document/19595", "doc_id": 19595, "rev_number": 2, "files": [ { "id": "/id/file/17496", "fileid": 17496, "datasetid": "document", "objectid": 19595, "filename": "preview.png", "mime_type": "image/png", "hash": "ef64a62aa474da57c05e7582d38fdc7a", "hash_type": "MD5", "filesize": 16143, "mtime": "2012-12-26 02:41:48", "url": "/1771/2/preview.png" } ], "eprint_id": 1771, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2872" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2872" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2872" } ] } }, { "id": "/id/document/121215", "doc_id": 121215, "rev_number": 1, "files": [ { "id": "/id/file/366607", "fileid": 366607, "datasetid": "document", "objectid": 121215, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "2a4f5f4e58417da2d86cc81de83b5630", "hash_type": "MD5", "filesize": 26144, "mtime": "2021-06-23 21:20:39", "url": "/1771/3/indexcodes.txt" } ], "eprint_id": 1771, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2872" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2872" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2872" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/71", "datestamp": "2004-05-28", "lastmod": "2021-11-05 22:38:52", "status_changed": "2009-09-25 02:14:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "pudomprasert@cfa.harvard.edu", "id": "Udomprasert-Patricia-Simcoe", "name": { "family": "Udomprasert", "given": "Patricia Simcoe" }, "show_email": "YES" } ] }, "title": "H\u2080 from Cosmic Background Imager Observations of the Sunyaev-Zel\u2019dovich Effect in Nearby Clusters.", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology; galaxy clusters", "abstract": "We present H\u2080 results from Cosmic Background Imager (CBI) observations of the Sunyaev-Zeldovich Effect (SZE) in 7 galaxy clusters, A85, A399, A401, A478, A754, A1651, and A2597. These observations are part of a program to study a complete, volume-limited sample of low-redshift (z < 0.1), X-ray selected clusters. Our focus on nearby objects allows us to study a well-defined, orientation unbiased sample, minimizing systematic errors due to cluster asphericity. We use density models derived from ROSAT imaging data and temperature measurements from ASCA and BeppoSAX spectral observations. We quantify in detail sources of error in our derivation of H\u2080, including calibration of the CBI data, density and temperature models from the X-ray data, Cosmic Microwave Background (CMB) primary anisotropy fluctuations, and residuals from radio point source subtraction. From these 7 clusters we obtain a result of Ho = 67+30-18(ran)+15-6(sys) km/s-1 Mpc-1 for an unweighted sample average. The respective quoted errors are random and systematic uncertainties at 68% confidence. The dominant source of error is confusion from intrinsic anisotropy fluctuations. We present results from simulations of an eigenmode weighting analysis that reduce the uncertainties due to CMB in h-1/2 by ~30%.", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-05132004-184937", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05132004-184937", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-28", "doi": "10.7907/VR2Z-MP09", "alt_title": { "items": [ "H0 from Cosmic Background Imager observations of the Sunyaev-Zeldovich effect in nearby clusters" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ael@astro.caltech.edu", "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew E." }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "george@astro.caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "orcid": "0000-0002-0603-3087", "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-13", "thesis_defense_date": "2003-08-12", "thesis_approved_date": "2004-05-28", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Udomprasert, Patricia Simcoe" }, { "id": "/id/eprint/1746", "eprint_id": 1746, "rev_number": 12, "documents": [ { "id": "/id/document/2825", "doc_id": 2825, "rev_number": 2, "files": [ { "id": "/id/file/17216", "fileid": 17216, "datasetid": "document", "objectid": 2825, "filename": "hunt_thesis.pdf", "mime_type": "application/pdf", "filesize": 1280282, "mtime": "2012-12-26 02:41:33", "url": "/1746/1/hunt_thesis.pdf" } ], "eprint_id": 1746, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "hunt_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "hunt_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19549" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19549" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19549" } ] } }, { "id": "/id/document/19549", "doc_id": 19549, "rev_number": 2, "files": [ { "id": "/id/file/17214", "fileid": 17214, "datasetid": "document", "objectid": 19549, "filename": "preview.png", "mime_type": "image/png", "hash": "c37bcd7e7055612146792bb31afadafe", "hash_type": "MD5", "filesize": 14115, "mtime": "2012-12-26 02:41:33", "url": "/1746/2/preview.png" } ], "eprint_id": 1746, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2825" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2825" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2825" } ] } }, { "id": "/id/document/121175", "doc_id": 121175, "rev_number": 1, "files": [ { "id": "/id/file/366567", "fileid": 366567, "datasetid": "document", "objectid": 121175, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "5dcbec43b4a78bc1509ffc6b58b7b191", "hash_type": "MD5", "filesize": 24582, "mtime": "2021-06-23 21:19:11", "url": "/1746/3/indexcodes.txt" } ], "eprint_id": 1746, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2825" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2825" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2825" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/46", "datestamp": "2004-05-28", "lastmod": "2021-01-20 23:13:20", "status_changed": "2009-09-25 02:14:20", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hunt-Matthew-Philip", "name": { "family": "Hunt", "given": "Matthew Philip" }, "orcid": "0000-0001-6920-5563", "show_email": "NO" } ] }, "title": "Faint Optically Selected AGN at z = 3", "ispublished": "unpub", "full_text_status": "public", "keywords": "active galactic nuclei; galaxy formation; luminosity function; qsos; quasars; smbh; supermassive black holes", "abstract": "We present the results of two surveys for z \u2248 3 AGN, the Lyman break galaxy (LBG) survey and a new survey based on the same techniques, but over a wider area. These surveys, spanning more than 2 deg\u00b2, yield 24 new QSOs, and 17 new narrow-lined AGN. The combined data from these surveys span a range of luminosity that is unprecedented at high redshift, covering 6.5 mag of the faint end of the QSO luminosity function. We find a substantially flatter faint-end slope at high redshift than in the local universe, \u03b2l=1.20, which has important implications for the study of supermassive black hole (SMBH) accretion and galaxy formation, as well as the state of the IGM at z \u2248 3. We also present estimates of the QSO lifetime (~ 10\u2077 yr) and compare our AGN sample with those obtained by deep X-ray imaging. We also present a guide to the reduction of imaging data from the Large Format Camera (LFC) on the Hale Telescope.", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-05122004-113008", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05122004-113008", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-28", "doi": "10.7907/J5MJ-AP67", "alt_title": { "items": [ "Faint Optically Selected AGN at z=3" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-12", "thesis_defense_date": "2004-05-20", "thesis_approved_date": "2004-05-28", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Hunt, Matthew Philip" }, { "id": "/id/eprint/1892", "eprint_id": 1892, "rev_number": 19, "documents": [ { "id": "/id/document/3211", "doc_id": 3211, "rev_number": 2, "files": [ { "id": "/id/file/19216", "fileid": 19216, "datasetid": "document", "objectid": 3211, "filename": "book_main.pdf", "mime_type": "application/pdf", "filesize": 6429477, "mtime": "2012-12-26 02:43:39", "url": "/1892/1/book_main.pdf" } ], "eprint_id": 1892, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "book_main.pdf", "language": "en", "security": "public", "license": "other", "main": "book_main.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19904" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19904" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19904" } ] } }, { "id": "/id/document/3212", "doc_id": 3212, "rev_number": 2, "files": [ { "id": "/id/file/19220", "fileid": 19220, "datasetid": "document", "objectid": 3212, "filename": "intro.pdf", "mime_type": "application/pdf", "filesize": 852752, "mtime": "2012-12-26 02:43:39", "url": "/1892/2/intro.pdf" } ], "eprint_id": 1892, "pos": 2, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "intro.pdf", "language": "en", "security": "public", "license": "other", "main": "intro.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3216" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/18/92", "datestamp": "2004-05-21", "lastmod": "2021-01-06 00:21:32", "status_changed": "2009-09-25 02:19:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "eberger@cfa.harvard.edu", "id": "Berger-Edo", "name": { "family": "Berger", "given": "Edo" }, "orcid": "0000-0002-9392-9681", "show_email": "YES" } ] }, "title": "Cosmic Explosions: The Beasts and Their Lair", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astrophysics; Gamma-ray bursts; High-redshift galaxies; Radio astronomy; Supernovae", "abstract": "The diversity of stellar death is revealed in the energy, velocity and geometry of the explosion debris (\"ejecta\"). Using multi-wavelength observations of gamma-ray burst (GRB) afterglows I show that GRBs, arising from the death of massive stars, are marked by relativistic, collimated ejecta (\"jets\") with a wide range of opening angles. I further show that the jet opening angles are strongly correlated with the isotropic-equivalent kinetic energies, such that the true relativistic energy of GRBs is nearly standard, with a value of few times 10^51 erg. A geometry-independent analysis which relies on the simple non-relativistic dynamics of GRBs at late time confirms these inferences. Still, the energy in the highest velocity ejecta, which give rise to the prompt gamma-ray emission, is highly variable. These results suggest that various cosmic explosions are powered by a common energy source, an \"engine\" (possibly an accreting stellar-mass black hole), with their diverse appearances determined solely by the variable high velocity output. On the other hand, using radio observations I show that local type Ibc core-collapse supernovae generally lack relativistic ejecta and are therefore not powered by engines. Instead, the highest velocity debris in these sources, typically with a velocity lower than 100,000 km/sec, are produced in the (effectively) spherical ejection of the stellar envelope. The relative rates of engine- and collapse-powered explosions suggest that the former account for only a small fraction of the stellar death rate. Motivated by the connection of GRBs to massive stars, and by their ability to overcome the biases inhenert in current galaxy surveys, I investigate the relation between GRB hosts and the underlying population of star-forming galaxies. Using the first radio and submillimeter observations of GRB hosts, I show that some are extreme starburst galaxies with the bursts directly associated with the regions of most intense star formation. I suggest, by comparison to other well-studied samples, that GRBs preferentially occur in sub-luminous, low mass galaxies, undergoing the early stages of a starburst process. If confirmed with future observations, this trend will place GRBs in the forefront of star formation and galaxy evolution studies.", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-05202004-165422", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05202004-165422", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-21", "doi": "10.7907/QV7S-4S81", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "chair" }, { "email": "dfrail@nrao.edu", "id": "Frail-D-A", "name": { "family": "Frail", "given": "Dale A." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "golwala@astro.caltech.edu", "id": "Golwala-S", "name": { "family": "Golwala", "given": "Sunil" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-20", "thesis_defense_date": "2004-05-18", "thesis_approved_date": "2004-05-21", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Berger, Edo" }, { "id": "/id/eprint/2135", "eprint_id": 2135, "rev_number": 11, "documents": [ { "id": "/id/document/3883", "doc_id": 3883, "rev_number": 3, "files": [ { "id": "/id/file/22729", "fileid": 22729, "datasetid": "document", "objectid": 3883, "filename": "main_color_snglspc.pdf", "mime_type": "application/pdf", "filesize": 10431343, "mtime": "2012-12-26 02:47:23", "url": "/2135/1/main_color_snglspc.pdf" } ], "eprint_id": 2135, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "main_color_snglspc.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20531" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20531" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20531" } ] } }, { "id": "/id/document/20531", "doc_id": 20531, "rev_number": 2, "files": [ { "id": "/id/file/22727", "fileid": 22727, "datasetid": "document", "objectid": 20531, "filename": "preview.png", "mime_type": "image/png", "hash": "ef4f96eef80179125f29e67655048e39", "hash_type": "MD5", "filesize": 13197, "mtime": "2012-12-26 02:47:22", "url": "/2135/2/preview.png" } ], "eprint_id": 2135, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3883" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3883" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3883" } ] } }, { "id": "/id/document/122160", "doc_id": 122160, "rev_number": 1, "files": [ { "id": "/id/file/367554", "fileid": 367554, "datasetid": "document", "objectid": 122160, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "367ef56de6bacc450761993ed48597cb", "hash_type": "MD5", "filesize": 50923, "mtime": "2021-06-23 21:49:13", "url": "/2135/3/indexcodes.txt" } ], "eprint_id": 2135, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3883" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3883" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3883" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/21/35", "datestamp": "2004-05-28", "lastmod": "2021-01-20 23:23:28", "status_changed": "2009-09-25 02:27:49", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kaplan@uwm.edu", "id": "Kaplan-David-Lior-Ariel", "name": { "family": "Kaplan", "given": "David Lior Ariel" }, "orcid": "0000-0001-6295-2881", "show_email": "YES" } ] }, "title": "The Diversity of Neutron Stars: Nearby Thermally Emitting Neutron Stars and the Compact Central Objects in Supernova Remnants", "ispublished": "unpub", "full_text_status": "public", "keywords": "compact objects; neutron stars; supernova remnants; X-rays", "abstract": "Neutron stars are invaluable tools for exploring stellar death, the physics of ultra-dense matter, and the effects of extremely strong magnetic fields. The observed population of neutron stars is dominated by the > 1000 radio pulsars, but there are distinct sub-populations that, while fewer in number, can have significant impact on our understanding of the issues mentioned above. These populations are the nearby, isolated neutron stars discovered by ROSAT, and the central compact objects in supernova remnants. The studies of both of these populations have been greatly accelerated in recent years through observations with the Chandra X-ray Observatory and the XMM-Newton telescope. First, we discuss radio, optical, and X-ray observations of the nearby neutron stars aimed at determining their relation to the Galactic neutron star population and at unraveling their complex physical processes by determining the basic astronomical parameters that define the population--distances, ages, and magnetic fields--the uncertainties in which limit any attempt to derive basic physical parameters for these objects. We conclude that these sources are 1e6 year-old cooling neutron stars with magnetic fields above 10e13 Gauss. Second, we describe the hollow supernova remnant problem: why many of the supernova remnants in the Galaxy have no indication central neutron stars. We have undertaken an X-ray census of neutron stars in a volume-limited sample of Galactic supernova remnants, and from it conclude that either many supernovae do not produce neutron stars contrary to expectation, or that neutron stars can have a wide range in cooling behavior that makes many sources disappear from the X-ray sky.\r\n", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-05272004-150045", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05272004-150045", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-28", "doi": "10.7907/2890-AB41", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-27", "thesis_defense_date": "2004-05-24", "thesis_approved_date": "2004-05-28", "thesis_awards": "Milton and Francis Clauser Doctoral Prize, 2004", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Kaplan, David Lior Ariel" }, { "id": "/id/eprint/1677", "eprint_id": 1677, "rev_number": 10, "documents": [ { "id": "/id/document/2655", "doc_id": 2655, "rev_number": 2, "files": [ { "id": "/id/file/16312", "fileid": 16312, "datasetid": "document", "objectid": 2655, "filename": "simcoe_dissertation.pdf", "mime_type": "application/pdf", "filesize": 4534686, "mtime": "2012-12-26 02:40:36", "url": "/1677/1/simcoe_dissertation.pdf" } ], "eprint_id": 1677, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "simcoe_dissertation.pdf", "language": "en", "security": "public", "license": "other", "main": "simcoe_dissertation.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19394" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19394" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19394" } ] } }, { "id": "/id/document/19394", "doc_id": 19394, "rev_number": 2, "files": [ { "id": "/id/file/16310", "fileid": 16310, "datasetid": "document", "objectid": 19394, "filename": "preview.png", "mime_type": "image/png", "hash": "8aebf255e25adde426e3ea93afa58e4f", "hash_type": "MD5", "filesize": 15041, "mtime": "2012-12-26 02:40:36", "url": "/1677/2/preview.png" } ], "eprint_id": 1677, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2655" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2655" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2655" } ] } }, { "id": "/id/document/121055", "doc_id": 121055, "rev_number": 1, "files": [ { "id": "/id/file/366445", "fileid": 366445, "datasetid": "document", "objectid": 121055, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "bbd3596e9e997fca23e1ffcaa25ac6a8", "hash_type": "MD5", "filesize": 33917, "mtime": "2021-06-23 21:15:32", "url": "/1677/3/indexcodes.txt" } ], "eprint_id": 1677, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2655" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2655" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2655" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/16/77", "datestamp": "2004-05-27", "lastmod": "2021-01-22 00:04:51", "status_changed": "2009-09-25 02:11:39", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "simcoe@space.mit.edu", "id": "Simcoe-Robert-Andrew", "name": { "family": "Simcoe", "given": "Robert Andrew" }, "show_email": "NO" } ] }, "title": "Observations of Intergalactic Heavy-Element Enrichment in the Early Universe", "ispublished": "unpub", "full_text_status": "public", "keywords": "Chemical Enrichment; Intergalactic Medium; Lyman Alpha Forest; Star Formation", "abstract": "We present the results of a search for OVI absorption in the intergalactic medium (IGM) at 2 \u227e z \u227e 3. The measurements are taken from a set of 7 quasars observed with Keck I/HIRES. We find two classes of OVI system in the high redshift IGM. The first class is more rare (2-4 per sightline) and also quite strong (NH1\u22651015.2). These systems resemble hot, collisionally ionized gas at high densities, and contain complex mixtures of HI and metals at a range of temperatures. Although we cannot measure the metallicities of individual strong absorbers, we estimate that the total population is enriched over 10 times above the level of the general IGM. We propose that the strong systems represent either accretion-shocked gas falling onto primitive large-scale structure, or (more likely) the remnants of high redshift galactic winds mixing into the IGM.
\r\n\r\nThe second class of OVI absorber is much weaker, arising in low-density gas that is photoionized by metagalactic UV/X-ray radiation. We measure the metal content of these systems, down to densities of \u03c1/\u03c1\u0305 \u2265 1.6 relative to the cosmic mean. This corresponds to the filaments of the cosmic web, which contain over half of the baryons in the high redshift universe. We develop a new method to calculate the metallicity distribution function of the Ly-\u03b1 forest using survival statistics. Carbon and oxygen are both distributed lognormally, with mean\u3008[O/H]\u3009\u2248 -2.85 and scatter of \u03c3 = 0.75 dex. We observe no decline in metallicity toward lower densities, indicating that metals are mixed very efficiently within the filaments. Comparison with Population III and galactic wind enrichment models suggests that the enrichment was dominated by superwinds. We estimate that roughly half of all baryons in the IGM came into contact with metal-rich winds by z ~ 2.5. Using a \"closed box\" model of intergalactic enrichment, we estimate that early galaxies typically recycled 0.1-0.4% of their mass back into the IGM as heavy elements prior to this epoch.
", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-05082004-134233", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05082004-134233", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-27", "doi": "10.7907/E1N9-BF97", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "mr@ociw.edu", "id": "Rauch-M", "name": { "family": "Rauch", "given": "Michael" }, "role": "member" }, { "email": "sgd@astro.caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-08", "thesis_defense_date": "2003-08-18", "thesis_approved_date": "2004-05-27", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Simcoe, Robert Andrew" }, { "id": "/id/eprint/1382", "eprint_id": 1382, "rev_number": 12, "documents": [ { "id": "/id/document/2111", "doc_id": 2111, "rev_number": 2, "files": [ { "id": "/id/file/13149", "fileid": 13149, "datasetid": "document", "objectid": 2111, "filename": "hqw_thesis_final.pdf", "mime_type": "application/pdf", "filesize": 10675147, "mtime": "2012-12-26 02:37:42", "url": "/1382/1/hqw_thesis_final.pdf" } ], "eprint_id": 1382, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "hqw_thesis_final.pdf", "language": "en", "security": "public", "license": "other", "main": "hqw_thesis_final.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18871" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18871" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18871" } ] } }, { "id": "/id/document/16630", "doc_id": 16630, "rev_number": 3, "files": [ { "id": "/id/file/201284", "fileid": 201284, "datasetid": "document", "objectid": 16630, "filename": "Wang_Huiqun_2004.txt", "mime_type": "text/plain", "filesize": 1557, "mtime": "2016-08-22 21:14:50", "url": "/1382/2/Wang_Huiqun_2004.txt" } ], "eprint_id": 1382, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Wang_Huiqun_2004.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/18871", "doc_id": 18871, "rev_number": 2, "files": [ { "id": "/id/file/13147", "fileid": 13147, "datasetid": 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"document", "objectid": 120732, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "fc42cf4e0aab3d5736619f6f6f0c52ce", "hash_type": "MD5", "filesize": 642, "mtime": "2021-06-23 21:02:56", "url": "/1382/5/indexcodes.txt" } ], "eprint_id": 1382, "pos": 5, "placement": 5, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16630" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16630" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16630" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/13/82", "datestamp": "2004-04-15", "lastmod": "2021-01-27 21:45:57", "status_changed": "2009-09-25 02:02:47", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "hwang@cfa.harvard.edu", "id": "Wang-Huiqun-Helen", "name": { "family": "Wang", "given": "Huiqun Helen" }, "orcid": "0000-0001-9722-9992", "show_email": "YES" } ] }, "title": "Global Observations of Martian Clouds with the Mars Orbiter Camera of the Mars Global Surveyor Spacecraft", "ispublished": "unpub", "full_text_status": "public", "keywords": "clouds; Mars; Mars Global Surveyor", "abstract": "We have studied the global cloud distribution on Mars using red and blue global map swaths taken by the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC).
\r\n\r\nIn Chapters 1 and 4, we summarize the results for the first and second MGS mapping years, respectively. In Chapter 2, we investigate the mechanism for a new type of \"flushing\" dust storm first observed by MGS. These dust storms moved from the northern high latitudes southward across the equator, and led to a planet-encircling dust storm in the first MGS mapping year (1999). In Chapter 3, we track cloud motion to measure winds using images separated by 2 hours.
\r\n\r\nThe systematic daily global coverage of MGS not only provides us with detailed and coherent pictures of Martian cloud evolution, but also increases the number of cloud-tracked wind vectors by three orders of magnitude. Except for the global dust storm in the second MGS mapping year (2001), Martian weather is highly repeatable. When the 2001 global dust storm initiated, Hellas storms increased in frequency, transporting dust out of the basin daily. When the 1999 planet-encircling dust storm initiated, \"flushing\" storms also increased in frequency, transporting dust to the southern subtropics daily. These observations suggest that timely dust supply by local or regional storms could have a global impact.
", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-04142004-151205", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04142004-151205", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-04-15", "doi": "10.7907/CYNM-8830", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "bcm@gps.caltech.edu", "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "email": "aalbee@gps.caltech.edu", "id": "Albee-A-L", "name": { "family": "Albee", "given": "Arden Leroy" }, "role": "member" }, { "email": "ged@gps.caltech.edu", "id": "Danielson-E", "name": { "family": "Danielson", "given": "Ed" }, "role": "member" }, { "email": "mir@gps.caltech.edu", "id": "Richardson-M-I", "name": { "family": "Richardson", "given": "Mark I." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-04-14", "thesis_defense_date": "2003-07-18", "thesis_approved_date": "2004-04-15", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "appliedmath" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Wang, Huiqun Helen" }, { "id": "/id/eprint/2191", "eprint_id": 2191, "rev_number": 12, "documents": [ { "id": "/id/document/4032", "doc_id": 4032, "rev_number": 3, "files": [ { "id": "/id/file/23486", "fileid": 23486, "datasetid": "document", "objectid": 4032, "filename": "main.pdf", "mime_type": "application/pdf", "filesize": 2998326, "mtime": "2012-12-26 02:48:10", "url": "/2191/1/main.pdf" } ], "eprint_id": 2191, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "main.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20657" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20657" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20657" } ] } }, { "id": "/id/document/20657", "doc_id": 20657, "rev_number": 2, "files": [ { "id": "/id/file/23484", "fileid": 23484, "datasetid": "document", "objectid": 20657, "filename": "preview.png", "mime_type": "image/png", "hash": "f56c1cc76b2b06e0a950536eb37b8715", "hash_type": "MD5", "filesize": 16760, "mtime": "2012-12-26 02:48:10", "url": "/2191/2/preview.png" } ], "eprint_id": 2191, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4032" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4032" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4032" } ] } }, { "id": "/id/document/122303", "doc_id": 122303, "rev_number": 1, "files": [ { "id": "/id/file/367698", "fileid": 367698, "datasetid": "document", "objectid": 122303, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "fcea78467be93b2daa1e8697ba554111", "hash_type": "MD5", "filesize": 28765, "mtime": "2021-06-23 21:53:28", "url": "/2191/3/indexcodes.txt" } ], "eprint_id": 2191, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4032" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4032" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4032" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/21/91", "datestamp": "2004-05-28", "lastmod": "2021-11-05 22:38:29", "status_changed": "2009-09-25 02:30:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "sieversj@ukzn.ac.za", "id": "Sievers-Jonathan-LeRoy", "name": { "family": "Sievers", "given": "Jonathan LeRoy" }, "orcid": "0000-0001-6903-5074", "show_email": "YES" } ] }, "title": "Data Analysis of and Results from Observations of the Cosmic Microwave Background with the Cosmic Background Imager", "ispublished": "unpub", "full_text_status": "public", "keywords": "cmbr; cosmology; early universe; radio astronomy", "abstract": "We present results from observations of the Cosmic Microwave Background (CMB) with the Cosmic Background Imager (CBI), a sensitive 13-element interferometer located high in the Chilean Andes. We also discuss methods of analyzing the data from the CBI, including an improved way of measuring the true power spectrum using maximum likelihood estimation. This improved method leads to a saving of a factor of two in memory usage, and an increase in speed of order the number of points in the spectrum. The initial results are discussed, in which the fall-off in power at ell > 1000 (the \"damping tail\") was first observed. We also present the results from the first year of observations with the CBI, and discuss cosmological intepretations both alone and in concert with the results from other experiments. These provide tight constraints on cosmological parameters, including a Hubble constant of 69 +/- 4 km/s/Mpc, an age of the universe of 13.7 +/- 0.2 billion years, and a denisty of dark energy of 0.70 +/- 0.05 of the critical density of the universe. Finally, we discuss an alternate method of data compression, with great flexibility in what information is kept, while being computationally tractable. We then apply this method to the CBI data to constrain the potential emission from foreground contaminants contributing to the observed CMB radiation. We find that the data is consistent with zero foreground, with a maximum allowed foreground contribution between about 8% and 12% of the total signal (at an ell of 600 and frequency of 30 GHz), depending on the spectral index of foreground emission.\r\n", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-05282004-140350", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05282004-140350", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "suggestions": "jonathan.sievers@mcgill.ca", "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-28", "doi": "10.7907/8706-VY52", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "chair" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" }, { "email": "tjp@astro.caltech.edu", "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "Timothy J." }, "orcid": "0000-0001-5213-6231", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-28", "thesis_defense_date": "2003-09-30", "thesis_approved_date": "2004-05-28", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Sievers, Jonathan LeRoy" }, { "id": "/id/eprint/1748", "eprint_id": 1748, "rev_number": 15, "documents": [ { "id": "/id/document/2827", "doc_id": 2827, "rev_number": 3, "files": [ { "id": "/id/file/17231", "fileid": 17231, "datasetid": "document", "objectid": 2827, "filename": "fselman_cv.pdf", "mime_type": "application/pdf", "filesize": 53125, "mtime": "2012-12-26 02:41:34", "url": "/1748/1/fselman_cv.pdf" } ], "eprint_id": 1748, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "fselman_cv.pdf", "language": "en", "security": "internal", "license": "other", "main": "fselman_cv.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"uri": "/id/document/2827" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2827" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2827" } ] } }, { "id": "/id/document/121178", "doc_id": 121178, "rev_number": 1, "files": [ { "id": "/id/file/366570", "fileid": 366570, "datasetid": "document", "objectid": 121178, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "771143a6389907941ccd1fd8ecb344aa", "hash_type": "MD5", "filesize": 40720, "mtime": "2021-06-23 21:19:21", "url": "/1748/6/indexcodes.txt" } ], "eprint_id": 1748, "pos": 6, "placement": 6, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2828" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2828" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2828" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/48", "datestamp": "2004-05-20", "lastmod": "2023-05-30 22:33:57", "status_changed": "2009-09-25 02:14:21", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "fselman@eso.org", "id": "Selman-Fernando-Javier", "name": { "family": "Selman", "given": "Fernando Javier" }, "orcid": "0000-0002-3721-0699", "show_email": "YES" } ] }, "title": "The Initial Mass Function and Star-Formation History in the 30 Doradus Super-Association", "ispublished": "unpub", "full_text_status": "public", "keywords": "30 Doradus; Large Magellanic Cloud; massive stars; star formation; stellar Initial Mass Function", "abstract": "We present a study of the star-formation history (SFH), and the initial mass function (IMF) in the 30 Doradus super-association. The study is divided in six natural stages: (1) profile fitting photometry; (2) characterization of the instrument; (3) calibration using stars with spectroscopy; (4) visualization of the stellar properties using the color-magnitude stereogram; (5) Bayesian analysis to obtain physical quantities; and (6) the construction of the SFH and IMF. The reduction and characterization of systematic errors are the most important steps of any IMF study: we note the following sources of systematic errors: (a) the upper magnitude cut-off, used to filter out saturated and non-linear stars, results in a false steepening of the high-mass end of the IMF, particularly affecting older systems; (b) Be stars and blue B-type super-giants mimic luminosity class V stars of higher effective temperatures, thus flattening the IMF; (c) the magnitude limit effect introduced by variable reddening, that flattens the low mass end of the derived IMF. For IMF determination we have identified the mass window 10M\u2299 \u2264 M \u2264 40M\u2299, that is free of effects (a) and (c) in our photometry. We have found that the SFH of the region is characterized by a 7-15~My old burst, across the whole area studied, followed by a period of reduced, nearly constant, star-formation activity. This activity has been punctuated by clustered, burst-like, star-formation episodes of varying intensity in several places. For NGC2070, the OB association LH104, and the field, the derived IMFs are consistent with a power law with Salpeter slope only if they have different SFH: a young and almost instantaneous burst for NGC2070, and nearly constant star formation, after the 7-15 My burst for the field and LH104. Other studies reveal star-formation episodes across the LMC, starting 15-30 My ago. We propose that the origin of such an apparently synchronized, large-scale, activity, is the recent entry of the LMC into a thick disk of ionized gas, analogous to that proposed by Moore and Davis (1994) to explain the origin of the Magellanic Stream.", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-05122004-130955", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05122004-130955", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-20", "doi": "10.7907/ZKTC-0760", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "chair" }, { "email": "jmelnick@eso.org", "id": "Melnick-J", "name": { "family": "Melnick", "given": "Jorge" }, "role": "member" }, { "email": "lah@astro.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "orcid": "0000-0002-1084-3656", "role": "member" }, { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-12", "thesis_defense_date": "2003-10-28", "thesis_approved_date": "2004-05-20", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Selman, Fernando Javier" }, { "id": "/id/eprint/4274", "eprint_id": 4274, "rev_number": 17, "documents": [ { "id": "/id/document/7015", "doc_id": 7015, "rev_number": 3, "files": [ { "id": "/id/file/42651", "fileid": 42651, "datasetid": "document", "objectid": 7015, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 3791278, "mtime": "2012-12-26 03:07:06", "url": "/4274/1/thesis.pdf" } ], "eprint_id": 4274, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23544" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23544" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23544" } ] } }, { "id": "/id/document/23544", "doc_id": 23544, "rev_number": 2, "files": [ { "id": "/id/file/42649", "fileid": 42649, "datasetid": "document", "objectid": 23544, "filename": "preview.png", "mime_type": "image/png", "hash": "7503fb53c84d85889b4a677b8ca89a37", "hash_type": "MD5", "filesize": 14975, "mtime": "2012-12-26 03:07:06", "url": "/4274/2/preview.png" } ], "eprint_id": 4274, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7015" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7015" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7015" } ] } }, { "id": "/id/document/124110", "doc_id": 124110, "rev_number": 1, "files": [ { "id": "/id/file/369540", "fileid": 369540, "datasetid": "document", "objectid": 124110, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "5edf32a4b298f15fdcef7fdaa8512e4d", "hash_type": "MD5", "filesize": 30779, "mtime": "2021-06-23 23:18:50", "url": "/4274/3/indexcodes.txt" } ], "eprint_id": 4274, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7015" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7015" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/7015" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/74", "datestamp": "2003-10-28", "lastmod": "2021-01-27 20:15:40", "status_changed": "2009-09-25 03:15:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "abouchez@keck.hawaii.edu", "id": "Bouchez-Antonin-Henri", "name": { "family": "Bouchez", "given": "Antonin Henri" }, "show_email": "YES" } ] }, "title": "Seasonal Trends in Titan\u2019s Atmosphere: Haze, Wind, and Clouds", "ispublished": "unpub", "full_text_status": "public", "keywords": "planetary atmospheres; satellites of Saturn", "abstract": "I present an analysis of visible and near-infrared adaptive optics images and spectra of Titan taken over 43 nights between October 1997 and January 2003 with the AEOS 3.6-m, Palomar Hale 5-m, and W.M. Keck 10-m telescopes. These observations reveal a seasonally changing stratospheric haze layer, two distinct regions of condensate clouds in the southern hemisphere, the albedo of Titan's surface, and the zonal wind field of the stratosphere.
\r\n\r\nTransient convective CH4 clouds are identified near Titan's south pole, rising to 16\u00b15 km above the surface. These clouds have been continuously present south of 70\u00b0S since at least December 2001, currently account for 0.5-1% of Titan's 2\u03bcm flux, and appear to be gradually brightening or thickening as the insolation of the south polar region increases. Above the polar clouds, an extensive but optically thin (\u03c4\u22480.05 at 2\u03bcm) cloud layer is noted near the tropopause south of 30\u00b0S. This cirrus-like structure has remained unchanged in extent and thickness since September 1999 despite seasonal changes in the underlying convective clouds and the overlying stratospheric haze. Aside from the convective CH4 clouds near the south pole, Titan's troposphere is free of aerosols with an upper limit of \u03c4<0.01 on the 2\u03bcm vertical optical depth in the 5-30 km altitude region.
\r\n\r\nThe albedo of Titan's surface at 2.0\u03bcm is derived from the radiative transfer analysis of spatially resolved spectra and images, and presented in the form of a ~600 km resolution global surface albedo map. At this resolution, the 2.0\u03bcm albedo ranges from 0.05 to 0.17, consistent with extensive exposure of clean water ice in some regions, while hydrocarbons and atmospheric sediments blanket others.
\r\n\r\nThe zonal wind field of Titan's stratosphere near southern summer solstice is derived from adaptive optics observations of the occultation of a binary star on 20 December 2001. Multiple refracted stellar images were detected on Titan's limb during the each successive occultation, allowing the angular deflection of the starlight at two altitudes over both hemispheres to be measured with an uncertainty of ~2 milliarcseconds. The zonal wind field derived from this measurement of the shape of Titan's limb exhibits strong but asymmetric high latitude jets, with peak wind speeds of 230\u00b120 m s-1 at 60\u00b0N and 160\u00b140 m s-1 at 40\u00b0S, and lower winds of 110\u00b140 m s-1 at the equator. The direction of the wind is not constrained.
", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-10272003-092206", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10272003-092206", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-10-28", "doi": "10.7907/7KVP-D712", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "chair" }, { "email": "mir@gps.caltech.edu", "id": "Richardson-M-I", "name": { "family": "Richardson", "given": "Mark I." }, "role": "member" }, { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-10-27", "thesis_defense_date": "2003-07-25", "thesis_approved_date": "2003-10-28", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Bouchez, Antonin Henri" }, { "id": "/id/eprint/1855", "eprint_id": 1855, "rev_number": 15, "documents": [ { "id": "/id/document/3115", "doc_id": 3115, "rev_number": 4, "files": [ { "id": "/id/file/18712", "fileid": 18712, "datasetid": "document", "objectid": 3115, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 2798490, "mtime": "2012-12-26 02:43:09", "url": "/1855/1/thesis.pdf" } ], "eprint_id": 1855, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Full thesis", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"uri": "/id/document/3115" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3115" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3115" } ] } }, { "id": "/id/document/121415", "doc_id": 121415, "rev_number": 1, "files": [ { "id": "/id/file/366807", "fileid": 366807, "datasetid": "document", "objectid": 121415, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "5f09311cfad96c569d76be26d372082c", "hash_type": "MD5", "filesize": 2142, "mtime": "2021-06-23 21:25:46", "url": "/1855/6/indexcodes.txt" } ], "eprint_id": 1855, "pos": 6, "placement": 6, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3116" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3116" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/3116" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/18/55", "datestamp": "2004-05-20", "lastmod": "2021-01-21 23:17:07", "status_changed": "2009-09-25 02:17:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mrs@ast.cam.ac.uk", "id": "Santos-Michael-Robert", "name": { "family": "Santos", "given": "Michael Robert" }, "show_email": "NO" } ] }, "title": "Galaxy Formation Near the Epoch of Reionization", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology", "abstract": "I present five explorations of the formation of early galaxies near the epoch of reionization: observable phenomena that demonstrate the interaction between galaxy formation and the intergalactic medium.
\r\n\r\nI calculated the contribution of the first stars (Pop III) to the cosmic infrared background (CIRB). Pop III stars produced the observed unexplained component of the NIR CIRB if they were very massive and formed efficiently over a redshift range 25 \u2273 z \u2273 7. A small escape fraction of ionizing photons from the nebular gas immediately surrounding the Pop III stars enhances the Pop III CIRB signal.
\r\n\r\nI calculated the effect of radiative transfer through the intergalactic medium (IGM) on the observed properties of Lyman alpha emission lines from z \u2273 6 galaxies. The detection of a Lyman alpha emitting galaxy at z = 6.5 resulted in claims that the universe was mostly ionized there. With existing information about the source galaxy it is almost impossible to deduce the ionization state of the z = 6.5 IGM, especially if there were galactic-scale super-winds.
\r\n\r\nI present a method to infer the stellar population responsible for completing reionization. We simulated helium and hydrogen absorption along lines-of-sight toward high-redshift QSOs assuming either Pop II or Pop III stars dominated the UV background at z=5. The final SDSS quasar sample may contain a quasar/line-of-sight combination that constrains the nature of the dominant ionizing sources only 300 Myr after the end of reionization.
\r\n\r\nI present an observational survey of low-luminosity Lyman alpha emitting galaxies at 4.5 < z < 6.7. This unprecedented survey utilized strong lensing by rich clusters of galaxies at intermediate redshifts to discover six likely Lyman alpha emitting galaxies. The z ~ 5 Lyman alpha luminosity function may be flatter than the mass function of dark matter halos, a sign of suppression of the star-formation efficiency in low-mass halos. However, our data by themselves are consistent with the slope of the halo mass function.
\r\n\r\nI modeled the formation of metal-poor globular cluster systems (GCSs), invoking reionization to explain the bimodality observed in GCS metallicity distributions. The model reproduces the mass and spatial extent of the Milky Way metal-poor GCS, and also the increasing number of metal-poor globular clusters per unit galaxy mass for galaxies in richer environments, as observed.
", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-05182004-154315", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05182004-154315", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-20", "doi": "10.7907/X9XT-YT35", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "advisor" }, { "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "awb@astro.caltech.edu", "id": "Blain-A-W", "name": { "family": "Blain", "given": "Andrew W." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-18", "thesis_defense_date": "2003-09-12", "thesis_approved_date": "2004-05-20", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "Santos, Michael Robert" }, { "id": "/id/eprint/3017", "eprint_id": 3017, "rev_number": 13, "documents": [ { "id": "/id/document/5408", "doc_id": 5408, "rev_number": 3, "files": [ { "id": "/id/file/31847", "fileid": 31847, "datasetid": "document", "objectid": 5408, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 1513234, "mtime": "2012-12-26 02:56:16", "url": "/3017/1/thesis.pdf" } ], "eprint_id": 3017, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21953" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21953" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21953" } ] } }, { "id": "/id/document/21953", "doc_id": 21953, "rev_number": 2, "files": [ { "id": "/id/file/31845", "fileid": 31845, "datasetid": "document", "objectid": 21953, "filename": "preview.png", "mime_type": "image/png", "hash": "259fad0e50207acb6402682aa2c29489", "hash_type": "MD5", "filesize": 13294, "mtime": "2012-12-26 02:56:15", "url": "/3017/2/preview.png" } ], "eprint_id": 3017, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5408" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5408" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5408" } ] } }, { "id": "/id/document/123296", "doc_id": 123296, "rev_number": 1, "files": [ { "id": "/id/file/368706", "fileid": 368706, "datasetid": "document", "objectid": 123296, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "8da8e8e525f648f0f845b64ba9588a95", "hash_type": "MD5", "filesize": 33976, "mtime": "2021-06-23 22:32:22", "url": "/3017/3/indexcodes.txt" } ], "eprint_id": 3017, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5408" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5408" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/5408" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/30/17", "datestamp": "2003-08-15", "lastmod": "2021-01-21 00:59:32", "status_changed": "2009-09-25 02:49:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "richard.oshaughnessy@ligo.org", "id": "O'Shaughnessy-Richard-William", "name": { "family": "O'Shaughnessy", "given": "Richard William" }, "orcid": "0000-0001-5832-8517", "show_email": "YES" } ] }, "title": "Topics in Gravitational-Wave Astronomy", "ispublished": "unpub", "full_text_status": "public", "keywords": "LIGO; LISA; numerical relativity; symmetric hyperbolic partial differential equation; thermoelastic noise", "abstract": "Both the Laser Interferometer Gravitational Wave Observatory (LIGO) and the Laser Interferometer Space Antenna (LISA) will over the next decade detect gravitational waves emitted by the motion of compact objects (e.g. black hole and neutron star binaries). This thesis presents methods to improve (i) LIGO detector quality, (ii) our knowledge of waveforms for certain LIGO and LISA sources, and (iii) models for the rate of detectability of a particular LISA source.
\r\n\t\t\t\t\t\t\t\t\t \r\n1) Plunge of compact object into a supermassive black hole: LISA should detect many inspirals of compact objects into supermassive black holes (~ 10\u2075-10\u2077 M\u2299). Since the inspiral of each compact object terminates shortly after the inspiralling object reaches its last stable orbit, the late-stage inspiral waveform provides insight into the location of the last stable orbit and strong-field relativity. I discovered that while LISA will easily see the overall inspiral (consisting of many cycles before plunge), the present LISA design will just miss detecting the waves emitted from the transition from inspiral to plunge.
\r\n\r\n2) Scheme to reduce thermoelastic noise in advanced LIGO: After its first upgrade, LIGO will have its sensitivity limited by thermoelastic noise. [Thermoelastic noise occurs because milimeter-scale thermal fluctuations in the mirror bulk expand and contract, causing the mirror surface to shimmer.] The interferometer's sensitivity could be enhanced substantially by reducing thermoelastic noise. In collaboration with Kip Thorne, Erika d'Ambrosio, Sergey Vyatchanin, and Sergey Strigin, I developed a proposal to reduce thermoelastic noise in advanced-LIGO by switching the LIGO cavity optics from simple spherical mirrors to a new, Mexican-hat shape.
\r\n\t\t\t\t\t\t\t\t\t \r\n3) Geometric-optics-based analysis of stability of symmetric-hyperbolic formulations of Einstein's equations: Einstein's equations must be evolved numerically to predict accurate waveforms for the late stages of binary black hole inspiral and merger. But no matter which representation of Einstein's equations is used, numerical simulations rarely run long. For examle, for first-order symmetric-hyperbolic (FOSH) formulations of Einstein's evolution equations, sometimes exact but unphysical solutions grow so large that the evolution fails. For FOSH formulations, I found easily-understood solutions (wave packets) and used them to predict which formulations will be particularly ill-behaved.
", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-08052003-161044", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08052003-161044", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-0099568" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department", "LIGO" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-08-15", "doi": "10.7907/4C1K-VZ17", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" }, { "email": "lindblom@tapir.caltech.edu", "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-08-05", "thesis_defense_date": "2003-07-29", "thesis_approved_date": "2003-08-15", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2004", "author_list": "O'Shaughnessy, Richard William" }, { "id": "/id/eprint/286", "eprint_id": 286, "rev_number": 11, "documents": [ { "id": "/id/document/431", "doc_id": 431, "rev_number": 2, "files": [ { "id": "/id/file/2731", "fileid": 2731, "datasetid": "document", "objectid": 431, "filename": "amc_thesis.pdf", "mime_type": "application/pdf", "filesize": 1296138, "mtime": "2012-12-26 02:28:38", "url": "/286/1/amc_thesis.pdf" } ], "eprint_id": 286, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "amc_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "amc_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17256" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17256" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17256" } ] } }, { "id": "/id/document/17256", "doc_id": 17256, "rev_number": 2, "files": [ { "id": "/id/file/2729", "fileid": 2729, "datasetid": "document", "objectid": 17256, "filename": "preview.png", "mime_type": "image/png", "hash": "db2baf795f54d6ea5d360eda23f7251f", "hash_type": "MD5", "filesize": 19361, "mtime": "2012-12-26 02:28:38", "url": "/286/2/preview.png" } ], "eprint_id": 286, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/431" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/431" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/431" } ] } }, { "id": "/id/document/119809", "doc_id": 119809, "rev_number": 1, "files": [ { "id": "/id/file/365177", "fileid": 365177, "datasetid": "document", "objectid": 119809, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "b460c16f5dd7606724bdc3b47190fef0", "hash_type": "MD5", "filesize": 32951, "mtime": "2021-06-23 20:21:00", "url": "/286/3/indexcodes.txt" } ], "eprint_id": 286, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/431" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/431" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/431" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/02/86", "datestamp": "2003-01-27", "lastmod": "2021-02-11 19:53:59", "status_changed": "2009-09-25 01:33:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chandler-Adam-Matthew", "name": { "family": "Chandler", "given": "Adam Matthew" }, "show_email": "NO" } ] }, "title": "Pulsar Searches: From Radio to Gamma-Rays", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "We report the results of four different pulsar searches, covering radio, X-ray, and gamma-ray wavelengths. These searches targeted pulsars in virtually all of their guises: young and old, long-period and short-period, accretion-powered and rotation-powered. Ten new pulsars were discovered.
\r\n\r\nThere are very few known gamma-ray pulsars, all of which were found by folding gamma-ray data with a pulse period known from other wavelengths. Some emission models indicate that there may be a large number of gamma-ray pulsars that are undetectable at lower energies. We searched several of the brightest unidentified gamma-ray sources for pulsations. This was the first attempt to identify gamma-ray pulsars by a direct search of gamma-ray data. No new identifications resulted and we report upper limits.
\r\n\r\nEven more rare than gamma-ray pulsars are accreting millisecond pulsars. We searched for coherent pulsations from Aql X-1, a low-mass X-ray binary suspected of harboring such an object. No pulsations were detected, and we argue that the quiescent emission of this system has a thermal origin (i.e., it is not due to low-level accretion).
\r\n\r\nThe two radio searches included here were both designed to detect millisecond pulsars. First, we report the results of a large area survey from Arecibo. Five new slow pulsars were discovered, including an apparent orthogonal rotator and an extremely unusual bursting radio pulsar. No short-period pulsars were discovered and we place some of the first useful observational constraints on the limiting spin period of a neutron star.
\r\n\r\nWe also performed pointed searches of several globular clusters using the new Green Bank Telescope. Three new binary millisecond pulsars were found in M62. These were the first new objects found with the GBT, and they bring the total pulsar population in M62 to six. We also discovered two isolated pulsars, one each in NGC 6544 and NGC 6624.
\r\n\r\nMany of the methods we developed will be relevant to future searches. Perhaps the most significant contribution is a dynamic power spectrum-based technique that finally allows sensitive searches for binary pulsars whose orbital periods are of the same order as the observation time.
", "date": "2003", "date_type": "degree", "id_number": "CaltechETD:etd-01232003-213508", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01232003-213508", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-01-27", "doi": "10.7907/MDJX-M255", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "prince@srl.caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "chair" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" }, { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-01-23", "thesis_defense_date": "2002-12-05", "thesis_approved_date": "2003-01-27", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"datestamp": "2014-03-12 16:28:12", "lastmod": "2021-02-11 23:53:34", "status_changed": "2014-03-12 16:28:12", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ytliu@illinois.edu", "id": "Liu-Yuk-Tung", "name": { "family": "Liu", "given": "Yuk Tung" }, "show_email": "NO" } ] }, "title": "Dynamical Stability of Nascent Neutron Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis presents a study of the dynamical stability of nascent neutron stars resulting from the\r\naccretion induced collapse of rapidly rotating white dwarfs.
\r\n\r\nChapter 2 and part of Chapter 3 study the equilibrium models for these neutron stars. They are\r\nconstructed by assuming that the neutron stars have the same masses, angular momenta, and specific\r\nangular momentum distributions as the pre-collapse white dwarfs. If the pre-collapse white dwarf is\r\nrapidly rotating, the collapsed object will contain a high density central core of size about 20 km,\r\nsurrounded by a massive accretion torus extending to hundreds of kilometers from the rotation axis.\r\nThe ratio of the rotational kinetic energy to gravitational binding energy, \u03b2, of these neutron stars\r\nis all found to be less than 0.27.
\r\n\r\nChapter 3 studies the dynamical stability of these neutron stars by numerically evolving the\r\nlinearized hydrodynamical equations. A dynamical bar-mode instability is observed when the \u03b2 of\r\nthe star is greater than the critical value \u03b2d \u2248 0.25. It is expected that the unstable mode will\r\npersist until a substantial amount of angular momentum is carried away by gravitational radiation.\r\nThe detectability of these sources is studied and it is estimated that LIGO II is unlikely to detect\r\nthem unless the event rate is greater than 10-6/year/galaxy.
\r\n\r\nAll the calculations on the structure and stability of the neutron stars in Chapters 2 and 3\r\nare carried out using Newtonian hydrodynamics and gravity. Chapter 4 studies the relativistic\r\neffects on the structure of these neutron stars. New techniques are developed and used to construct\r\nneutron star models to the first post-Newtonian (1PN) order. The structures of the 1PN models\r\nare qualitatively similar to the corresponding Newtonian models, but the values of \u03b2 are somewhat\r\nsmaller. The maximum \u03b2 for these 1PN neutron stars is found to be 0.24, which is 8% smaller than\r\nthe Newtonian result (0.26). However, relativistic effects will also change the critical value \u03b2d. A\r\ndetailed post-Newtonian stability analysis has yet to be carried out to study the relativistic effects\r\non the dynamical stability of these neutron stars.
", "date": "2003", "date_type": "degree", "id_number": "CaltechTHESIS:03112014-101628149", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03112014-101628149", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9796079" }, { "agency": "NSF", "grant_number": "PHY-9900776" }, { "agency": "NSF", "grant_number": "AST-9731698" }, { "agency": "NASA", "grant_number": "NAG5-4093" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2014-03-12 16:28:12", "doi": "10.7907/61ZS-XQ28", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" }, { "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2002-05-08", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2003", "author_list": "Liu, Yuk Tung" }, { "id": "/id/eprint/1485", "eprint_id": 1485, "rev_number": 11, "documents": [ { "id": "/id/document/2259", "doc_id": 2259, "rev_number": 3, "files": [ { "id": "/id/file/14085", "fileid": 14085, "datasetid": "document", "objectid": 2259, "filename": "shapley_cv.pdf", "mime_type": "application/pdf", "filesize": 30073, "mtime": "2012-12-26 02:38:27", "url": "/1485/1/shapley_cv.pdf" } ], "eprint_id": 1485, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "shapley_cv.pdf", "language": "en", "security": "internal", "license": "other", "main": "shapley_cv.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", 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"uri": "/id/document/2259" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2259" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2259" } ] } }, { "id": "/id/document/120792", "doc_id": 120792, "rev_number": 1, "files": [ { "id": "/id/file/366180", "fileid": 366180, "datasetid": "document", "objectid": 120792, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "74ba080087428418badd92bc8b134cb6", "hash_type": "MD5", "filesize": 29149, "mtime": "2021-06-23 21:06:01", "url": "/1485/6/indexcodes.txt" } ], "eprint_id": 1485, "pos": 6, "placement": 6, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2260" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2260" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2260" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/14/85", "datestamp": "2003-04-24", "lastmod": "2021-02-12 00:48:04", "status_changed": "2009-09-25 02:05:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "aes@astro.ucla.edu", "id": "Shapley-Alice-Eve", "name": { "family": "Shapley", "given": "Alice Eve" }, "orcid": "0000-0003-3509-4855", "show_email": "YES" } ] }, "title": "Detailed Astrophysical Properties of Lyman Break Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "galaxy evolution; galaxy formation; high-redshift galaxies; observational cosmology; starburst galaxies", "abstract": "A large statistical sample of z~3 galaxies has been efficiently UV-color-selected, and confirmed spectroscopically. Here we present additional observations providing insight into the physical conditions in these Lyman Break Galaxies (LBGs), selected to be rapidly forming stars when the universe was ~15% of its current age. In Part I, we present the results of an optical/IR survey of 118 LBGs. The distribution of LBG optical/IR colors is used in conjunction with the rest-frame UV luminosity function to construct the rest-frame optical luminosity function and luminosity density of LBGs. Broad-band optical/IR spectral energy distributions are used to model the stellar populations of LBGs, and an evolutionary sequence is proposed to explain the observations. In Part II, we utilize the large database of ~1000 individual rest-frame UV LBG spectra to construct high S/N composite spectra. The composite spectra provide information about hot stars, dust, ionized gas in H II regions, and the large-scale outflows of neutral and ionized interstellar material propelled out of the galaxies by the mechanical energy injected into the interstellar medium by frequent supernova explosions. An analysis of the composite LBG spectra uncovers strong trends among the continuum and spectroscopic properties of these star-forming galaxies, and highlights the importance of outflows in determining the overall UV spectroscopic appearance. While the composite spectra reveal many properties of the galaxies, they are limited by low spectral resolution and the loss of information incurred by averaging over large samples of galaxies. Therefore, in Part III, we present some new results from a pilot program to obtain deep, higher-resolution spectroscopic observations of individual bright LBGs. With these observations, we hope to place much tighter constraints on the properties of the outflows in LBGs, and the amount of mass, energy, and metals they return to the surrounding intergalactic medium. We also present other future directions to be pursued.", "date": "2003", "date_type": "degree", "id_number": "CaltechETD:etd-04242003-004156", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04242003-004156", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-04-24", "doi": "10.7907/6F95-VD13", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "wws@astro.caltech.edu", "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "email": "rse@astro.caltech.edu", "id": "Ellis-R-S", "name": { "family": "Ellis", "given": "Richard S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-04-24", "thesis_defense_date": "2003-04-17", "thesis_approved_date": "2003-04-24", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2003", "author_list": "Shapley, Alice Eve" }, { "id": "/id/eprint/2230", "eprint_id": 2230, "rev_number": 12, "documents": [ { "id": "/id/document/4122", "doc_id": 4122, "rev_number": 2, "files": [ { "id": "/id/file/23954", "fileid": 23954, "datasetid": "document", "objectid": 4122, "filename": "jkc_thesis.pdf", "mime_type": "application/pdf", "filesize": 6078828, "mtime": "2012-12-26 02:48:36", "url": "/2230/1/jkc_thesis.pdf" } ], "eprint_id": 2230, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "jkc_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "jkc_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"disk0/00/00/22/30", "datestamp": "2003-05-29", "lastmod": "2021-11-05 22:39:28", "status_changed": "2009-09-25 02:31:25", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cartwright-John-Kenneth", "name": { "family": "Cartwright", "given": "John Kenneth" }, "show_email": "NO" } ] }, "title": "A Limit on the Polarization of the Cosmic Microwave Background Radiation", "ispublished": "unpub", "full_text_status": "public", "keywords": "CMB; CMBR; cosmic microwave background radiation; cosmology; microwave; microwave instrumentation; polarization", "abstract": "We describe polarization observations of the CMBR with the Cosmic Background Imager, a 13-element interferometer which operates in the 26-36 GHz band and is located on the Llano de Chajnantor in northern Chile. The array consists of 90 cm Cassegrain antennas mounted on a steerable platform which can be rotated about the optical axis to facilitate polarization observations. The CBI employs single-mode circularly polarized receivers and it samples multipoles from \u2113 ~ 400 to \u2113 ~ 4250. The instrumental polarization of the CBI was calibrated with 3C279, a bright polarized point source which was monitored with the VLA. Observations of two deep fields during the 2000 season yielded three limits (95% c.l.) for C\u2113EE under the assumption that C\u2113BB = 0: 7.0 \u00b5K (\u2113 = 603); 12.8 \u00b5K (\u2113 = 1144); and 25.1 \u00b5K (\u2113 = 2048). The low-\u2113 limit approaches the levels of fluctuations predicted by standard models.
\r\n\r\nThis thesis also entailed the design and implementation of several major components of the CBI signal chain including the downconverter, the noise calibration system, and the low noise HEMT amplifiers. We discuss the design and performance of these critical systems.
", "date": "2003", "date_type": "degree", "id_number": "CaltechETD:etd-05292003-131234", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05292003-131234", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-05-29", "doi": "10.7907/D3CT-YV96", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "chair" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew E." }, "role": "member" }, { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "member" }, { "id": "Padin-S", "name": { "family": "Padin", "given": "Steve" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-05-29", "thesis_defense_date": "2002-11-12", "thesis_approved_date": "2003-05-29", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2003", "author_list": "Cartwright, John Kenneth" }, { "id": "/id/eprint/8107", "eprint_id": 8107, "rev_number": 27, "documents": [ { "id": "/id/document/46388", "doc_id": 46388, "rev_number": 3, "files": [ { "id": "/id/file/135924", "fileid": 135924, "datasetid": "document", "objectid": 46388, "filename": "Purdue_pm_2003.pdf", "mime_type": "application/pdf", "hash": "5e85a3d96f550d26a498faff06f0c01a", "hash_type": "MD5", "filesize": 29542394, "mtime": "2014-03-06 17:05:30", "url": "/8107/1/Purdue_pm_2003.pdf" } ], "eprint_id": 8107, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Purdue_pm_2003.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 87, "dir": "disk0/00/00/81/07", "datestamp": "2014-03-06 17:33:39", "lastmod": "2021-02-12 00:33:32", "status_changed": "2014-03-06 17:33:39", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Purdue-Patricia-Marie", "name": { "family": "Purdue", "given": "Patricia Marie" }, "show_email": "NO" } ] }, "title": "Topics in LIGO-Related Physics: Interferometric Speed Meters and Tidal Work", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics ", "abstract": "In the quest to develop viable designs for third-generation optical interferometric gravitational-wave\r\ndetectors, one strategy is to monitor the relative momentum or speed of the test-mass mirrors,\r\nrather than monitoring their relative position. The most straightforward design for a speed-meter\r\ninterferometer that accomplishes this is described and analyzed in Chapter 2. This design (due\r\nto Braginsky, Gorodetsky, Khalili, and Thorne) is analogous to a microwave-cavity speed meter\r\nconceived by Braginsky and Khalili. A mathematical mapping between the microwave speed meter\r\nand the optical interferometric speed meter is developed and used to show (in accord with the speed\r\nbeing a quantum nondemolition observable) that in principle the interferometric speed meter can\r\nbeat the gravitational-wave standard quantum limit (SQL) by an arbitrarily large amount, over an\r\narbitrarily wide range of frequencies . However, in practice, to reach or beat the SQL, this specific\r\nspeed meter requires exorbitantly high input light power. The physical reason for this is explored,\r\nalong with other issues such as constraints on performance due to optical dissipation.
\r\n\r\nChapter 3 proposes a more sophisticated version of a speed meter. This new design requires\r\nonly a modest input power and appears to be a fully practical candidate for third-generation LIGO.\r\nIt can beat the SQL (the approximate sensitivity of second-generation LIGO interferometers) over\r\na broad range of frequencies (~ 10 to 100 Hz in practice) by a factor h/hSQL ~ \u221aW^(SQL)_(circ)/Wcirc.\r\nHere Wcirc is the light power circulating in the interferometer arms and WSQL \u2243 800 kW is the\r\ncirculating power required to beat the SQL at 100 Hz (the LIGO-II power). If squeezed vacuum\r\n(with a power-squeeze factor e-2R) is injected into the interferometer's output port, the SQL can\r\nbe beat with a much reduced laser power: h/hSQL ~ \u221aW^(SQL)_(circ)/Wcirce-2R. For realistic parameters\r\n(e-2R \u2243 10 and Wcirc \u2243 800 to 2000 kW), the SQL can be beat by a factor ~ 3 to 4 from 10\r\nto 100 Hz. [However, as the power increases in these expressions, the speed meter becomes more\r\nnarrow band; additional power and re-optimization of some parameters are required to maintain the\r\nwide band.] By performing frequency-dependent homodyne detection on the output (with the aid\r\nof two kilometer-scale filter cavities), one can markedly improve the interferometer's sensitivity at\r\nfrequencies above 100 Hz.
\r\n\r\nChapters 2 and 3 are part of an ongoing effort to develop a practical variant of an interferometric\r\nspeed meter and to combine the speed meter concept with other ideas to yield a promising third-\r\ngeneration interferometric gravitational-wave detector that entails low laser power.
\r\n\r\nChapter 4 is a contribution to the foundations for analyzing sources of gravitational waves for\r\nLIGO. Specifically, it presents an analysis of the tidal work done on a self-gravitating body (e.g., a\r\nneutron star or black hole) in an external tidal field (e.g., that of a binary companion). The change\r\nin the mass-energy of the body as a result of the tidal work, or \"tidal heating,\" is analyzed using the\r\nLandau-Lifshitz pseudotensor and the local asymptotic rest frame of the body. It is shown that the\r\nwork done on the body is gauge invariant, while the body-tidal-field interaction energy contained\r\nwithin the body's local asymptotic rest frame is gauge dependent. This is analogous to Newtonian\r\ntheory, where the interaction energy is shown to depend on how one localizes gravitational energy,\r\nbut the work done on the body is independent of that localization. These conclusions play a role\r\nin analyses, by others, of the dynamics and stability of the inspiraling neutron-star binaries whose\r\ngravitational waves are likely to be seen and studied by LIGO.
", "date": "2003", "date_type": "degree", "id_number": "CaltechTHESIS:03062014-090212906", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03062014-090212906", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department", "LIGO" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2014-03-06 17:33:39", "doi": "10.7907/0YKJ-SW34", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2002-06-18", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2003", "author_list": "Purdue, Patricia Marie" }, { "id": "/id/eprint/877", "eprint_id": 877, "rev_number": 55, "documents": [ { "id": "/id/document/1310", "doc_id": 1310, "rev_number": 5, "files": [ { "id": "/id/file/8248", "fileid": 8248, "datasetid": "document", "objectid": 1310, "filename": "Chapter1_doubleside.pdf", "mime_type": "application/pdf", "filesize": 310026, "mtime": "2012-12-26 02:33:07", "url": "/877/1/Chapter1_doubleside.pdf" } ], "eprint_id": 877, "pos": 1, "placement": 3, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Chapter1_doubleside.pdf", "language": "en", "security": "public", "license": "other", "main": "Chapter1_doubleside.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { 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20:42:49", "url": "/877/36/indexcodes.txt" } ], "eprint_id": 877, "pos": 36, "placement": 36, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1321" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1321" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/1321" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/08/77", "datestamp": "2003-03-06", "lastmod": "2021-02-11 00:55:54", "status_changed": "2009-09-25 01:48:30", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "lfenton@seti.org", "id": "Fenton-Lori-Kay", "name": { "family": "Fenton", "given": "Lori Kay" }, "orcid": "0000-0001-8116-4901", "show_email": "NO" } ] }, "title": "Aeolian Processes on Mars: Atmospheric Modeling and GIS Analysis", "ispublished": "unpub", "full_text_status": "public", "keywords": "climate change; dunes; dust; dust devils; eolian processes; GCM; geomorphology; GFDL; global circulation model; mesoscale model; MM5; Noachis Terra; obliquity variations; sand; sedimentary history; wind stress", "abstract": "Wind is currently the dominant geological agent acting on the surface of Mars. A study of Martian aeolian activity leads to an understanding of the forces that have sculpted the planet's face over the past billion years or more and to the potential discovery of climate shifts recorded in surface wind features that reflect ancient wind patterns. This work takes advantage of newly available tools and data to reconstruct the sedimentary history reflected in aeolian features on Mars. The thesis is divided into two main projects. In the first section, a widely accepted hypothesis, that oscillations in Martian orbital parameters influence atmospheric circulation patterns, is challenged. A Mars global circulation model is run at different obliquity, eccentricity, and perihelion states and the predicted surface wind orientations are correlated with observed aeolian features on the Martian surface. The model indicates that orbital parameters have little effect on wind patterns, suggesting that aeolian features not aligned with the current wind regime must have formed under atmospheric conditions unrelated to orbital parameters. In the second project, new spacecraft data and a mesoscale model are used to determine the sedimentary history of Proctor Crater, a 150 km diameter crater in the southern highlands of Mars. Using high-resolution imagery, topography, composition, and thermal information, a GIS was constructed to study the aeolian history of the crater, which was found to have a complex interaction of deposition and erosion. Surficial features include 450 m of sediments filling the crater basin, small bright bedforms, dust devil tracks, and a dark dunefield consisting of coarse, basaltic sand and containing slipfaces indicative of a multidirectional, convergent wind regime. All wind features, both ancient and contemporary, are coaligned, indicating that formative wind directions have changed little since the first aeolian features formed in this area. Mesoscale model runs over Proctor Crater indicate that two dune slipfaces are created by winter afternoon geostrophic westerlies and summer evening katabatic easterlies, and that dust devil tracks are created by summer noontime rotational westerlies. Using all available tools, this thesis begins the work of understanding how aeolian processes have influenced the Martian surface.\r\n", "date": "2003", "date_type": "degree", "id_number": "CaltechETD:etd-03052003-124751", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03052003-124751", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-03-06", "doi": "10.7907/C9V4-8050", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "chair" }, { "email": "aalbee@caltech.edu", "id": "Albee-A-L", "name": { "family": "Albee", "given": "Arden Leroy" }, "role": "member" }, { "email": "bcm@gps.caltech.edu", "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "member" }, { "email": "sieh@gps.caltech.edu", "id": "Sieh-K-E", "name": { "family": "Sieh", "given": "Kerry E." }, "role": "member" }, { "email": "mir@gps.caltech.edu", "id": "Richardson-M-I", "name": { "family": "Richardson", "given": "Mark I." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-03-05", "thesis_defense_date": "2003-02-03", "thesis_approved_date": "2003-03-06", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "eleceng" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2003", "author_list": "Fenton, Lori Kay" }, { "id": "/id/eprint/2286", "eprint_id": 2286, "rev_number": 13, "documents": [ { "id": "/id/document/4303", "doc_id": 4303, "rev_number": 3, "files": [ { "id": "/id/file/24885", "fileid": 24885, "datasetid": "document", "objectid": 4303, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 4577313, "mtime": "2012-12-26 02:49:35", "url": "/2286/1/thesis.pdf" } ], "eprint_id": 2286, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20890" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20890" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20890" } ] } }, { "id": "/id/document/20890", "doc_id": 20890, "rev_number": 2, "files": [ { "id": "/id/file/24883", "fileid": 24883, "datasetid": "document", "objectid": 20890, "filename": "preview.png", "mime_type": "image/png", "hash": "750c5215e65862d9d23097f3ab7f4243", "hash_type": "MD5", "filesize": 16345, "mtime": "2012-12-26 02:49:35", "url": "/2286/2/preview.png" } ], "eprint_id": 2286, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4303" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4303" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4303" } ] } }, { "id": "/id/document/122571", "doc_id": 122571, "rev_number": 1, "files": [ { "id": "/id/file/367969", "fileid": 367969, "datasetid": "document", "objectid": 122571, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "4be08110b6e448a2b63ed4627b6a7c37", "hash_type": "MD5", "filesize": 49725, "mtime": "2021-06-23 22:01:01", "url": "/2286/3/indexcodes.txt" } ], "eprint_id": 2286, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4303" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4303" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4303" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/22/86", "datestamp": "2003-05-30", "lastmod": "2021-11-05 18:15:51", "status_changed": "2009-09-25 02:33:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "yanbei@tapir.caltech.edu", "id": "Chen-Yanbei", "name": { "family": "Chen", "given": "Yanbei" }, "orcid": "0000-0002-9730-9463", "show_email": "NO" } ] }, "title": "Topics of LIGO Physics: Quantum Noise in Advanced Interferometers and Template Banks for Compact-Binary Inspirals", "ispublished": "unpub", "full_text_status": "public", "keywords": "black-hole binaries; gravitational waves; quantum measurement; quantum non-demolition", "abstract": "This thesis deals with the planning for advanced interferometric gravitational-wave detectors, as well as the detection of inspiral waves using first-generation interferometers.\r\n\r\nIn Chapters 2 -- 4 (in collaboration with Alessandra Buonanno), the the signal recycling interferometer proposed for LIGO-II is studied in the two-photon formalism. This study reveals the optical spring effect, which allows the interferometer to beat the standard quantum limit, while in the same time introduces a dynamical instability. A classical control system is designed to suppress this instability. In Chapter 5 (in collaboration with Alessandra Buonanno and Nergis Mavalvala), the quantum noise in heterodyne readout schemes for advanced interferometers is studied. In Chapter 6 (in collaboration with Patricia Purdue), a QND Speed-Meter interferometer with Michelson topology is proposed, analyzed and shown to be a promising candidate for third-generation interferometers (LIGO-III or EURO). This design requires adding a kilometer-scale cavity into the interferometer. In Chapter 7, Sagnac interferometers are analyzed and shown to exhibit a similar broadband QND performance without the need of additional cavity --- as expected since these interferometers are sensitive only to time-dependent mirror displacement, and are automatic speed meters.\r\n\r\nIn Chapter 8 (in collaboration with Alessandra Buonanno and Michele Vallisneri), the Post-Newtonian (PN) breakdown at late-stage inspirals of non-spinning binary black holes is studied. We propose the use of Detection Template Families (DTFs) --- extensions of ordinary PN templates that can mimic all different PN waveforms and hence are plausible to catch the real waveform, yet do not provide straightforward parameter estimation. In Chapter 9 (in collaboration with Alessandra Buonanno and Michele Vallisneri), binaries carrying spins are studied using an adiabatic PN model. Based on features of the precession dynamics, we construct a DTF, using a modified Apostolatos' ansatz, that can mimic the modulated waveforms reasonably well, while keeping a small number of parameters to be searched over one by one, with the rest searched over automatically. We also propose a (computationally) plausible way of searching over the entire physical parameter space of neutron-star--black-hole binaries.", "date": "2003", "date_type": "degree", "id_number": "CaltechETD:etd-05302003-044325", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05302003-044325", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department", "LIGO" ] }, "suggestions": "Caltech faculty", "deposited_by": "Imported from ETD-db", "deposited_on": "2003-05-30", "doi": "10.7907/VQH0-QA78", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@its.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "hmabuchi@its.caltech.edu", "id": "Mabuchi-H", "name": { "family": "Mabuchi", "given": "Hideo" }, "role": "member" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-05-30", "thesis_defense_date": "2003-05-08", "thesis_approved_date": "2003-05-30", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2003", "author_list": "Chen, Yanbei" }, { "id": "/id/eprint/1940", "eprint_id": 1940, "rev_number": 11, "documents": [ { "id": "/id/document/3382", "doc_id": 3382, "rev_number": 3, "files": [ { "id": "/id/file/20040", "fileid": 20040, "datasetid": "document", "objectid": 3382, "filename": "mhartl_thesis_new.pdf", "mime_type": "application/pdf", "filesize": 6196925, "mtime": "2012-12-26 02:44:35", "url": "/1940/1/mhartl_thesis_new.pdf" } ], "eprint_id": 1940, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "mhartl_thesis_new.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"lastmod": "2021-02-11 20:32:44", "status_changed": "2009-09-25 02:21:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mhartl@post.harvard.edu", "id": "Hartl-Michael-David", "name": { "family": "Hartl", "given": "Michael David" }, "show_email": "NO" } ] }, "title": "Dynamics of Spinning Compact Binaries in General Relativity", "ispublished": "unpub", "full_text_status": "public", "keywords": "chaos theory; compact binaries; gravitational waves; Lyapunov exponents", "abstract": "This thesis investigates the dynamics of binary systems composed of spinning compact objects (such as white dwarfs, neutron stars, and black holes) in the context of general relativity. In particular, we use the method of Lyapunov exponents to determine whether such systems are chaotic. Compact binaries are promising sources of gravitational radiation for both ground- and space-based gravitational-wave detectors, and radiation from chaotic orbits would be difficult to detect and analyze. For chaotic orbits, the number of waveform templates needed to match a given gravitational-wave signal would grow exponentially with increasing detection sensitivity, rendering the preferred matched filter detection method computationally impractical. It is therefore urgent to understand whether the binary dynamics can be chaotic, and, if so, how prevalent this chaos is.
\r\n\r\nWe first consider the dynamics of a spinning compact object orbiting a much more massive rotating black hole, as modeled by the Papapetrou equations in Kerr spacetime. We find that many initial conditions lead to positive Lyapunov exponents, indicating chaotic dynamics. The Lyapunov exponents come in positive/negative pairs, a characteristic of Hamiltonian dynamical systems. Despite the formal existence of chaotic solutions, we find that chaos occurs only for physically unrealistic values of the small body's spin. As a result, chaos will not affect theoretical templates in the extreme mass-ratio limit for which the Papapetrou equations are valid. Chaos will therefore not affect the ability of space-based gravitational-wave detectors (such as LISA, the Laser Interferometer Space Antenna) to perform precision tests of general relativity using extreme mass-ratio inspirals.
\r\n\r\nWe next consider the dynamics of spinning black-hole binaries, as modeled by the post-Newtonian (PN) equations, which are valid for orbital velocities much smaller than the speed of light. We study thoroughly the special case of quasi-circular orbits with comparable mass ratios, which are particularly relevant from the perspective of gravitational wave generation for LIGO (the Laser Interferometer Gravitational-wave Observatory) and other ground-based interferometers. In this case, unlike the extreme mass-ratio case, we find chaotic solutions for physically realistic values of the spin. On the other hand, our survey shows that chaos occurs in a negligible fraction of possible configurations, and only for such small radii that the PN approximation is likely to be invalid. As a result, at least in the case of comparable mass black-hole binaries, theoretical templates will not be significantly affected by chaos.
\r\n\r\nIn a final, self-contained chapter, we discuss various methods for the calculation of Lyapunov exponents in systems of ordinary differential equations. We introduce several new techniques applicable to constrained dynamical systems, developed in the course of studying the dynamics of spinning compact binaries.
\r\n\r\nConsidering the Papapetrou and post-Newtonian systems together, our most important general conclusion is that we find no chaos in any relativistic binary system for orbits that clearly satisfy the approximations required for the equations of motion to be physically valid.
", "date": "2003", "date_type": "degree", "id_number": "CaltechETD:etd-05222003-161626", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05222003-161626", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-05-23", "doi": "10.7907/KZ5M-MR27", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "chair" }, { "email": "marsden@cds.caltech.edu", "id": "Marsden-J-E", "name": { "family": "Marsden", "given": "Jerrold E." }, "role": "member" }, { "email": "kip@tapir.caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" }, { "email": "rdb@tapir.caltech.edu", "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-05-22", "thesis_defense_date": "2003-05-22", "thesis_approved_date": "2003-05-23", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2003", "author_list": "Hartl, Michael David" }, { "id": "/id/eprint/120", "eprint_id": 120, "rev_number": 12, "documents": [ { "id": "/id/document/191", "doc_id": 191, "rev_number": 3, "files": [ { "id": "/id/file/1183", "fileid": 1183, "datasetid": "document", "objectid": 191, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 3981058, "mtime": "2012-12-26 02:27:27", "url": "/120/1/thesis.pdf" } ], "eprint_id": 120, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17016" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17016" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17016" } ] } }, { "id": "/id/document/17016", "doc_id": 17016, "rev_number": 2, "files": [ { "id": "/id/file/1181", "fileid": 1181, "datasetid": "document", "objectid": 17016, "filename": "preview.png", "mime_type": "image/png", "hash": "548eff4d159f22527d4232a91de001d3", "hash_type": "MD5", "filesize": 15520, "mtime": "2012-12-26 02:27:27", "url": "/120/2/preview.png" } ], "eprint_id": 120, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/191" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/191" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/191" } ] } }, { "id": "/id/document/119699", "doc_id": 119699, "rev_number": 1, "files": [ { "id": "/id/file/365065", "fileid": 365065, "datasetid": "document", "objectid": 119699, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "607530081f22186007b7f2f4581068a1", "hash_type": "MD5", "filesize": 28981, "mtime": "2021-06-23 20:15:06", "url": "/120/3/indexcodes.txt" } ], "eprint_id": 120, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/191" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/191" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/191" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/01/20", "datestamp": "2002-01-17", "lastmod": "2021-11-06 00:10:58", "status_changed": "2009-09-25 01:29:09", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "john.ward@jpl.nasa.gov", "id": "Ward-John-Strawn", "name": { "family": "Ward", "given": "John Strawn" }, "show_email": "NO" } ] }, "title": "Observations of Carbon Monoxide in the Starburst Galaxy M82 with a 690 GHz Wide Spectral Bandwidth Receiver", "ispublished": "unpub", "full_text_status": "public", "keywords": "intersteller medium; submillimeter", "abstract": "A 690 GHz wide spectral bandwidth heterodyne receiver was developed to observe the J=6-5 rotational emission line of carbon monoxide (CO) in extragalactic sources. This receiver is based on a niobium superconductor-insulator-superconductor (SIS) mixer with a twin-slot antenna in a superconducting NbTiN ground plane. A 4-8 GHz low-noise amplifier was developed to amplify the intermediate frequency (IF) signal from the mixer with a spectral bandwidth of 1,700 km/s, enough to comfortably observe the entire emission line of the broadest extragalactic submillimeter sources with a single receiver tuning. This amplifier is a quasi-monolithic microwave integrated circuit (QMMIC); three 160 micron gate InP high-electron-mobility transistors (HEMTs) were bump-bonded to a thin-film GaAs substrate containing passive tuning and DC bias circuitry. The measured amplifier gain is 32 dB and the noise is approximately 8 Kelvin from 4 to 8 GHz at a physical temperature of 4 Kelvin. The complete receiver achieves a measured uncorrected double-sideband noise temperature of 180 Kelvin.
\r\n\r\nPrior to this development effort, a versatile microwave simulation package was written to calculate and optimize the signal and noise performance of high-frequency circuits, especially those containing superconductors and superconducting tunnel junctions. Using this package, called SuperMix, C++ programs can be written to simulate and optimize circuits of arbitrary size, complexity, and topology. SuperMix was used to simulate the complete 690 GHz SIS receiver.
\r\n\r\nThe receiver was used at the Caltech Submillimeter Observatory (CSO) to map the 12CO J=6-5 emission line in the central kiloparsec of the nearby starburst galaxy M82 at a resolution of 14 arc seconds. Hot spots were found on either side of the dynamical center. A novel deconvolution technique was used to compute a 12CO J=6-5 / 12CO J=2-1 line ratio map based on high-resolution J=2-1 interferometer data. The 12CO J=6-5 map, along with observations of 12CO J=4-3, 12CO J=3-2, 13CO J=3-2, an upper limit for 13CO J=6-5, and five other measured CO lines from the literature, were analyzed in the context of a two-component large velocity gradient (LVG) excitation model. Likelihood curves were calculated for each of the model parameters as well as a variety of related physical quantities for the two hot spots based on the measured line intensities and their associated uncertainties. This approach reveals in an unbiased way how well various quantities can be constrained by the CO observations. The results of this analysis suggest that the warm gas is less dense than the cool gas, and that over half of the total molecular gas mass in these nuclear regions is warmer than 50 K.
", "date": "2002", "date_type": "degree", "id_number": "CaltechETD:etd-01112002-085240", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01112002-085240", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-01-17", "doi": "10.7907/5S4X-NV83", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "jonas@submm.caltech.edu", "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "chair" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" }, { "email": "nzs@radio.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "phillips@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-01-11", "thesis_defense_date": "2001-12-18", "thesis_approved_date": "2002-01-17", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Ward, John Strawn" }, { "id": "/id/eprint/6967", "eprint_id": 6967, "rev_number": 25, "documents": [ { "id": "/id/document/14655", "doc_id": 14655, "rev_number": 5, "files": [ { "id": "/id/file/94702", "fileid": 94702, "datasetid": "document", "objectid": 14655, "filename": "Dyudina_ua_2002.pdf", "mime_type": "application/pdf", "filesize": 30330221, "mtime": "2012-12-26 04:42:15", "url": "/6967/1/Dyudina_ua_2002.pdf" } ], "eprint_id": 6967, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Dyudina_ua_2002.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/27964" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/27964" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/27964" } ] } }, { "id": "/id/document/14656", "doc_id": 14656, "rev_number": 3, "files": [ { "id": "/id/file/207870", "fileid": 207870, "datasetid": "document", "objectid": 14656, "filename": "Dyudina_ua_2002.zip", "mime_type": "application/zip", "filesize": 79582182, "mtime": "2016-08-22 21:23:51", "url": "/6967/2/Dyudina_ua_2002.zip" } ], "eprint_id": 6967, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Dyudina_ua_2002.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/27964", "doc_id": 27964, "rev_number": 3, "files": [ { "id": "/id/file/94700", "fileid": 94700, "datasetid": "document", "objectid": 27964, "filename": "preview.png", "mime_type": "image/png", "hash": "838d50a1d292adf59de0a3b17073201c", "hash_type": "MD5", "filesize": 22456, "mtime": "2012-12-26 04:42:14", "url": "/6967/3/preview.png" } ], "eprint_id": 6967, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14655" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/14655" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14655" } ] } }, { "id": "/id/document/127348", "doc_id": 127348, "rev_number": 1, "files": [ { "id": "/id/file/372784", "fileid": 372784, "datasetid": "document", "objectid": 127348, "filename": "indexcodes.txt", "mime_type": "text/x-c", "hash": "95fd1ae4a42d7e58379ec4e1fa8170a9", "hash_type": "MD5", "filesize": 22707, "mtime": "2021-06-24 01:40:57", "url": "/6967/4/indexcodes.txt" } ], "eprint_id": 6967, "pos": 4, "placement": 4, "mime_type": "text/x-c", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14655" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14655" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14655" } ] } } ], "eprint_status": "archive", "userid": 104, "dir": "disk0/00/00/69/67", "datestamp": "2012-04-24 22:43:39", "lastmod": "2021-11-12 23:01:46", "status_changed": "2012-04-24 22:43:39", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dyudina-Ulyana-Anatolyevna", "name": { "family": "Dyudina", "given": "Ulyana Anatolyevna" }, "show_email": "NO" } ] }, "title": "Light Scattering in the Clouds on Jupiter", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Computer Science", "abstract": "We construct maps of jovian cloud properties from images taken simultaneously by the Galileo solid state imaging system (SSI) and the near-infrared mapping spectrometer (NIMS) at 26 visible and near infrared wavelengths, ranging from 0.41 to 5.2 \u00b5m. Three regions - the Great Red Spot (GRS), a 5-micron Hot Spot, and one of the White Ovals - are studied. We perform a principal component analysis (PCA) on the multispectral images. PCA shows that the pixel-to-pixel variations at the different wavelengths are highly correlated, and that 91% of the variance in the data can be summarized using only three maps. The three maps are combined into one color map, which indicates different 26-wavelength spectra as different colors. Using the representative spectra for each color we compare different areas on the map qualitatively. We find that in the GRS there is a red chromophore which is associated with clouds that block 5-\u00b5m emission. At the hot spot and white oval regions there is no chromophore associated with clouds. Most of the bright, optically thick clouds blocking thermal emission are also extended vertically to the upper troposphere. Some of the bright, optically thick clouds blocking thermal emission are deep and do not extend vertically to the upper troposphere. A small convective stormlike cloud to the northwest of the GRS is unusually reflective at long wavelengths (4\u00b5m) and might indicate large particles.
\r\n\r\nWe study lightning on Jupiter and the clouds illuminated by the lightning. The Galileo SSI lightning images have a resolution of 25 km/pixel and are able to resolve the diffuse spots of light scattered in the clouds, which have full widths at half maximum in the range 90-160 km. We compare the lightning images with the images produced by our 3D Monte Carlo light scattering model. The model reproduces non isotropic non-conservative scattering of the photons in the non-homogeneous opacity distribution. We derive that some of the observed scattering patterns are produced in a 3D cloud rather than in a plane-parallel cloud layer, suggesting deep convection. For the six flashes studied, the clouds above the lightning are optically thick (\u0393 > 5). Lightning is as deep as the bottom of the water cloud. Jovian flashes are more regular\r\nand circular than the largest terrestrial flashes observed from space.
", "date": "2002", "date_type": "degree", "id_number": "CaltechTHESIS:04242012-142706141", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04242012-142706141", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Dan Anguka", "deposited_on": "2012-04-24 22:43:39", "doi": "10.7907/N7JD-N925", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "co-chair" }, { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "member" }, { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2001-12-27", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "compsci" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Dyudina, Ulyana Anatolyevna" }, { "id": "/id/eprint/6771", "eprint_id": 6771, "rev_number": 26, "documents": [ { "id": "/id/document/14080", "doc_id": 14080, "rev_number": 6, "files": [ { "id": "/id/file/90685", "fileid": 90685, "datasetid": "document", "objectid": 14080, "filename": "Alvi_k_2002.pdf", "mime_type": "application/pdf", "filesize": 21554023, "mtime": "2012-12-26 04:39:47", "url": "/6771/1/Alvi_k_2002.pdf" } ], "eprint_id": 6771, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Alvi_k_2002.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/27764" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/27764" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/27764" } ] } }, { "id": "/id/document/14081", "doc_id": 14081, "rev_number": 4, "files": [ { "id": "/id/file/207685", "fileid": 207685, "datasetid": "document", "objectid": 14081, "filename": "Alvi_k_2002.zip", "mime_type": "application/zip", "filesize": 56008884, "mtime": "2016-08-22 21:23:29", "url": "/6771/2/Alvi_k_2002.zip" } ], "eprint_id": 6771, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Alvi_k_2002.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/27764", "doc_id": 27764, "rev_number": 3, "files": [ { "id": "/id/file/90683", "fileid": 90683, "datasetid": "document", "objectid": 27764, "filename": "preview.png", "mime_type": "image/png", "hash": "c539800dda3c0cd58874a7778fb6b90e", "hash_type": "MD5", "filesize": 37152, "mtime": "2012-12-26 04:39:47", "url": "/6771/3/preview.png" } ], "eprint_id": 6771, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14080" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/14080" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14080" } ] } }, { "id": "/id/document/127149", "doc_id": 127149, "rev_number": 1, "files": [ { "id": "/id/file/372583", "fileid": 372583, "datasetid": "document", "objectid": 127149, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "94b4792c7f964d4f237824e1fe221c0c", "hash_type": "MD5", "filesize": 17884, "mtime": "2021-06-24 01:29:22", "url": "/6771/4/indexcodes.txt" } ], "eprint_id": 6771, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14080" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14080" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14080" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/00/67/71", "datestamp": "2012-01-23 15:36:12", "lastmod": "2021-11-05 20:18:02", "status_changed": "2012-01-23 15:36:12", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Alvi-Kashif-Siddiq", "name": { "family": "Alvi", "given": "Kashif Siddiq" }, "show_email": "NO" } ] }, "title": "Topics in General Relativity: Binary Black Holes and Hyperbolic Formulations of Einstein's Equations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis consists of three projects in general relativity on topics related to binary black holes\r\nand the gravitational waves they emit. The first project involves calculating a four-metric that is an approximate solution to Einstein's equations representing two widely separated nonrotating black holes in a circular orbit. This metric is constructed by matching a post-Newtonian metric to\r\ntwo tidally distorted Schwarzschild metrics using the framework of matched asymptotic expansions. The four-metric presented here provides physically realistic initial data that are tied to the binary's inspiral phase and can be evolved numerically to determine the gravitational wave output during the late stages of inspiral as well as the merger.
\r\n\r\nThe second project is on the tidal interaction of binary black holes during the inspiral phase. The holes' tidal distortion results in the flow of energy and angular momentum into or out of the holes in a process analogous to Newtonian tidal friction in a planet-moon system. The changes in the black holes' masses, spins, and horizon areas during inspiral are calculated for a circular binary with holes of possibly comparable masses. The absorption or emission of energy and angular momentum by the holes is shown to have a negligible influence on the binary 's orbital evolution when the holes have comparable masses. The tidal-interaction analysis presented in this thesis is applicable to a black hole in a binary with any companion body (e.g., a neutron star) that is well separated from\r\nthe hole.
\r\n\r\nThe final project is on first-order hyperbolic formulations of Einstein's equations, which are promising as a basis for numerical simulation of binary black holes. This thesis presents two first-order symmetrizable hyperbolic systems that include the lapse and shift as dynamical fields and have only physical characteristic speeds. The first system may be useful in numerical work; the second system allows one to show that any solution to Einstein's equations in any gauge can be obtained\r\nusing hyperbolic evolution of the entire metric, including the gauge fields.
", "date": "2002", "date_type": "degree", "id_number": "CaltechTHESIS:01202012-112836824", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01202012-112836824", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2012-01-23 15:36:12", "doi": "10.7907/5S0S-MF65", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" }, { "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "member" }, { "id": "Mabuchi-H", "name": { "family": "Mabuchi", "given": "Hideo" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2002-05-21", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Alvi, Kashif Siddiq" }, { "id": "/id/eprint/2226", "eprint_id": 2226, "rev_number": 22, "documents": [ { "id": "/id/document/4117", "doc_id": 4117, "rev_number": 3, "files": [ { "id": "/id/file/23920", "fileid": 23920, "datasetid": "document", "objectid": 4117, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 2118011, "mtime": "2012-12-26 02:48:34", "url": "/2226/1/thesis.pdf" } ], "eprint_id": 2226, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20724" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20724" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20724" } ] } }, { "id": "/id/document/4118", "doc_id": 4118, "rev_number": 3, "files": [ { "id": "/id/file/23924", "fileid": 23924, "datasetid": "document", "objectid": 4118, "filename": "thesis.ps", "mime_type": "application/postscript", "filesize": 4568293, "mtime": "2012-12-26 02:48:34", "url": "/2226/2/thesis.ps" } ], "eprint_id": 2226, "pos": 2, "mime_type": "application/postscript", "format": "application/postscript", "format_desc": "thesis.ps", "language": "en", "security": "internal", "license": "other", "main": "thesis.ps", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20725" }, { "type": 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"http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4117" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4117" } ] } }, { "id": "/id/document/20725", "doc_id": 20725, "rev_number": 2, "files": [ { "id": "/id/file/23922", "fileid": 23922, "datasetid": "document", "objectid": 20725, "filename": "preview.png", "mime_type": "image/png", "hash": "e8e697362206c29844b11ed8e79286bb", "hash_type": "MD5", "filesize": 14814, "mtime": "2012-12-26 02:48:34", "url": "/2226/4/preview.png" } ], "eprint_id": 2226, "pos": 4, "placement": 4, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4118" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4118" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4118" } ] } }, { "id": "/id/document/122386", "doc_id": 122386, "rev_number": 1, "files": [ { "id": "/id/file/367784", "fileid": 367784, "datasetid": "document", "objectid": 122386, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "3ac146158f3b81e1b527ccfc945d7636", "hash_type": "MD5", "filesize": 34188, "mtime": "2021-06-23 21:56:07", "url": "/2226/5/indexcodes.txt" } ], "eprint_id": 2226, "pos": 5, "placement": 5, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4117" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4117" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4117" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/22/26", "datestamp": "2002-06-11", "lastmod": "2021-11-06 00:02:40", "status_changed": "2009-09-25 02:31:14", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "vallis@vallis.org", "id": "Vallisneri-Michele", "name": { "family": "Vallisneri", "given": "Michele" }, "orcid": "0000-0002-4162-0033", "show_email": "NO" } ] }, "title": "Modeling and Detecting Gravitational Waves from Compact Stellar Objects", "ispublished": "unpub", "full_text_status": "public", "keywords": "Black hole binaries; gravitational waves; neutron stars; stellar instabilities", "abstract": "In the next few years, the first detections of gravity-wave signals using Earth-based interferometric detectors will begin to provide precious new information about the structure, dynamics, and evolution of compact bodies, such as neutron stars and black holes, both isolated and in binary systems. The intrinsic weakness of gravity-wave signals requires a proactive approach to modeling the prospective sources and anticipating the shape of the signals that we seek to detect. Full-blown 3-D numerical simulations of the sources are playing and will play an important role in planning the gravity-wave data-analysis effort. This thesis explores the interplay between numerical source modeling and data analysis, looking closely at three case studies.
\r\n\r\n1. I evaluate the prospects for extracting equation-of-state information from neutron-star tidal disruption in neutron-star\u2013black-hole binaries with LIGO-II, and I estimate that the observation of disrupting systems at distances that yield about one event per year should allow the determination of the neutron-star radius to about 15%, which compares favorably to the currently available electromagnetic determinations.
\r\n\r\n2. In collaboration with Lee Lindblom and Joel Tohline, I perform numerical simulations of the nonlinear dynamics of the r-mode instability in young, rapidly spinning neutron stars, and I find evidence that nonlinear couplings to other modes will not pose a significant limitation to the growth of the r-mode amplitude.
\r\n\r\n3. In collaboration with Alessandra Buonanno and Yanbei Chen, I study the problem of detecting gravity waves from solar-mass black-hole\u2013black-hole binaries with LIGO-I, and I construct two families of detection templates that address the inadequacy of standard post-Newtonian theory to predict reliable waveforms for these systems.
\r\n", "date": "2002", "date_type": "degree", "id_number": "CaltechETD:etd-05292002-113750", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05292002-113750", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1103/physrevlett.84.3519" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1103/physrevd.65.084039" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-9731698" }, { "agency": "NSF", "grant_number": "AST-9987344" }, { "agency": "NSF", "grant_number": "PHY-9796079" }, { "agency": "NSF", "grant_number": "PHY-9900776" }, { "agency": "NSF", "grant_number": "PHY-9907949" }, { "agency": "NSF", "grant_number": "PHY-0099568" }, { "agency": "NASA", "grant_number": "NAG5-4093" }, { "agency": "NASA", "grant_number": "NAG5-8497" }, { "agency": "NASA", "grant_number": "NAG5-10707" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department", "LIGO" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-06-11", "doi": "10.7907/JN6M-BW40", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "orcid": "0000-0002-8744-3298", "role": "member" }, { "id": "Lindblom-L-A", "name": { "family": "Lindblom", "given": "Lee A." }, "role": "member" }, { "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-05-29", "thesis_defense_date": "2002-05-07", "thesis_approved_date": "2002-06-11", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Vallisneri, Michele" }, { "id": "/id/eprint/4106", "eprint_id": 4106, "rev_number": 19, "documents": [ { "id": "/id/document/6787", "doc_id": 6787, "rev_number": 3, "files": [ { "id": "/id/file/41151", "fileid": 41151, "datasetid": "document", "objectid": 6787, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 40626495, "mtime": "2012-12-26 03:05:28", "url": "/4106/1/thesis.pdf" } ], "eprint_id": 4106, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23319" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23319" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23319" } ] } }, { "id": "/id/document/23319", "doc_id": 23319, "rev_number": 2, "files": [ { "id": "/id/file/41149", "fileid": 41149, "datasetid": "document", "objectid": 23319, "filename": "preview.png", "mime_type": "image/png", "hash": "679c59935ca5e8fe12b2bb3f57d9e72a", "hash_type": "MD5", "filesize": 13211, "mtime": "2012-12-26 03:05:28", "url": "/4106/2/preview.png" } ], "eprint_id": 4106, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6787" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6787" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6787" } ] } }, { "id": "/id/document/123995", "doc_id": 123995, "rev_number": 1, "files": [ { "id": "/id/file/369425", "fileid": 369425, "datasetid": "document", "objectid": 123995, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "5360eb58832cc50897d264e1d960ee25", "hash_type": "MD5", "filesize": 66877, "mtime": "2021-06-23 23:12:58", "url": "/4106/3/indexcodes.txt" } ], "eprint_id": 4106, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6787" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6787" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/6787" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/41/06", "datestamp": "2001-10-22", "lastmod": "2021-11-05 20:04:17", "status_changed": "2009-09-25 03:11:39", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "adam@astro.ucla.edu", "id": "Burgasser-Adam-Jonathan", "name": { "family": "Burgasser", "given": "Adam Jonathan" }, "orcid": "0000-0002-6523-9536", "show_email": "YES" } ] }, "title": "The Discovery and Characterization of Methane-bearing Brown Dwarfs and the Definition of the T Spectral Class", "ispublished": "unpub", "full_text_status": "public", "keywords": "brown dwarfs; infrared spectroscopy; L dwarfs; low-mass stars; spectral classification; stellar populations; T dwarfs", "abstract": "I present the discovery of 18 T dwarfs, brown dwarfs exhibiting CH4 absorption analogous to Gliese 229B, identified in the Two Micron All Sky Survey. Follow-up spectroscopic observations reveal the presence of strong H2O and CH4 bands in these objects, as well as broadened Na I and K I absorption in the red optical; fine lines of K I, Cs I, and Rb I; and FeH absorption at 9896 \u00ae Three objects are analyzed in detail; the widely-separated companion brown dwarf Gliese 570D, the coolest known brown dwarf with Teff = 810+/-45 K; the active T dwarf 2MASS 1237+6526, whose unique and steady H alpha emission may be the result of Roche-lobe overflow accretion from a closely-separated companion; and 2MASS 0559-1404, the brightest T dwarf currently known, which appears to be overluminous but unresolved in HST images. The variation in spectral features amongst these objects and those identified by the Sloan Digital Sky Survey have been used to derive a near-infrared spectral classification scheme, tied to the observed strengths of H2O and CH4 bands, color ratios, and K-band spectral morphology. The grid of subclasses segregates the currently known population into seven distinct groups, ranging from T1 V to T8 V. I show that the possible presence of CH4 in the L7 V DENIS 0205-1159AB argues for few subtypes between the latest known L dwarfs and the earliest T dwarfs. One peculiar object, 2MASS 0937+2931, has a highly suppressed K-band peak, likely due to increased H2 opacity in a high-gravity or low-metallicity atmosphere. Examination of absolute brightness and effective temperature across the L/T transition indicates rapid evolution of spectral features, possibly linked to heterogenous cloud coverage as condensibles rain out of the photosphere. Finally, I have used the T dwarf search samples to constrain the substellar field mass function. Through rigorous analysis of selection biases and Monte Carlo simulations, I show that my results are consistent with a power-law mass function scaling as 0.5 [less than] alpha [less than] 1.0, consistent with young stellar cluster surveys but significantly less than current estimates in the field.
", "date": "2002", "date_type": "degree", "id_number": "CaltechETD:etd-10162001-185319", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10162001-185319", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2001-10-22", "doi": "10.7907/KECQ-7R18", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Janda-K-C", "name": { "family": "Janda", "given": "Kenneth C." }, "role": "advisor" }, { "id": "Porter-F-C", "name": { "family": "Porter", "given": "Frank C." }, "orcid": "0000-0003-1948-8889", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "chair" }, { "email": "bts@mop.caltech.edu", "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" }, { "email": "davy@ipac.caltech.edu", "id": "Kirkpatrick-J-D", "name": { "family": "Kirkpatrick", "given": "J. Davy" }, "role": "member" }, { "email": "lah@warning.caltech.edu", "id": "Hillenbrand-L-A", "name": { "family": "Hillenbrand", "given": "Lynne A." }, "role": "member" }, { "email": "pmg@gps.caltech.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Janda-K-C", "name": { "family": "Janda", "given": "Kenneth C." }, "role": "member" }, { "id": "Porter-F-C", "name": { "family": "Porter", "given": "Frank C." }, "orcid": "0000-0003-1948-8889", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2001-10-16", "thesis_defense_date": "2001-08-24", "thesis_approved_date": "2001-10-22", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "option_minor": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Burgasser, Adam Jonathan" }, { "id": "/id/eprint/3767", "eprint_id": 3767, "rev_number": 14, "documents": [ { "id": "/id/document/6405", "doc_id": 6405, "rev_number": 3, "files": [ { "id": "/id/file/38412", "fileid": 38412, "datasetid": "document", "objectid": 6405, "filename": "Adelberger_kl_2002.pdf", "mime_type": "application/pdf", "filesize": 73056574, "mtime": "2012-12-26 03:02:51", "url": "/3767/1/Adelberger_kl_2002.pdf" } ], "eprint_id": 3767, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Adelberger_kl_2002.pdf", "language": "en", "security": "public", "license": "other", "main": "Adelberger_kl_2002.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22937" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22937" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22937" } ] } }, { "id": "/id/document/22937", "doc_id": 22937, "rev_number": 3, "files": [ { "id": "/id/file/38410", "fileid": 38410, "datasetid": "document", "objectid": 22937, "filename": "preview.png", "mime_type": "image/png", "hash": "24d1f507f020cd16c7900c750b1434ad", "hash_type": "MD5", "filesize": 12076, "mtime": "2012-12-26 03:02:50", "url": "/3767/2/preview.png" } ], "eprint_id": 3767, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6405" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6405" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6405" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/67", "datestamp": "2008-10-07", "lastmod": "2021-11-05 20:13:57", "status_changed": "2009-09-25 03:05:25", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adelberger-Kurt-Ludvig", "name": { "family": "Adelberger", "given": "Kurt Ludvig" }, "show_email": "NO" } ] }, "title": "Star Formation and Structure Formation between Redshifts 1 < z < 4", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "The universe of galaxies beyond redshift one has finally become relatively easy to observe. While only a handful of galaxies with redshifts z > 1 were known 10 years ago, more than 2000 have spectroscopic redshifts today. These surveys are beginning to provide us with a detailed view of the first half of cosmic history. Their creation and interpretation is the subject of this thesis. Chapter 1 describes efficient techniques that can be used to locate galaxies at 1 \u227e z \u227e 5 among the numerous foreground and background objects in deep optical images. Chapter 2 characterizes the effects of dust obscuration on the resulting large high-redshift samples. The remainder of the thesis attemtps to place star-forming high-redshift galaxies into a larger cosmological context. Chapter 3 investigates the spatial clustering of galaxies at z ~ 3, finds it to be strong, and shows that this suggests a close link between rapidly star-forming galaxies and massive virialized objects in the underlying distribution of dark matter. Chapter 4 analyses the curious spatial association of high-redshift galaxies with inter-galactic hydrogen and metals, and finds some evidence that the numerous supernova explosions in young galaxies may profoundly affect the evolution of the universe's baryons.", "date": "2002", "date_type": "degree", "id_number": "CaltechETD:etd-09252008-090426", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09252008-090426", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-07", "doi": "10.7907/F2SF-4J89", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "orcid": "0000-0002-0603-3087" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" } }, { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-25", "thesis_defense_date": "2001-02-22", "thesis_approved_date": "2008-10-07", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Adelberger, Kurt Ludvig" }, { "id": "/id/eprint/2567", "eprint_id": 2567, "rev_number": 13, "documents": [ { "id": "/id/document/4835", "doc_id": 4835, "rev_number": 3, "files": [ { "id": "/id/file/27972", "fileid": 27972, "datasetid": "document", "objectid": 4835, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 1449979, "mtime": "2012-12-26 02:52:39", "url": "/2567/1/thesis.pdf" } ], "eprint_id": 2567, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21385" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21385" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21385" } ] } }, { "id": "/id/document/21385", "doc_id": 21385, "rev_number": 2, "files": [ { "id": "/id/file/27970", "fileid": 27970, "datasetid": "document", "objectid": 21385, "filename": "preview.png", "mime_type": "image/png", "hash": "8c4f4f4b8222eefa38a9eda3229b1251", "hash_type": "MD5", "filesize": 10209, "mtime": "2012-12-26 02:52:39", "url": "/2567/2/preview.png" } ], "eprint_id": 2567, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4835" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4835" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4835" } ] } }, { "id": "/id/document/123050", "doc_id": 123050, "rev_number": 1, "files": [ { "id": "/id/file/368457", "fileid": 368457, "datasetid": "document", "objectid": 123050, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "eac341485f3e0cdd1cb8aa133640ce73", "hash_type": "MD5", "filesize": 27389, "mtime": "2021-06-23 22:17:23", "url": "/2567/3/indexcodes.txt" } ], "eprint_id": 2567, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4835" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4835" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4835" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/25/67", "datestamp": "2002-10-04", "lastmod": "2021-11-05 23:22:05", "status_changed": "2009-09-25 02:40:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mao-Peter-Hsih-Jen", "name": { "family": "Mao", "given": "Peter Hsih-Jen" }, "show_email": "NO" } ] }, "title": "Hard X-Ray Observations of the Extragalactic Sky: The High Energy Focusing Telescope and the Serendipitous Extragalactic X-ray Source Identification Survey", "ispublished": "unpub", "full_text_status": "public", "keywords": "active galactic nuclei; cosmic x-ray background; massively parallel computing", "abstract": "Extending the energy range of high sensitivity astronomical x-ray observations to the hard x-ray band (10-100 keV) is important for the study of nonthermal emission mechanisms and heavily obscured sources. This thesis, in two parts, describes the development of the High Energy Focusing Telescope (HEFT), a focusing telescope for the hard x-ray band, and the Serendipitous Extragalactic X-ray Source Identification (SEXSI) survey, a degree-scale x-ray/optical survey of sources detected in the Chandra hard band (2-7 keV).
\r\n\r\nHEFT is a balloon-borne x-ray telescope that is expected to have its first flight in the fall of 2003. The telescope will be among the first to focus x-rays at energies greater than 20 keV. HEFT's mirrors use graded multilayers -- thin film coatings (~1 \u00b5m) that enhance high energy reflectance via constructive interference. In the first half of the thesis, I describe the optimization algorithm that I developed for x-ray optics and how I applied this algorithm to the design of the HEFT optics. In addition, I present x-ray measurements that verify the HEFT multilayer coating designs at energies where the telescope will operate.
\r\n\r\nThe SEXSI survey complements Chandra deep-field surveys by covering a much larger area of the sky, but to a shallower x-ray flux limit. For the SEXSI survey, we use public data from the Chandra archive to compile a catalog of extragalactic sources detected in the 2-7 keV band. We identify the optical counterparts to the x-ray sources and obtain their optical spectra (400-1000 nm). Presently SEXSI includes 30 Chandra fields, covering roughly 2 square degrees and yielding over 1200 x-ray sources to a flux limit of 10\u207b\u00b9\u2075-10\u207b\u00b9\u00b3 erg cm\u207b\u00b2 s\u207b\u00b9. In the second part of the thesis, I present results from 10 fields for which we have substantial spectroscopic coverage.
", "date": "2002", "date_type": "degree", "id_number": "CaltechETD:etd-06132002-131531", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06132002-131531", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-10-04", "doi": "10.7907/R5E3-RQ86", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "chair" }, { "email": "acr@deimos.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "email": "rdb@tapir.caltech.edu", "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "tat@its.caltech.edu", "id": "Tombrello-T-A", "name": { "family": "Tombrello", "given": "Thomas A." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-06-13", "thesis_defense_date": "2002-05-24", "thesis_approved_date": "2002-10-04", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Mao, Peter Hsih-Jen" }, { "id": "/id/eprint/38", "eprint_id": 38, "rev_number": 13, "documents": [ { "id": "/id/document/84", "doc_id": 84, "rev_number": 3, "files": [ { "id": "/id/file/465", "fileid": 465, "datasetid": "document", "objectid": 84, "filename": "book_main_old.pdf", "mime_type": "application/pdf", "filesize": 5286035, "mtime": "2012-12-26 02:26:57", "url": "/38/1/book_main_old.pdf" } ], "eprint_id": 38, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "book_main_old.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/16912" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/16912" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/16912" } ] } }, { "id": "/id/document/16912", "doc_id": 16912, "rev_number": 2, "files": [ { "id": "/id/file/463", "fileid": 463, "datasetid": "document", "objectid": 16912, "filename": "preview.png", "mime_type": "image/png", "hash": "b7a0569bd935714c8c5c651f3a1675bc", "hash_type": "MD5", "filesize": 10615, "mtime": "2012-12-26 02:26:57", "url": "/38/2/preview.png" } ], "eprint_id": 38, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/84" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/84" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/84" } ] } }, { "id": "/id/document/119653", "doc_id": 119653, "rev_number": 1, "files": [ { "id": "/id/file/365019", "fileid": 365019, "datasetid": "document", "objectid": 119653, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "30501a4193d93cc128a285f2010ce204", "hash_type": "MD5", "filesize": 50595, "mtime": "2021-06-23 20:12:22", "url": "/38/3/indexcodes.txt" } ], "eprint_id": 38, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/84" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/84" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/84" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/00/38", "datestamp": "2003-01-06", "lastmod": "2021-11-05 20:19:39", "status_changed": "2009-09-25 01:26:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jbloom@cfa.harvard.edu", "id": "Bloom-Joshua-Simon", "name": { "family": "Bloom", "given": "Joshua Simon" }, "orcid": "0000-0002-7777-216X", "show_email": "YES" } ] }, "title": "Toward an Understanding of the Progenitors of Gamma-Ray Bursts", "ispublished": "unpub", "full_text_status": "public", "keywords": "black hole; cosmology; gravitational waves; neutrinos; neutron stars; novae; population III; stars; Type Ic supernova", "abstract": "The various possibilities for the origin (\"progenitors\") of gamma-ray bursts (GRBs) manifest in differing observable properties. Through deep spectroscopic and high-resolution imaging observations of some GRB hosts, I demonstrate that well-localized long-duration GRBs are connected with otherwise normal star-forming galaxies at moderate redshifts of order unity. Using high-mass binary stellar population synthesis models, I quantify the expected spatial extent around galaxies of coalescing neutron stars, one of the leading contenders for GRB progenitors. I then test this scenario by examining the offset distribution of GRBs about their apparent hosts making extensive use of ground-based optical data from Keck and Palomar and space-based imaging from the Hubble Space Telescope. The offset distribution appears to be inconsistent with the coalescing neutron star binary hypothesis (and, similarly, black-hole-neutron star coalescences); instead, the distribution is statistically consistent with a population of progenitors that closely traces the ultra-violet light of galaxies. This is naturally explained by bursts which originate from the collapse of massive stars (\"collapsars\"). This claim is further supported by the unambiguous detections of intermediate-time (approximately three weeks after the bursts) emission \"bumps\" which appear substantially more red than the afterglows themselves. I claim that these bumps could originate from supernovae that occur at approximately the same time as the associated GRB; if true, GRB 980326 and GRB 011121 provide strong observational evidence connecting cosmological GRBs to high-redshift supernovae and implicate massive stars as the progenitors of at least some long-duration GRBs. Regardless of the true physical origin of these bumps, it appears that all viable alternative models of these bumps (such as dust scattering of the afterglow light) require a substantial amount of circumburst matter that is distributed as a wind-stratified medium; this too, implicates massive stars. Also suggested herein are some future observations which could further solidify or refute the supernova claim. In addition to the observational and modeling work, I also constructed the Jacobs Camera (JCAM), a dual-beam optical camera for the Palomar 200-inch Telescope designed to follow-up rapid GRB localizations.
\r\n", "date": "2002", "date_type": "degree", "id_number": "CaltechETD:etd-01062003-061357", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01062003-061357", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1046/j.1365-8711.1999.02437.x" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1086/311682" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1086/312059" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "https://doi.org/10.1086/321398" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "https://doi.org/10.1086/338893" }, { "description": "Article adapted for Chapter 7.", "type": "doi", "url": "https://doi.org/10.1038/46744" }, { "description": "Article adapted for Chapter 8.", "type": "doi", "url": "https://doi.org/10.1086/341551" }, { "description": "Article adapted for Chapter 9.", "type": "doi", "url": "https://doi.org/10.1086/311655" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Fannie and John Hertz Foundation" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-01-06", "doi": "10.7907/GKHP-2K61", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "chair" }, { "email": "george@astro.caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "orcid": "0000-0002-0603-3087", "role": "member" }, { "email": "kamion@tapir.caltech.edu", "id": "Kamionkowski-M-P", "name": { "family": "Kamionkowski", "given": "Marc P." }, "orcid": "0000-0001-7018-2055", "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-01-06", "thesis_defense_date": "2002-04-01", "thesis_approved_date": "2003-01-06", "thesis_awards": "Everhart Distinguished Graduate Student Lecturer Award, 2002", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Bloom, Joshua Simon" }, { "id": "/id/eprint/2430", "eprint_id": 2430, "rev_number": 13, "documents": [ { "id": "/id/document/4617", "doc_id": 4617, "rev_number": 2, "files": [ { "id": "/id/file/26619", "fileid": 26619, "datasetid": "document", "objectid": 4617, "filename": "thesis020605.pdf", "mime_type": "application/pdf", "filesize": 5424798, "mtime": "2012-12-26 02:51:19", "url": "/2430/1/thesis020605.pdf" } ], "eprint_id": 2430, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis020605.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis020605.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21174" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21174" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21174" } ] } }, { "id": "/id/document/21174", "doc_id": 21174, "rev_number": 2, "files": [ { "id": "/id/file/26617", "fileid": 26617, "datasetid": "document", "objectid": 21174, "filename": "preview.png", "mime_type": "image/png", "hash": "cdd05464e1815f0d8dec5757a5fc06a4", "hash_type": "MD5", "filesize": 19443, "mtime": "2012-12-26 02:51:19", "url": "/2430/2/preview.png" } ], "eprint_id": 2430, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4617" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4617" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4617" } ] } }, { "id": "/id/document/122881", "doc_id": 122881, "rev_number": 1, "files": [ { "id": "/id/file/368281", "fileid": 368281, "datasetid": "document", "objectid": 122881, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "0cb69794b06b007ed121695e39d49c86", "hash_type": "MD5", "filesize": 27642, "mtime": "2021-06-23 22:10:53", "url": "/2430/3/indexcodes.txt" } ], "eprint_id": 2430, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4617" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4617" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/4617" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/24/30", "datestamp": "2002-06-06", "lastmod": "2021-11-05 20:41:18", "status_changed": "2009-09-25 02:37:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "=", "id": "Kern-Brian-Daniel", "name": { "family": "Kern", "given": "Brian Daniel" }, "show_email": "NO" } ] }, "title": "Optical Pulse-Phased Observations of Faint Pulsars with a Phase-Binning CCD Camera", "ispublished": "unpub", "full_text_status": "public", "keywords": "instrumentation; magnetars; outer gap; polar cap; polarization; pulsars", "abstract": "We have constructed a phase-binning CCD camera optimized for optical observations of faint pulsars. The phase-binning CCD camera combines the high quantum efficiency of a CCD with a pulse-phased time resolution capable of observing pulsars as fast as 10 ms, with no read noise penalty. The phase-binning CCD can also operate as a two-channel imaging polarimeter, obtaining pulse-phased linear photopolarimetric observations.\r\n\r\nWe have used this phase-binning CCD to make the first measurements of optical pulsations from an anomalous X-ray pulsar. We measured the optical pulse profile of 4U 0142+61, finding a pulsed fraction of 27%, many times larger than the pulsed fraction in X-rays. From this observation, we concluded that 4U 0142+61 must be a magnetar, an ultramagnetized neutron star (B > 10^14 G). The optical pulse is double-peaked, similar to the soft X-ray pulse profile.\r\n\r\nWe also used the phase-binning CCD to obtain the photometric and polarimetric pulse profiles of PSR B0656+14, a middle-aged isolated rotation-powered pulsar. The optical pulse profile we measured significantly disagrees with the low signal-to-noise profile previously published for this pulsar. Our results show that the optical flux is entirely pulsed, with optical peaks at phases 0.2 and 0.8 with respect to the radio peak, and a bridge of emission between the peaks. The significance of the detection of pulsed polarized flux is low, but the position angles match the extrapolation of the radio polarization profile. The optical data, both photometric and polarimetric, are consistent with the polar cap model of pulsar magnetospheric emission. The fit of the optical data with the competing emission model, the outer gap model, has not yet been determined.\r\n\r\nWe have developed a number of statistical tools, both to estimate the errors in our measurements and to identify systematic errors present in the pulse profiles. The statistical tools, when applied to the data presented here, show that the systematic errors are negligible, bolstering the claims of significance of these results.", "date": "2002", "date_type": "degree", "id_number": "CaltechETD:etd-06042002-125011", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06042002-125011", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-06-06", "doi": "10.7907/XP9W-WM62", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "advisor" }, { "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "orcid": "0000-0002-0603-3087", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "pmg@gps.caltech.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "email": "ccs@astro.caltech.edu", "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "orcid": "0000-0002-4834-7260", "role": "member" }, { "email": "cmartin@srl.caltech.edu", "id": "Martin-D-Christopher", "name": { "family": "Martin", "given": "D. Christopher" }, "orcid": "0000-0002-8650-1644", "role": "member" }, { "email": "fiona@srl.caltech.edu", "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "orcid": "0000-0002-0603-3087", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-06-04", "thesis_defense_date": "2002-05-29", "thesis_approved_date": "2002-06-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Kern, Brian Daniel" }, { "id": "/id/eprint/6796", "eprint_id": 6796, "rev_number": 23, "documents": [ { "id": "/id/document/14146", "doc_id": 14146, "rev_number": 5, "files": [ { "id": "/id/file/91093", "fileid": 91093, "datasetid": "document", "objectid": 14146, "filename": "Lithwick_y_2002.pdf", "mime_type": "application/pdf", "filesize": 28809074, "mtime": "2012-12-26 04:40:02", "url": "/6796/1/Lithwick_y_2002.pdf" } ], "eprint_id": 6796, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Lithwick_y_2002.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/27783" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/27783" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/27783" } ] } }, { "id": "/id/document/14147", "doc_id": 14147, "rev_number": 5, "files": [ { "id": "/id/file/207708", "fileid": 207708, "datasetid": "document", "objectid": 14147, "filename": "Lithwick_y_2002.zip", "mime_type": "application/zip", "filesize": 73407811, "mtime": "2016-08-22 21:23:32", "url": "/6796/2/Lithwick_y_2002.zip" } ], "eprint_id": 6796, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Lithwick_y_2002.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/27783", "doc_id": 27783, "rev_number": 3, "files": [ { "id": "/id/file/91091", "fileid": 91091, "datasetid": "document", "objectid": 27783, "filename": "preview.png", "mime_type": "image/png", "hash": "0842e200bf4c6443e895a129bb21cfd3", "hash_type": "MD5", "filesize": 13805, "mtime": "2012-12-26 04:40:02", "url": "/6796/3/preview.png" } ], "eprint_id": 6796, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14146" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/14146" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14146" } ] } }, { "id": "/id/document/127170", "doc_id": 127170, "rev_number": 1, "files": [ { "id": "/id/file/372604", "fileid": 372604, "datasetid": "document", "objectid": 127170, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "3086a20b5801c50667a9aa16c105a768", "hash_type": "MD5", "filesize": 22470, "mtime": "2021-06-24 01:31:04", "url": "/6796/4/indexcodes.txt" } ], "eprint_id": 6796, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/14146" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/14146" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/14146" } ] } } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/67/96", "datestamp": "2012-01-31 16:09:43", "lastmod": "2021-11-05 22:39:43", "status_changed": "2012-01-31 16:09:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "y-lithwick@northwestern.edu", "id": "Lithwick-Yoram", "name": { "family": "Lithwick", "given": "Yoram" }, "orcid": "0000-0003-4450-0528", "show_email": "NO" } ] }, "title": "Topics in MHD Turbulence", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "I consider two topics in MHD turbulence. First, I work out the theory of compressible MHD turbulence, including kinetic effects. I use this theory to understand features of interstellar scintillation that have hitherto been unexplained. Second, I work out the theory of imbalanced weak MHD turbulence.", "date": "2002", "date_type": "degree", "id_number": "CaltechTHESIS:01302012-162107660", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01302012-162107660", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_on": "2012-01-31 16:09:43", "doi": "10.7907/FP3Q-EZ29", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" }, { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "co-chair" }, { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2002-05-03", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2002", "author_list": "Lithwick, Yoram" }, { "id": "/id/eprint/4691", "eprint_id": 4691, "rev_number": 18, "documents": [ { "id": "/id/document/7566", "doc_id": 7566, "rev_number": 2, "files": [ { "id": "/id/file/46273", "fileid": 46273, "datasetid": "document", "objectid": 7566, "filename": "qch_thesis.pdf", "mime_type": "application/pdf", "filesize": 6850519, "mtime": "2012-12-26 03:11:03", "url": "/4691/1/qch_thesis.pdf" } ], "eprint_id": 4691, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "qch_thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "qch_thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/24085" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/24085" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/24085" } ] } }, { "id": "/id/document/24085", "doc_id": 24085, "rev_number": 2, "files": [ { "id": "/id/file/46271", "fileid": 46271, "datasetid": "document", "objectid": 24085, "filename": "preview.png", "mime_type": "image/png", "hash": "daec08c1ddc5c8374a0b422d88fd38ce", "hash_type": "MD5", "filesize": 15441, "mtime": "2012-12-26 03:11:03", "url": "/4691/2/preview.png" } ], "eprint_id": 4691, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7566" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7566" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7566" } ] } }, { "id": "/id/document/124492", "doc_id": 124492, "rev_number": 1, "files": [ { "id": "/id/file/369922", "fileid": 369922, "datasetid": "document", "objectid": 124492, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "1bbd6db82302e209275362fb42c58f81", "hash_type": "MD5", "filesize": 18103, "mtime": "2021-06-23 23:37:31", "url": "/4691/3/indexcodes.txt" } ], "eprint_id": 4691, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7566" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7566" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/7566" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/46/91", "datestamp": "2001-12-10", "lastmod": "2023-11-08 00:16:43", "status_changed": "2009-09-25 03:24:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "cqi@cfa.harvard.edu", "id": "Qi-Chunhua", "name": { "family": "Qi", "given": "Chunhua" }, "show_email": "YES" } ] }, "title": "Aperture Synthesis Studies of the Chemical Composition of Protoplanetary Disks and Comets", "ispublished": "unpub", "full_text_status": "public", "keywords": "comets: individual(Hale-Bopp); ISM: molecules; radio continuum; radio emission lines; stars: circumstellar matter; stars: formation; techniques: interferometric", "abstract": "Improvements in observational methods have now made it possible to directly observe planet-forming environments around young stars and to better characterize the most primitive relics of planetary growth in our own solar system. This thesis describes one such method, aperture synthesis imaging using the Owens Valley Radio Observatory (OVRO) Millimeter Array, and its application to the chemical composition of circumstellar accretion disks and comets.
\r\n\r\nThe observations presented in this thesis concentrate on [lambda]~3 mm transitions of HCN/HCO+ and {13}CO/CN in LkCa 15, GM Aur, MWC 480, and HD 163296. These disks were chosen based on their large spatial extent, Keplerian kinematic patterns, and strong CO emission.
\r\n \r\nEven at a resolution of 2\" (or a linear scale of ~300 AU at the distance of Taurus and Ophiuchus), the OVRO observations show that the chemistry in circumstellar disks is sensitive to both the central stellar luminosity and the degree of dust settling toward the disk midplane. Abundance ratios such as CN/HCN and HCO+/CO serve as unique probes of pivotal processes such as photoevaporation or cosmic ray induced ionization. The observed lower limit to the fractional ionization of 10{-10} is sufficient to support magnetorotational instabilities that are likely to dominate the transport mechanisms in the outer reaches of protoplanetary disks. CN/HCN gradients in the T Tauri and Herbig Ae star disks appear to be correlated with the local UV radiation field and with the degree of dust settling as judged by recent fits to their spectral energy distributions, illustrating the important role of photochemistry at large disk radii.
\r\n\r\nThe disk emission toward LkCa 15 is particularly intense, with many molecules being detected, including HCN/HCO+ and their {13}C-isotopomers, DCN, CN, HC_3N, CH_3OH, CS, {13}CO, and C{18}O. The overall abundance patterns are consistent with recent models of photon-dominated chemistry in the near surface regions of flaring circumstellar disks that also provide a natural explanation for the mid- and far-infrared properties of the disk spectral energy distribution.
\r\n\r\nDirect ties between accretion disks and the formation of planetary systems can be tested by examining primitive solar system bodies such as comets. Comet Hale-Bopp was observed at OVRO from 1997 March 29 to April 2 in a variety of spectroscopic settings between 3.4 and 1.2 mm. The resulting aperture synthesis millimeter-wave continuum and molecular line images reveal in great detail the inner coma. The millimeter-wave continuum brightness of Hale-Bopp is dominated by emission from dust grains in the coma. By subtracting a spherically symmetric coma model from the continuum visibilities, the millimeter-wave flux from the nucleus has been isolated, and leads to an estimated radius of 19-22.5 km.
\r\n\r\nThe large size of comet Hale-Bopp accounts for its extraordinary outgassing rates, which permitted the aperture synthesis observations of over 18 millimeter transitions of HCN, DCN, HDO, HC_3N, HNC, HNCO, CS, H_2S}, SO, OCS, CO, CH_3OH and CH_3OCH_3. The OVRO Millimeter Array was able to image, for the first time, molecular analogs of the dust jets commonly observed at optical and infrared wavelengths. This is particularly significant for investigating the true composition of comets, since jets are known to lift off large, icy grains from which direct sublimation can occur as they are exposed to the Sun. The production rates derived from the aperture synthesis images are similar to those found by other researchers, and reveal a marked similarity between the composition of Hale-Bopp and that derived for dense molecular clouds, in particular the hot cores observed near massive young stars. In addition, quite substantial D/H fractionations, comparable to the OVRO DCN/HCN measurement in LkCa 15, are found in the jets. While this clearly suggests an evolutionary history in which cometary materials remain at very low temperatures throughout their assemblage and for the bulk of their lives, the complex, kinetically controlled chemistry revealed in the OVRO images of the cold, outer regions of disks around young stars means that it is difficult to characterize cometary volatiles as being primarily \"interstellar\" or \"nebular\" in origin.
", "date": "2001", "date_type": "degree", "id_number": "CaltechETD:etd-11302001-000213", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-11302001-000213", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2001-12-10", "doi": "10.7907/VNV1-8B86", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mbrown@gps.caltech.edu", "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "orcid": "0000-0002-8255-0545", "role": "chair" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "member" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2001-11-30", "thesis_defense_date": "2000-08-21", "thesis_approved_date": "2001-12-10", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2001", "author_list": "Qi, Chunhua" }, { "id": "/id/eprint/3670", "eprint_id": 3670, "rev_number": 26, "documents": [ { "id": "/id/document/6272", "doc_id": 6272, "rev_number": 4, "files": [ { "id": "/id/file/37581", "fileid": 37581, "datasetid": "document", "objectid": 6272, "filename": "Kuchner_mj_2001.pdf", "mime_type": "application/pdf", "filesize": 7392327, "mtime": "2012-12-26 03:01:57", "url": "/3670/1/Kuchner_mj_2001.pdf" } ], "eprint_id": 3670, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Kuchner_mj_2001.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22810" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22810" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22810" } ] } }, { "id": "/id/document/22810", "doc_id": 22810, "rev_number": 3, "files": [ { "id": "/id/file/37579", "fileid": 37579, "datasetid": "document", "objectid": 22810, "filename": "preview.png", "mime_type": "image/png", "hash": "1a63ebfd4e8d3031512a1b99b2d0b59c", "hash_type": "MD5", "filesize": 13230, "mtime": "2012-12-26 03:01:57", "url": "/3670/2/preview.png" } ], "eprint_id": 3670, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6272" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6272" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6272" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/36/70", "datestamp": "2008-11-06", "lastmod": "2022-09-12 22:49:11", "status_changed": "2009-09-25 03:03:11", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kuchner-Marc-Jason", "name": { "family": "Kuchner", "given": "Marc Jason" }, "show_email": "NO" } ] }, "title": "Exozodiacal Dust", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "Besides the sun, the most luminous feature of the solar system is a cloud of \"zodiacal\" dust released by asteroids and comets that pervades the region interior to the asteroid belt. Similar clouds of dust around other stars\u2014exozodiacal clouds\u2014may be the best tracers of the habitable zones of extra-solar planetary systems. This thesis discusses three searches for exozodiacal dust:
\r\n\r\nWe also discuss the interaction of dust with planets. We used the COBE DIRBE Sky and Zodi Atlas and the IRAS Sky Survey Atlas to search for dynamical signatures of three different planets in the solar system dust complex:
\r\n\r\nThe science of precision millisecond pulsar timing can yield the most precise astrometric measurements ever made. This potential can only be realized through an extraordinary amount of investment in the experimental apparatus, the effort of many observers, and the close attention to details required to avoid the many pitfalls along the way. This thesis describes the work and results from a precision timing project aimed at monitoring the brightest millisecond pulsar, PSR J0437-4715. This pulsar is a very suitable target for such a study because of its small period (5.75 ms), low DM (2.69 pc cm\u207b\u00b3), and high flux density (~ 90 mJy at 1.4 GHz). The initial work for this thesis involved completion and installation of the Fast Pulsar Timing Machine (FPTM) at Parkes observatory, Australia. With a bandwidth of 128 MHz and time resolution of 4 \u00b5s, this machine made a quantum jump in the time of arrival precision for PSR J0437-4715. The precision improved from ~ 2 \u00b5s to ~ 0.2 \u00b5s. In order to further enhance the signal-to-noise ratio achievable with this pulsar and probe the limits of precision pulsar timing, we have subsequently improved the FPTM significantly by doubling its bandwidth, so that it can record the pulsar radio emission over a 256 MHz bandwidth. This required us to double the IF processing hardware in the FPTM and implement numerous software modifications to control the observing apparatus, interface the FPTM with the observatory control computers, as well as process the data to produce final times of arrival.
\r\n\r\nIntegration of just a few minutes with the 64 m Parkes radio telescope yield times of arrival for PSR J0437-4715 with a precision of 100 nanoseconds. The longer term residuals (3 years) show root-mean-square deviations of 500 nanoseconds. This excessively large scatter in the residuals has been traced to inaccurate polarization calibration, and a systematic quadratic trend of ~ 5 \u00b5s in the times of arrival as a function of baseband frequency. The latter phenomenon has been simulated in software and shown to arise from the large dynamic range in the baseband spectrum. Despite the systematic errors, our measurement of the pulsar's astrometric and binary parameters match the best obtained so far with other millisecond pulsars. This has allowed us to measure the pulsar's parallax, and the secular change in the binary's projected semi-major axis due to the system's proper motion. The latter effect restricts the inclination angle of the binary, i < 43\u00b0. The parallax, along with the period derivative and orbital period derivative, enable us to constrain the distance of the pulsar, 162 < d < 205 pc. A stability analysis of the pulsar's time of arrival residuals demonstrates that it matches the long term stability of the best studied millisecond pulsars, PSRs B1937+21 and B1855+09, at least on the time scale of the data available so far, 3 years. The precision in the pulsar position now matches the amplitude of the modulation of position expected from the pulsar's binary motion. Detection of this effect will require reduction of the calibration and spectral shape errors, as well as further refinements in the timing software used. Along with radio interferometric observations of the pulsar and optical detection of the white-dwarf companion, the pulsar timing position will provide the best contraints for frame tie between the ecliptic and extragalactic reference frames.
", "date": "2001", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-084556", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-084556", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-31", "doi": "10.7907/17DD-8X47", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "chair" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "co-chair" }, { "id": "Anderson-S-B", "name": { "family": "Anderson", "given": "Stuart B." }, "role": "member" }, { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "orcid": "0000-0002-3330-5439", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "2000-09-28", "thesis_approved_date": "2008-10-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2001", "author_list": "Sandhu, Jagmit Singh" }, { "id": "/id/eprint/4431", "eprint_id": 4431, "rev_number": 26, "documents": [ { "id": "/id/document/7224", "doc_id": 7224, "rev_number": 2, "files": [ { "id": "/id/file/44050", "fileid": 44050, "datasetid": "document", "objectid": 7224, "filename": "01title_page.pdf", "mime_type": "application/pdf", "filesize": 35117, "mtime": "2012-12-26 03:08:36", "url": "/4431/1/01title_page.pdf" } ], "eprint_id": 4431, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "01title_page.pdf", "language": "en", "security": "public", "license": "other", "main": "01title_page.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7229" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7229" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/7229" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/44/31", "datestamp": "2001-11-12", "lastmod": "2022-08-24 23:46:36", "status_changed": "2009-09-25 03:18:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "alexey.a.pankine@gaerospace.com", "id": "Pankine-Alexey-Anatolyevich", "name": { "family": "Pankine", "given": "Alexey Anatolyevich" }, "show_email": "YES" } ] }, "title": "Low Order Model of Martian Circulation and Interannual Variability of Global Dust Storms", "ispublished": "unpub", "full_text_status": "public", "keywords": "atmospheric feedback; chaotic systems with external periodic forcing; global circulation; martian dust storms ;\r\nPlanetary Science and Fluid Mechanics and Stochastic Processes", "abstract": "The main theme of this work is the development of a simplified model of the martian circulation suitable for conducting computationally fast long term simulations of the martian climate system. In particular, we are looking for causes of the irregular occurrence of the martian global dust storms (GDSs). The low-order model (LOM) is constructed by Galerkin projection of a 2D (zonally averaged) general circulation model (GCM) onto a truncated set of basis functions. The resulting low-order model consists of twelve coupled nonlinear ordinary differential equations (ODEs). The forcing of the model is described by simplified physics based on Newtonian cooling and Rayleigh friction. The atmosphere and surface are coupled: atmospheric heating depends on the dustiness of the atmosphere, and the surface dust source depends on the strength of the atmospheric winds. Parameters of the model are tuned to fit output of the NASA Ames GCM.
\r\n\r\nThe model performance is examined for different seasons and dust opacities and it is found that the simulated mean meridional circulation and temperature fields compare well with the more sophisticated GCM. The time of occurence and duration of the global dust storms produced by the model compare well with observations by Viking Landers (VLs). The intensity of the meridional circulation as simulated by the LOM during northern summer is stronger than that predicted by the GCM. The situation can be improved if the Rayleigh friction varies seasonally. The LOM uncoupled from the dust source can be further simplified to form the Lorenz system with forcing.
\r\n\r\nThe model is applied to the problem of interannual variability of martian global dust storms. Basic hypotheses of the intrinsic and of the extrinsic irregularity of the martian climate system are tested. The intrinsic irregularity hypothesis implies that the system under consideration is chaotic, so that small variations in initial conditions make the behavior of the system essentially unpredictable. Different paths taken by the system in state space would correspond to years with and without a GDS. The extrinsic irregularity hypothesis, on the other hand, implies that without noise the system behaves periodically, but stochastic forcing of the system causes it to behave irregularly. It is concluded that the observed variability of GDSs is more easily explained by extrinsic irregularity. The stochastic forcing (``noise') could be provided by transient weather systems or some surface process, like size sorting or redistribution of the sand particles in the ``active' (i.e., storm generating) zones on the surface. The results are very sensitive to the value of the saltation threshold, which hints at the possible feedback between saltation threshold and dust storm activity. According to this hypothesis, the saltation threshold has adjusted its value so that dust storms are barely able to occur.
", "date": "2001", "date_type": "degree", "id_number": "CaltechETD:etd-11072001-160517", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-11072001-160517", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2001-11-12", "doi": "10.7907/MGSA-ZT98", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "advisor" }, { "id": "Muhleman-D-O", "name": { "family": "Muhleman", "given": "Duane Owen" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "bcm@gps.caltech.edu", "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "member" }, { "id": "Albee-A-L", "name": { "family": "Albee", "given": "Arden Leroy" }, "role": "member" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2001-11-07", "thesis_defense_date": "2000-12-08", "thesis_approved_date": "2001-11-12", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "engappsci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2001", "author_list": "Pankine, Alexey Anatolyevich" }, { "id": "/id/eprint/8219", "eprint_id": 8219, "rev_number": 35, "documents": [ { "id": "/id/document/47575", "doc_id": 47575, "rev_number": 3, "files": [ { "id": "/id/file/139109", "fileid": 139109, "datasetid": "document", "objectid": 47575, "filename": "Maron_j_2001.pdf", "mime_type": "application/pdf", "hash": "78287ed9fa7b82a2820292363f4bfdb3", "hash_type": "MD5", "filesize": 13543876, "mtime": "2014-05-05 22:26:09", "url": "/8219/1/Maron_j_2001.pdf" } ], "eprint_id": 8219, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Maron_j_2001.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 87, "dir": "disk0/00/00/82/19", "datestamp": "2014-05-06 14:42:48", "lastmod": "2022-09-12 22:50:54", "status_changed": "2014-05-06 14:42:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Maron-Jason-L", "name": { "family": "Maron", "given": "Jason L." }, "show_email": "NO" } ] }, "title": "Magnetohydrodynamic Turbulence", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "We simulate incompressible, MHD turbulence using a pseudo-spectral code. Our\r\nmajor conclusions are as follows.
\r\n\r\n1) MHD turbulence is most conveniently described in terms of counter propagating\r\nshear Alfv\u00e9n and slow waves. Shear Alfv\u00e9n waves control the cascade dynamics. Slow\r\nwaves play a passive role and adopt the spectrum set by the shear Alfv\u00e9n waves. Cascades\r\ncomposed entirely of shear Alfv\u00e9n waves do not generate a significant measure\r\nof slow waves.
\r\n\r\n2) MHD turbulence is anisotropic with energy cascading more rapidly along k\u22a5 than\r\nalong k\u2225, where k\u22a5 and k\u2225 refer to wavevector components perpendicular and parallel\r\nto the local magnetic field. Anisotropy increases with increasing k\u22a5 such that excited\r\nmodes are confined inside a cone bounded by k\u2225 \u221d k\u03b3\u22a5 where \u03b3 less than 1. The opening\r\nangle of the cone, \u03b8(k\u22a5) \u221d k-(1-\u03b3)\u22a5, defines the scale dependent anisotropy.
\r\n\r\n3) MHD turbulence is generically strong in the sense that the waves which comprise it\r\nsuffer order unity distortions on timescales comparable to their periods. Nevertheless,\r\nturbulent fluctuations are small deep inside the inertial range. Their energy density is less than that of the background field by a factor \u03b82 (k\u22a5)\u226a1.
\r\n\r\n4) MHD cascades are best understood geometrically. Wave packets suffer distortions\r\nas they move along magnetic field lines perturbed by counter propagating waves.\r\nField lines perturbed by unidirectional waves map planes perpendicular to the local\r\nfield into each other. Shear Alfv\u00e9n waves are responsible for the mapping's shear and\r\nslow waves for its dilatation. The amplitude of the former exceeds that of the latter\r\nby 1/\u03b8(k\u22a5) which accounts for dominance of the shear Alfv\u00e9n waves in controlling\r\nthe cascade dynamics.
\r\n\r\n5) Passive scalars mixed by MHD turbulence adopt the same power spectrum as the\r\nvelocity and magnetic field perturbations.
\r\n\r\n6) Decaying MHD turbulence is unstable to an increase of the imbalance between\r\nthe flux of waves propagating in opposite directions along the magnetic field. Forced\r\nMHD turbulence displays order unity fluctuations with respect to the balanced state\r\nif excited at low k by \u03b4(t) correlated forcing. It appears to be statistically stable to\r\nthe unlimited growth of imbalance.
\r\n\r\n7) Gradients of the dynamic variables are focused into sheets aligned with the magnetic\r\nfield whose thickness is comparable to the dissipation scale. Sheets formed by\r\noppositely directed waves are uncorrelated. We suspect that these are vortex sheets\r\nwhich the mean magnetic field prevents from rolling up.
\r\n\r\n8) Items (1)-(5) lend support to the model of strong MHD turbulence put forth by\r\nGoldreich and Sridhar (1995, 1997). Results from our simulations are also consistent\r\nwith the GS prediction \u03b3 = 2/3. The sole not able discrepancy is that the 1D power\r\nlaw spectra, E(k\u22a5) \u221d k-\u221d\u22a5, determined from our simulations exhibit \u221d \u2248 3/2, whereas\r\nthe GS model predicts \u221d = 5/3.
\r\n\r\n\r\n\r\n", "date": "2001", "date_type": "degree", "id_number": "CaltechTHESIS:05052014-152343905", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05052014-152343905", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2014-05-06 14:42:48", "doi": "10.7907/x455-kq95", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Janda-K-C", "name": { "family": "Janda", "given": "Kenneth C." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Pullin-D-I", "name": { "family": "Pullin", "given": "Dale Ian" }, "role": "member" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "co-chair" }, { "id": "Janda-K-C", "name": { "family": "Janda", "given": "Kenneth C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2000-09-19", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2001", "author_list": "Maron, Jason L." }, { "id": "/id/eprint/7474", "eprint_id": 7474, "rev_number": 22, "documents": [ { "id": "/id/document/35403", "doc_id": 35403, "rev_number": 3, "files": [ { "id": "/id/file/111850", "fileid": 111850, "datasetid": "document", "objectid": 35403, "filename": "Moyer 2001.pdf", "mime_type": "application/pdf", "hash": "53b6575c875097668ef11b23a6717588", "hash_type": "MD5", "filesize": 26464849, "mtime": "2013-02-12 19:17:34", "url": "/7474/1/Moyer 2001.pdf" } ], "eprint_id": 7474, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Moyer 2001.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/35404", 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"dir": "disk0/00/00/74/74", "datestamp": "2013-02-12 19:35:32", "lastmod": "2023-11-08 00:36:10", "status_changed": "2013-02-12 19:35:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Moyer-Elisabeth-Jeanne-Bailey", "name": { "family": "Moyer", "given": "Elisabeth Jeanne Bailey" }, "show_email": "NO" } ] }, "title": "Tracers of Rapid Transport in the Lower Stratosphere", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Environmental Engineering", "abstract": "This thesis consists of three parts, each related to the use of tracer measurements to\r\ndiagnose the small-scale structure and mechanisms by which air is transported, both\r\nvertically and horizontally, in the lower stratosphere.
\r\n\r\n1. I demonstrate that the isotopic composition of water vapor can diagnose rapid convective\r\ntransport across the tropopause. I use data from the space shuttle- and balloon-borne\r\nFourier transform solar occultation spectrometers ATMOS (Atmospheric Trace\r\nMOlecule Spectrometer) and Mark-IV to reconstruct the mean deuterium isotopic composition\r\nof water entering the stratosphere. Initial \u03b4D is -670 per mil (33% of deuterated\r\nwater retained). I construct a one-dimensional model simulating isotopic fractionation\r\nduring ascent to the tropopause and demonstrate that for all but the most rapid ascent.\r\nvirtually all deuterated water is stripped from an air parcel in the last few kilometers of\r\nthe uppermost troposphere. The observed stratospheric \u03b4D is then far heavier than modeled\r\ndepletions under most conditions. I conclude that the observations can be matched\r\nonly by substantial evaporation of lofted condensate or by ascent in highly-supersaturated\r\nconditions, and infer that mean stratospheric air must have experienced rapid convection\r\nto at least near-tropopause altitudes. This study serves to demonstrate that the isotopic\r\ncomposition of water vapor is a valuable tracer that can be used to constrain mechanisms\r\nof stratosphere-troposphere transport.
\r\n\r\n\r\n2. I use in-situ tunable diode laser measurements of CO, H_2O, and N_2O taken over\r\nFairbanks, AK to show rapid transport by streamers of air in the lower stratosphere. I\r\nwas part of a team that used ALIAS and JPL-H2O, two tunable diode laser spectrometers built by the Webster group of the Jet Propulsion Laboratory, to obtain data in the upper troposphere and lower stratosphere on 21 ER-2 flights between April and September, 1991, during the POLARIS (Photochemistry of Ozone Loss in the Arctic Region In Summer) mission. I use this dataset to identify episodes of rapid polewards advection in the lowermost stratosphere in which filaments of air move from tropics to 65 N latitude\r\nin weeks. I find that the lowermost stratosphere is a region of intense filamentary activity,\r\nbut that tropical filamentation is absent above the 420 K surface, in contradiction\r\nto the results of previous trajectory simulations. Individual filaments extend from the\r\n\u201coverworld\u201d stratosphere to the local tropopause, showing that the boundary between\r\n\u201coverworld and \u201cmiddleworld\u201d is not a true dynamical barrier. The filamentation is\r\nstrongly seasonal, in agreement with previous trajectory results, but with a longer period\r\nof activity. I conclude that the tropopause transition layer extends to 420 K \u019f, and that\r\ntransport in this layer is coupled to changes in the tropospheric subtropical jet.
\r\n\r\n\r\n3. I describe the design and construction of a new lightweight open-path tunable-diode-\r\nlaser instrument for measurements of water, vapor isotopic composition from aircraft\r\nplatforms. I initiated and led an effort to design and build an instrument capable\r\nof resolving transport issues such as those mentioned in (1). WISP (Water Isotope SPectrometer) is a 3-channel tunable-diode-laser spectrometer, with two mid-infrared and one\r\nnear-infrared laser sources. Light is injected into a 94-pass Herriott cell for a total of 94\r\nmeters of pathlength. The expected threshold sensitivity is a few parts in 10^5 absorption.\r\nDetection of HDO has an expected SNR >10 up to near-tropopause altitudes. All isotopomers\r\nof water vapor, and methane, are detected in a single scan, allowing improved\r\naccuracy as common systematics drop out of the ratio. I led the integration of the instrument on NASA\u2019s WB-57 aircraft as part of the ACCENT mission. The instrument can\r\nprovide a versatile tool for t racer measurements in the tropopause region.
\r\n", "date": "2001", "date_type": "degree", "id_number": "CaltechTHESIS:02122013-103240444", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:02122013-103240444", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_on": "2013-02-12 19:35:32", "doi": "10.7907/snq4-db56", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Webster-C", "name": { "family": "Webster", "given": "Chris" }, "role": "advisor" }, { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "chair" }, { "id": "Hoffmann-M-R", "name": { "family": "Hoffmann", "given": "Michael R." }, "orcid": "0000-0001-6495-1946", "role": "member" }, { "id": "Webster-C", "name": { "family": "Webster", "given": "Chris" }, "role": "member" }, { "id": "Wennberg-P-O", "name": { "family": "Wennberg", "given": "Paul O." }, "orcid": "0000-0002-6126-3854", "role": "member" }, { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2000-10-06", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "envreng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2001", "author_list": "Moyer, Elisabeth Jeanne Bailey" }, { "id": "/id/eprint/7438", "eprint_id": 7438, "rev_number": 26, "documents": [ { "id": "/id/document/35027", "doc_id": 35027, "rev_number": 4, "files": [ { "id": "/id/file/110817", "fileid": 110817, "datasetid": "document", "objectid": 35027, "filename": "Lee-yt-2001.pdf", "mime_type": "application/pdf", "hash": "df66d98b24d6632f3796cfc57110f846", "hash_type": "MD5", "filesize": 27988916, "mtime": "2013-01-25 18:55:21", "url": "/7438/1/Lee-yt-2001.pdf" } ], "eprint_id": 7438, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Lee-yt-2001.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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104, "dir": "disk0/00/00/74/38", "datestamp": "2013-01-25 19:17:59", "lastmod": "2023-11-08 00:36:10", "status_changed": "2013-01-25 19:17:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lee-Yuan-Tai", "name": { "family": "Lee", "given": "Yuan-Tai" }, "show_email": "NO" } ] }, "title": "Atmospheric Chemistry and Transport Modeling in the Outer Solar System", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Astronomy", "abstract": "This thesis consists of 1-D and 2-D photochemical dynamical modeling in the upper atmospheres of outer planets. For 1-D modeling, a unified hydrocarbon photochemical model has been studied in Jupiter, Saturn, Uranus, Neptune, and Titan, by comparing with the Voyager observations, and the recent measurements of methyl radicals by ISO in Saturn and Neptune. The CH_3 observation implies a kinetically sensitive test to the measured and estimated hydrocarbon rate constants at low temperatures. We identify the key reactions that control the concentrations of CH_3 in the model, such as the three-body recombination reaction, CH_3 + CH_3 + M \u2192 C_(2)H_6 + M, and the recycling reaction H + CH_3 + M \u2192CH_4 + M. The results show reasonable agreement with ISO values. In Chapter 4, the detection of PH_3 in the lower stratosphere and upper troposphere of Jupiter has provided a photochemical-dynamical coupling model to derive the eddy diffusion coefficient in the upper troposphere of Jupiter. Using a two-layers photochemical model with updated photodissociation cross-sections and chemical rate constants for NH_3 and PH_3, we find that the upper tropospheric eddy diffusion coefficient <10^5 cm^2 sec^(-1) and the deeper tropospheric value >10^6 cm^2 sec^(-1) are required to match the derived PH_3 vertical profile by the observation. The best-fit functional form derivation of eddy diffusion coefficient in the upper troposphere of Jupiter above 400 mbar is K = 2.0 x 10^4 (n/2.2 x 10^19)^(-0.5)cm^2 sec^(-1). On the other hand, Chapter 5 demonstrates a dynamical-only 2-D model of C_(2)H_6 providing a complete test for the current 2-D transport models in Jovian lower stratosphere and upper troposphere (270 to 0.1 mbar pressure levels). Different combinations of residual advection, horizontal eddy dispersion, and vertical eddy mixing are examined at different latitudes.
\r\n", "date": "2001", "date_type": "degree", "id_number": "CaltechTHESIS:01252013-101859233", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01252013-101859233", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Dan Anguka", "deposited_on": "2013-01-25 19:17:59", "doi": "10.7907/y7ep-g464", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "advisor" }, { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "chair" }, { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "member" }, { "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "orcid": "0000-0001-9432-7159", "role": "member" }, { "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "member" }, { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2000-08-09", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"/id/file/373332", "fileid": 373332, "datasetid": "document", "objectid": 127896, "filename": "indexcodes.txt", "mime_type": "text/x-c", "hash": "f142b725e0c5bdce390921f8d9a1e6ff", "hash_type": "MD5", "filesize": 26009, "mtime": "2021-06-24 02:14:00", "url": "/7433/8/indexcodes.txt" } ], "eprint_id": 7433, "pos": 8, "placement": 8, "mime_type": "text/x-c", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/34974" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/34974" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/34974" } ] } } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/74/33", "datestamp": "2013-01-24 19:41:12", "lastmod": "2022-08-24 23:52:16", "status_changed": "2013-01-24 19:41:12", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Toigo-Anthony-Domenick", "name": { "family": "Toigo", "given": "Anthony Domenick" }, "show_email": "NO" } ] }, "title": "Behavior of Dust in the Martian Atmosphere", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Mechanical Engineering", "abstract": "Two aspects of the dust cycle on Mars are examined: the seasonal variation of dust aerosols\r\nin the atmosphere as observed by spacecraft and dust lifting by high wind stress at the south\r\npole during late spring employing a specially developed mesoscale atmospheric model. Reanalysis\r\nof Viking mission optical depth measurements shows that the visible to infrared\r\nratio of total extinction opacity varies with season, and is due to seasonally varying water\r\nice haze. The Martian atmosphere is clearer of dust, especially during northern spring and\r\nsummer, than previously thought. Water ice hazes can provide roughly 50% of the total\r\nvisible opacity in these seasons, and that they represent only 1-5% of the total water column.\r\nNext, the conversion for use on Mars of a terrestrial mesoscale atmospheric model\r\n(the Mars MM5) is presented and described. Validation of the Mars MM5 is conducted\r\nby comparison with a general circulation model on scales of a few hundred kilometers and\r\nwith Martian surface landers (Viking Lander 1, Viking Lander 2, and Mars Pathfinder)\r\non scales of a few kilometers, and in both cases there is good agreement in the meteorological\r\nvariables of temperature, pressure, and wind. Tides are found to be at least as\r\nimportant as slopes in generating the diurnal cycle of winds at the lander sites, in contrast\r\nto previous one-dimensional studies. Finally, assuming that dust injection is related to the\r\nmovement of sand-sized grains or aggregates, the Mars MM5 predicts wind stresses of sufficient\r\nstrength to initiate movement of sand-sized particles, and hence dust lifting, during\r\nlate southern spring in the south polar region. It is found that the direct cap edge thermal\r\ncontrast provides the primary drive for high surface wind stresses at the cap edge at this season\r\nwhile sublimation flow is not found to be particularly important. Comparison between\r\nsimulations, in which dust is injected when wind stresses are high and those with inactive\r\ndust injection, show no signs of consistent feedback due to dust clouds on the surface wind stress fields during the late spring season examined here.\r\n", "date": "2001", "date_type": "degree", "id_number": "CaltechTHESIS:01242013-112821494", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01242013-112821494", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_on": "2013-01-24 19:41:12", "doi": "10.7907/7v06-j640", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "chair" }, { "id": "Albee-A-L", "name": { "family": "Albee", "given": "Arden Leroy" }, "role": "member" }, { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "orcid": "0000-0002-4263-2562", "role": "member" }, { "id": "Richardson-M-I", "name": { "family": "Richardson", "given": "Mark I." }, "role": "member" }, { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2001-05-18", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "mecheng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2001", "author_list": "Toigo, Anthony Domenick" }, { "id": "/id/eprint/6351", "eprint_id": 6351, "rev_number": 22, "documents": [ { "id": "/id/document/12419", "doc_id": 12419, "rev_number": 6, "files": [ { "id": "/id/file/81510", "fileid": 81510, "datasetid": "document", "objectid": 12419, "filename": "Jenet_fa_2001.pdf", "mime_type": "application/pdf", "filesize": 12083275, "mtime": "2012-12-26 04:34:30", "url": "/6351/1/Jenet_fa_2001.pdf" } ], "eprint_id": 6351, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Jenet_fa_2001.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/27355" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/27355" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/27355" } ] } }, { "id": "/id/document/12420", "doc_id": 12420, "rev_number": 4, "files": [ { "id": "/id/file/206714", "fileid": 206714, "datasetid": "document", "objectid": 12420, "filename": "Jenet_fa_2001.zip", "mime_type": "application/zip", "filesize": 11754318, "mtime": "2016-08-22 21:21:58", "url": "/6351/2/Jenet_fa_2001.zip" } ], "eprint_id": 6351, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Jenet_fa_2001.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/27355", "doc_id": 27355, "rev_number": 3, "files": [ { "id": "/id/file/81508", "fileid": 81508, "datasetid": "document", "objectid": 27355, "filename": "preview.png", "mime_type": "image/png", "hash": "1cc1bf83294dfff5c80e9ee78e8e4bfe", "hash_type": "MD5", "filesize": 16629, "mtime": "2012-12-26 04:34:30", "url": "/6351/3/preview.png" } ], "eprint_id": 6351, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/12419" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/12419" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/12419" } ] } } ], "eprint_status": "archive", "userid": 51, "dir": "disk0/00/00/63/51", "datestamp": "2011-05-05 17:23:57", "lastmod": "2022-09-12 22:22:34", "status_changed": "2011-05-05 17:23:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jenet-Fredrick-August", "name": { "family": "Jenet", "given": "Fredrick August" }, "show_email": "NO" } ] }, "title": "High Time Resolution Observations of Radio Pulsars: The First Detection of Coherent Emission", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Recent advances in recording technology and computational power have made possible the development of a wide bandwidth digital recording system for radio astronomy. A prototype 50 MHz bandwidth system along with two production systems with 10-50 MHz bandwidth have been designed and built at Caltech. Signal processing techniques have been developed in order to remove various artifacts introduced into the signal by the digitization process. These techniques along with various pulsar signal processing algorithms have been successfully implemented in a suite of highly portable analysis programs designed to run on multi-purpose parallel supercomputers, networked workstations, and stand-alone workstations. The single pulse radio emission properties of the bright millisecond pulsar PSR J0437-4715 have been studied using standard analysis methods. New techniques have been developed in order to study the single pulse properties of \"weak\" or low-intensity pulsars. These techniques have been used to analyze the pulse-to-pulse amplitude and pulse shape variations of the fastest millisecond pulsar PSR B1937+21. Techniques have also been developed in order to search for the presence of coherent non-Gaussian emission statistics. Such statistics have been detected in pulsars B0823+26, B0950+08, and B1133+16. This is the first time such a phenomenon has been observed.\r\n", "date": "2001", "date_type": "degree", "id_number": "CaltechTHESIS:04252011-131341033", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04252011-131341033", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Tony Diaz", "deposited_on": "2011-05-05 17:23:57", "doi": "10.7907/frka-dh94", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Harrison-F-A", "name": { "family": "Harrison", "given": "Fiona A." }, "orcid": "0000-0003-2992-8024", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2000-09-19", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2001", "author_list": "Jenet, Fredrick August" }, { "id": "/id/eprint/4089", "eprint_id": 4089, "rev_number": 12, "documents": [ { "id": "/id/document/6765", "doc_id": 6765, "rev_number": 4, "files": [ { "id": "/id/file/40998", "fileid": 40998, "datasetid": "document", "objectid": 6765, "filename": "Gal_rr_2001.pdf", "mime_type": "application/pdf", "filesize": 40256991, "mtime": "2012-12-26 03:05:19", "url": "/4089/1/Gal_rr_2001.pdf" } ], "eprint_id": 4089, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Gal_rr_2001.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23297" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23297" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23297" } ] } }, { "id": "/id/document/23297", "doc_id": 23297, "rev_number": 3, "files": [ { "id": "/id/file/40996", "fileid": 40996, "datasetid": "document", "objectid": 23297, "filename": "preview.png", "mime_type": "image/png", "hash": "0b8d7a3baeb972e32238b9d46db2764d", "hash_type": "MD5", "filesize": 18527, "mtime": "2012-12-26 03:05:19", "url": "/4089/2/preview.png" } ], "eprint_id": 4089, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6765" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6765" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6765" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/40/89", "datestamp": "2008-10-24", "lastmod": "2022-09-12 22:03:09", "status_changed": "2009-09-25 03:11:15", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gal-Roy-R", "name": { "family": "Gal", "given": "Roy R." }, "orcid": "0000-0001-8255-6560", "show_email": "NO" } ] }, "title": "The Northern Sky Optical Cluster Survey: Galaxy Clusters from Five Thousand Square Degrees of DPOSS", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy)", "abstract": "Clusters of galaxies are the largest bound systems in the Universe and, as such, have been used to study how matter is distributed over extremely large scales. They provide fundamental constraints for theories of large-scale structure formation and evolution, and are valuable samples for studying galaxy evolution in dense environments. Despite their importance, the last large-area Northern sky cluster catalog was produced over forty years ago, via visual inspection of photographic plates of POSS-I, presented in George Abell's seminal 1958 paper and thesis. To remedy the limitations of this earlier work, we present a modern, objectively generated catalog of galaxy clusters drawn from the object catalogs of the three-band Digitized Second Palomar Observatory Sky Survey (DPOSS). In this thesis we have undertaken the following:\r\n
This dissertation explores three separate issues in the field of gravitational-wave astronomy: optimal detection algorithms for quasi-periodic signals, gravitational-wave signatures of the equation of state in the early universe, and local Newtonian gravitational noise from nearby airborne masses as possible contaminants of the gravitational-wave signal.
\r\n\r\n\r\nContinuous quasi-periodic signals are waveforms that maintain phase coherence over times longer than practical observation times, although the phase may drift in a way that can be modeled with few parameters. Sensitivity to such signals is limited by the computational cost of the analysis, especially since the detection algorithm must search over many values of the parameters in the phase model; it is therefore crucial to develop computationally efficient search strategies. One such strategy is a hierarchical stack search: a technique combining coherent phase corrections on short stretches of data with incoherent frequency drift corrections among several such stretches. The procedure is repeated at least twice, with each pass increasing the confidence in any putative signal. This dissertation discusses how to choose parameter values and observation times for greatest sensitivity, and shows how several astrophysically interesting sources may be detectable by this method.
\r\n\r\n\r\nA background of gravitational waves originating in the Big Bang or a pre-Big-Bang collapsing universe will not thermalize in any cosmological epoch, but may be amplified by an intermediate epoch when the wavelengths were stretched outside the Hubble radius. The present-day spectral index is related simply and generically to the initial spectrum, and to the cosmological equation of state at the beginning and end of the intermediate epoch. This dissertation derives this relation, and compares it to related but more model-specific formulae in the current literature.
\r\n\r\n\r\nFinally, this dissertation considers two atmospheric sources of background Newtonian gravita\u00adtional noise (infrasonic pressure waves and wind-advected density perturbations), and two sources of transient Newtonian gravitational signals (atmospheric shockwaves and massive airborne bodies, especially tumbleweeds). Neither background noise source will exceed the noise floor for advanced detectors, but sonic booms and wind-borne debris striking the detector can both produce detectable spurious signals through their gravitational effects. Possible corrective measures arc discussed.
", "date": "2000", "date_type": "degree", "id_number": "CaltechTHESIS:08302017-093459499", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08302017-093459499", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9424337" }, { "agency": "NSF", "grant_number": "AST-9731698" }, { "agency": "NASA", "grant_number": "NAG5-6840" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-30 17:31:24", "doi": "10.7907/6xcj-0z64", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1999-10-22", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2000", "author_list": "Creighton, Teviet David" }, { "id": "/id/eprint/3275", "eprint_id": 3275, "rev_number": 13, "documents": [ { "id": "/id/document/5778", "doc_id": 5778, "rev_number": 3, "files": [ { "id": "/id/file/34253", "fileid": 34253, "datasetid": "document", "objectid": 5778, "filename": "Murphy_tw_2000.pdf", "mime_type": "application/pdf", "filesize": 16977876, "mtime": "2012-12-26 02:58:40", "url": "/3275/1/Murphy_tw_2000.pdf" } ], "eprint_id": 3275, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Murphy_tw_2000.pdf", "language": "en", "security": "public", "license": "other", "main": "Murphy_tw_2000.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22319" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22319" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22319" } ] } }, { "id": "/id/document/22319", "doc_id": 22319, "rev_number": 3, "files": [ { "id": "/id/file/34251", "fileid": 34251, "datasetid": "document", "objectid": 22319, "filename": "preview.png", "mime_type": "image/png", "hash": "d512bb14d3e025017a429f136e563a53", "hash_type": "MD5", "filesize": 10313, "mtime": "2012-12-26 02:58:39", "url": "/3275/2/preview.png" } ], "eprint_id": 3275, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5778" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5778" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5778" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/75", "datestamp": "2008-09-04", "lastmod": "2020-12-02 02:46:20", "status_changed": "2009-09-25 02:55:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "tmurphy@physics.ucsd.edu", "id": "Murphy-Thomas-Williams-Jr", "name": { "family": "Murphy", "given": "Thomas Williams, Jr." }, "orcid": "0000-0003-1591-6647", "show_email": "NO" } ] }, "title": "Ultraluminous Infrared Galaxies: Power Sources and Ages Along the Merger Sequence", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Ultraluminous infrared galaxies (ULIRGs) are the most luminous galaxies in the local universe, with power outputs above 10\u00b9\u00b2 times that of our sun. Almost all ULIRGs are found to be associated with collisions between large, gas-rich galaxies. With most of the energy output emerging at far-infrared wavelengths, these galaxies are understood to be extremely dusty. As such, the nature of the power source within the dust shroud is not clearly understood. The two most likely explanations involve either a massive burst of star formation or the presence of an active galactic nucleus (AGN) in the form of a dust-enshrouded quasar.
\r\n\r\nThis work presents two separate approaches to investigating the nature of ultraluminous infrared galaxies. The first is a spectrosciopic survey of 33 ULIRGs in the near-infrared band around a wavelength of 2 microns, where dust extinction is much less severe than in visible light. The aim of this study is to search for evidence of buried AGN, as indicated by velocity-broadened hydrogen recombination lines as well as the presence of the high excitation [Si VI] emission line. This survey finds that signs of AGN are rare in ULIRGs, with the most natural conclusion being that the majority of ULIRGs are powered by starburst phenomena.
\r\n\r\nThe second approach presented involves the design, construction, and use of a novel instrument built specifically to study the spatial and kinematical properties of gas within the morphologically complex ULIRGs. A single long slit is generally not capable of capturing the rich phenomenology found in the complex environments of ULIRGs. Data from the Palomar Integral Field Spectrograph reveals that several ULIRGs are found to exist at times very early in the galaxy encounter process. The possibility that ultraluminous activity may develop so early in the merger history suggests a non-trivial luminosity evolution among galaxy mergers, wherein the less powerful class of luminous infrared galaxies may represent a different phase of the same overall phenomenon.
\r\n", "date": "2000", "date_type": "degree", "id_number": "CaltechETD:etd-08292008-130426", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08292008-130426", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-04", "doi": "10.7907/JR80-9T40", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "chair" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "member" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-29", "thesis_defense_date": "2000-05-17", "thesis_approved_date": "2008-09-04", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2000", "author_list": "Murphy, Thomas Williams, Jr." }, { "id": "/id/eprint/480", "eprint_id": 480, "rev_number": 11, "documents": [ { "id": "/id/document/716", "doc_id": 716, "rev_number": 2, "files": [ { "id": "/id/file/4537", "fileid": 4537, "datasetid": "document", "objectid": 716, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 2085207, "mtime": "2012-12-26 02:30:03", "url": "/480/1/thesis.pdf" } ], "eprint_id": 480, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "thesis.pdf", "language": "en", "security": "public", "license": "other", "main": "thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17534" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17534" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17534" } ] } }, { "id": "/id/document/17534", "doc_id": 17534, "rev_number": 2, "files": [ { "id": "/id/file/4535", "fileid": 4535, "datasetid": "document", "objectid": 17534, "filename": "preview.png", "mime_type": "image/png", "hash": "d6e52dfe0215129c543beae75f5a090f", "hash_type": "MD5", "filesize": 12632, "mtime": "2012-12-26 02:30:03", "url": "/480/2/preview.png" } ], "eprint_id": 480, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/716" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/716" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/716" } ] } }, { "id": "/id/document/119942", "doc_id": 119942, "rev_number": 1, "files": [ { "id": "/id/file/365311", "fileid": 365311, "datasetid": "document", "objectid": 119942, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "0ba7d4e01a91593abaed7e28bc69e91b", "hash_type": "MD5", "filesize": 23883, "mtime": "2021-06-23 20:28:21", "url": "/480/3/indexcodes.txt" } ], "eprint_id": 480, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/716" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/716" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/716" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/04/80", "datestamp": "2004-02-06", "lastmod": "2020-03-10 23:29:40", "status_changed": "2009-09-25 01:38:15", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "goutam@ieee.org", "id": "Chattopadhyay-Goutam", "name": { "family": "Chattopadhyay", "given": "Goutam" }, "orcid": "0000-0001-7942-5025", "show_email": "YES" } ] }, "title": "Dual polarized and balanced receivers at millimeter and submillimeter wavelengths", "ispublished": "unpub", "full_text_status": "public", "keywords": "Balanced Receivers; Dual Polarization; Submillimeter Wavelengths", "abstract": "Dramatic advances in millimeter and submillimeter wave receivers in recent years have resulted from the development of superconductor insulator superconductor (SIS) mixers, which now offer unsurpassed performance from 70 GHz to 1 THz. To increase the sensitivity of the receivers further at these frequencies, one needs to use dual-polarized and balanced receivers. When both the polarizations are received simultaneously, there is a square root of two improvement in the signal to noise ratio (SNR). Balanced mixers improve the sensitivity of receivers by suppressing local oscillator (LO) amplitude modulation (AM) noise and rejecting LO thermal noise. This thesis describes the design, fabrication and performance of mixers and components for low noise dual-polarized and balanced receivers at millimeter and submillimeter wavelengths both in quasi-optical and waveguide configurations. The quasi-optical receiver utilizes a novel cross-slot antenna on a silicon hyperhemispherical lens, two junction tuning circuits, niobium trilayer junctions, and an IF circuit containing a lumped element 180 degree hybrid. The antenna has four feed points, two for each polarization; and each feed point is coupled to a two-junction SIS mixer. For dual polarization operation, the mixer is mounted in such a way that a single LO can pump the junctions for both the polarizations. For the balanced receiver, the LO and the RF signals are coupled to the mixer in orthogonal polarizations using a wire-grid polarizer. For waveguide dual polarization receivers, a moderately broadband septum ortho-mode transducer (OMT) is designed and experimental results are presented at millimeter wavelengths. Broadband finline OMTs are investigated for possible use at millimeter wavelengths, and experimental results of a finline OMT is presented at X-band.", "date": "2000", "date_type": "degree", "id_number": "CaltechETD:etd-02032004-163517", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-02032004-163517", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-02-06", "doi": "10.7907/RMVX-0619", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Rutledge-D-B", "name": { "family": "Rutledge", "given": "David B." }, "role": "chair" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "co-chair" }, { "id": "Hajimiri-A", "name": { "family": "Hajimiri", "given": "Ali" }, "role": "member" }, { "id": "Carlstrom-J-E", "name": { "family": "Carlstrom", "given": "John E." }, "role": "member" }, { "id": "Weinreb-S", "name": { "family": "Weinreb", "given": "Sander" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-02-03", "thesis_defense_date": "1999-09-17", "thesis_approved_date": "2004-02-06", "review_status": "approved", "option_major": { "items": [ "eleceng" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2000", "author_list": "Chattopadhyay, Goutam" }, { "id": "/id/eprint/3596", "eprint_id": 3596, "rev_number": 13, "documents": [ { "id": "/id/document/6168", "doc_id": 6168, "rev_number": 4, "files": [ { "id": "/id/file/36898", "fileid": 36898, "datasetid": "document", "objectid": 6168, "filename": "Behr_bb_2000.pdf", "mime_type": "application/pdf", "filesize": 5366317, "mtime": "2012-12-26 03:01:13", "url": "/3596/1/Behr_bb_2000.pdf" } ], "eprint_id": 3596, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Behr_bb_2000.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22706" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22706" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22706" } ] } }, { "id": "/id/document/22706", "doc_id": 22706, "rev_number": 3, "files": [ { "id": "/id/file/36896", "fileid": 36896, "datasetid": "document", "objectid": 22706, "filename": "preview.png", "mime_type": "image/png", "hash": "309e634edae1acb450e4d3ed73b6c706", "hash_type": "MD5", "filesize": 8876, "mtime": "2012-12-26 03:01:13", "url": "/3596/2/preview.png" } ], "eprint_id": 3596, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6168" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6168" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6168" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/96", "datestamp": "2008-09-18", "lastmod": "2023-01-18 22:44:26", "status_changed": "2009-09-25 03:01:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Behr-Bradford-B", "name": { "family": "Behr", "given": "Bradford B." }, "show_email": "NO" } ] }, "title": "A New Spin on Horizontal-Branch Stars: Anomalous Abundances and Rapid Rotation Rates", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "High-resolution spectroscopy of blue horizontal-branch stars in metal-poor globular clusters reveals remarkable differences in photospheric composition and rotation rate between cooler and hotter stars. For the cooler stars (Teff < 11000 K), the derived abundances are in good agreement with the canonical cluster metallicities, and we confirm the range of v sin i rotation velocities, some as high as 40 km s-1, previously reported in the literature. In the hotter stars, however, metals are enhanced by factors of 100 or more, and helium is depleted by as much as two orders of magnitude. In addition, the hot stars are almost exclusively slow rotators, with v sin i < 8 km s-1. The anomalous abundances are due to atomic diffusion mechanisms \u2014 gravitational settling of helium, and radiative levitation of metals - in the stable, non-convective atmospheres of these hot stars. The enhanced metal content in the stellar photospheres can alter the emergent spectral energy distributions, creating the photometric \"gaps\" observed in the clusters' color-magnitude diagrams. We discuss the connections between rotation and the diffusion mechanisms, and explore potential implications regarding the internal structure and evolution of these stars.", "date": "2000", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-111737", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-111737", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-18", "doi": "10.7907/rdxg-qg24", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "McCarthy-James-K", "name": { "family": "McCarthy", "given": "James K." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673", "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "orcid": "0000-0002-0603-3087", "role": "member" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "McCarthy-James-K", "name": { "family": "McCarthy", "given": "James K." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "2000-05-16", "thesis_approved_date": "2008-09-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2000", "author_list": "Behr, Bradford B." }, { "id": "/id/eprint/3669", "eprint_id": 3669, "rev_number": 23, "documents": [ { "id": "/id/document/6271", "doc_id": 6271, "rev_number": 3, "files": [ { "id": "/id/file/37574", "fileid": 37574, "datasetid": "document", "objectid": 6271, "filename": "Baker_aj_2000.pdf", "mime_type": "application/pdf", "filesize": 8695598, "mtime": "2012-12-26 03:01:57", "url": "/3669/1/Baker_aj_2000.pdf" } ], "eprint_id": 3669, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Baker_aj_2000.pdf", "language": "en", "security": "public", "license": "other", "main": "Baker_aj_2000.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/36/69", "datestamp": "2008-10-31", "lastmod": "2020-10-08 23:51:44", "status_changed": "2009-09-25 03:03:10", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "andrew.baker@rutgers.edu", "id": "Baker-Andrew-Jordan", "name": { "family": "Baker", "given": "Andrew Jordan" }, "orcid": "0000-0002-7892-396X", "show_email": "NO" } ] }, "title": "Molecular Gas in Nearby Active Galactic Nuclei", "ispublished": "unpub", "full_text_status": "public", "keywords": "radio astronomy; active galaxies; molecular gas", "abstract": "This thesis describes the distributions, physical conditions, and kinematics of the molecular gas in eight nearby galaxies whose Seyfert and LINER nuclei display broad H\u03b1 emission. We have mapped these systems at a linear resolution of ~ 100 pc in the CO(2-1) rotational transition, as well as at lower resolution in the CO(1-0) line, using the Owens Valley Radio Observatory millimeter array. Subsequent kinematical modelling allows us to improve on this angular resolution by exploiting our high effective velocity resolution; we simultaneously determine the radial emissivity profile of each line and the velocity field which the gas traces. Analysis of the molecular emission from individual objects reveals (1) massive concentrations of molecular gas (~ 10\u2079M\u2609) at small galactocentric radii (r \u2264 500 pc); (2) a pattern of high excitation at small radius, implied by variation in the ratio of CO (2-1) to CO(1-0) integrated intensities, which we attribute in part to the external heating of molecular clouds by energetic photons; (3) a high occurrence of nonaxisymmetric structures within 500 pc of the nucleus, including four gas bars; (4) evidence for episodic mass inflow along stellar bars outside 500 pc; and (5) apparent redirection of radio jets and ionizing photons from the nucleus by the molecular gas which they encounter. Our most striking discoveries are a dynamically decoupled secondary bar in the nucleus of NGC 7479, a mean integrated intensity ratio \u2265 1.85 in the nucleus of NGC 2681, and a warped molecular disk in the nucleus of NGC 1068.\r\n", "date": "2000", "date_type": "degree", "id_number": "CaltechETD:etd-09202008-104918", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09202008-104918", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-31", "doi": "10.7907/c2qn-2b77", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "chair" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-20", "thesis_defense_date": "2000-01-05", "thesis_approved_date": "2008-10-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2000", "author_list": "Baker, Andrew Jordan" }, { "id": "/id/eprint/3600", "eprint_id": 3600, "rev_number": 12, "documents": [ { "id": "/id/document/6172", "doc_id": 6172, "rev_number": 3, "files": [ { "id": "/id/file/36929", "fileid": 36929, "datasetid": "document", "objectid": 6172, "filename": "Chiang_e_2000.pdf", "mime_type": "application/pdf", "filesize": 5991255, "mtime": "2012-12-26 03:01:15", "url": "/3600/1/Chiang_e_2000.pdf" } ], "eprint_id": 3600, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Chiang_e_2000.pdf", "language": "en", "security": "public", "license": "other", "main": "Chiang_e_2000.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22710" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22710" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22710" } ] } }, { "id": "/id/document/22710", "doc_id": 22710, "rev_number": 3, "files": [ { "id": "/id/file/36927", "fileid": 36927, "datasetid": "document", "objectid": 22710, "filename": "preview.png", "mime_type": "image/png", "hash": "d4f5a5d565418136cb148958600774ad", "hash_type": "MD5", "filesize": 15300, "mtime": "2012-12-26 03:01:14", "url": "/3600/2/preview.png" } ], "eprint_id": 3600, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6172" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6172" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6172" } ] } }, { "id": "/id/document/46378", "doc_id": 46378, "rev_number": 3, "files": [ { "id": "/id/file/135890", "fileid": 135890, "datasetid": "document", "objectid": 46378, "filename": "chiang Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "0b3287925e31fc747c47f847450d205e", "hash_type": "MD5", "filesize": 768, "mtime": "2014-03-05 20:42:15", "url": "/3600/3/chiang Thesis Permission Form.txt" } ], "eprint_id": 3600, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "author ok 03052014", "language": "en", "security": "internal", "license": "other", "main": "chiang Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/36/00", "datestamp": "2008-11-05", "lastmod": "2019-12-21 04:43:05", "status_changed": "2009-09-25 03:01:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "echiang@astro.berkeley.edu", "id": "Chiang-E", "name": { "family": "Chiang", "given": "Eugene" }, "show_email": "NO" } ] }, "title": "Circumstellar and circumplanetary disks", "ispublished": "unpub", "full_text_status": "public", "keywords": "Circumstellar ; circumplanetary ; disks", "abstract": "This thesis studies disks in three astrophysical contexts: (1) protoplanetary disks; (2) the Edgeworth-Kuiper Belt; and (3) planetary rings.
\r\n\r\nWe derive hydrostatic, radiative equilibrium models of passive protoplanetary disks surrounding T Tauri and Herbig Ae/Be stars. Each disk is encased by an optically thin layer of superheated dust grains. This layer is responsible for up to ~70% of the disk luminosity at wavelengths between ~5 and 60 \u03bcm. The heated disk flares and absorbs more stellar radiation at a given stellocentric distance than a flat disk would. Spectral energy distributions are computed and found to compare favorably with the observed flattish infrared excesses of several young stellar objects. Spectral features from dust grains in the superheated layer appear in emission if the disk is viewed nearly face-on.
\r\n\r\nWe present the results of a pencil-beam survey of the Kuiper Belt using the Keck 10-m telescope. Two new objects are discovered. Data from all surveys are pooled to construct the luminosity function from mR = 20 to 27. The cumulative number of objects per square degree, \u2211(< mR, is such that log10\u2211(< mR = 0.52(mR - 23.5). The luminosity function is consistent with a power-law size distribution for which the smallest objects possess most of the surface area but the largest bodies contain most of the mass. To order-of-magnitude, 0.2M\u2d32 and 1 x 1010 comet progenitors lie between 30 and 50 AU. The classical Kuiper Belt appears truncated at a distance of 50 AU.
\r\n\r\nWe propose that rigid precession of narrow eccentric planetary rings surrounding Uranus and Saturn is maintained by a balance of forces due to ring self-gravity, planetary oblateness, and interparticle collisions. Collisional impulses play an especially dramatic role near ring edges. Pressure-induced accelerations are maximal near edges because there (1) velocity dispersions are enhanced by resonant satellite perturbations, and (2) the surface density declines steeply. Remarkably, collisional forces felt by material in the last ~100 m of a ~10 km wide ring can increase equilibrium masses up to a factor of ~100. New ring surface densities are derived which accord with Voyager radio measurements.
\r\n", "date": "2000", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-151500", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-151500", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-05", "doi": "10.7907/8B2W-8V06", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "co-chair" }, { "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "role": "member" }, { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "member" }, { "id": "Brown-M-E", "name": { "family": "Brown", "given": "Michael E." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "2000-05-11", "thesis_approved_date": "2008-11-05", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2000", "author_list": "Chiang, Eugene" }, { "id": "/id/eprint/3593", "eprint_id": 3593, "rev_number": 10, "documents": [ { "id": "/id/document/6165", "doc_id": 6165, "rev_number": 3, "files": [ { "id": "/id/file/36875", "fileid": 36875, "datasetid": "document", "objectid": 6165, "filename": "Krasnopolsky_r_2000.pdf", "mime_type": "application/pdf", "filesize": 6686386, "mtime": "2012-12-26 03:01:11", "url": "/3593/1/Krasnopolsky_r_2000.pdf" } ], "eprint_id": 3593, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Krasnopolsky_r_2000.pdf", "language": "en", "security": "public", "license": "other", "main": "Krasnopolsky_r_2000.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22703" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22703" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22703" } ] } }, { "id": "/id/document/22703", "doc_id": 22703, "rev_number": 3, "files": [ { "id": "/id/file/36873", "fileid": 36873, "datasetid": "document", "objectid": 22703, "filename": "preview.png", "mime_type": "image/png", "hash": "91ef503dd0181d593c7c94dd2333e53c", "hash_type": "MD5", "filesize": 14451, "mtime": "2012-12-26 03:01:11", "url": "/3593/2/preview.png" } ], "eprint_id": 3593, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6165" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6165" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6165" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/93", "datestamp": "2008-11-03", "lastmod": "2021-04-16 22:09:52", "status_changed": "2009-09-25 03:01:20", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Krasnopolsky-R", "name": { "family": "Krasnopolsky", "given": "Ruben" }, "show_email": "NO" } ] }, "title": "Hydromagnetic astrophysical outflows", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\n\r\nThe launching, acceleration and stability of MHD outflows were studied numerically in two and three dimensions using a parallelized version of the ZEUS code.\r\n\r\nThe launching from Keplerian accretion disks was investigated using time-dependent simulations, to determine parameter dependence and stability to 3D perturbations. The most critical factors controlling the cold outflows from the disk surface were found to be the poloidal magnetic field profile and the mass discharge rate: together they determine the acceleration of gas away from the disk, and the location of the Alfven surface, which, in turn, fixes the angular momentum loss and the asymptotic speed. The flows were found to be remarkably stable in 3D against perturbations of the initial conditions, at least in the formation region of the jet before the Alfven surface. This is surprising in the context of previous studies.\r\n\r\nIntermittent flows are found when the mass discharge rate is too large for a given magnetic field profile. This may be relevant to some observed episodic sources. This intermittency can be suppressed if the mass loading has the angular dependence suggested by the magnetocentrifugal mechanism, namely that the discharge is a function of the angle \u03b8 between the poloidal fieldline threading the disk and the rotation axis, turning off when \u03b8[...]30\u00b0. The mechanism of intermittency sets up a maximum mass loading to the observed smooth jets, may explain those that are pulsed, and shows a possible transition back and forth between both regimes. The result presented here may be compared to some recently published papers which suggest that intermittency could occur if the mass loading is too small: here it occurs when it is too large. If both results are generic, mass loading is bracketed for steady flows.\r\n\r\nLaunching from disks was simulated using a cold disk and atmosphere. The number of boundary conditions that was imposed on the disk surface is what is necessary and sufficient to take into account information propagating upstream from the fast and Alfven critical surfaces, avoiding over-determination of the flow and unphysical effects, such as numerical \"boundary layers\" that otherwise isolate the disk from the flow, produce impulsive accelerations and confuse the connection between the disk parameters and the flow.\r\n\r\nThe solar wind provides another example of an MHD outflow, using the high solar latitude observations by the satellite Ulysses. The simulations performed here allowed an estimate of the mean value of the azimuthal velocity, which is not directly accessible to measurement, and is necessary to estimate the torque of the solar wind. The Alfven point was found to be located at ~11R[...]. Similar outflows from faster rotators were simulated, and found to be collimated along the rotational axis.\r\n", "date": "2000", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-092907", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-092907", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-03", "doi": "10.7907/j2ak-0b24", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "advisor" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "2000-01-26", "thesis_approved_date": "2008-11-03", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "2000", "author_list": "Krasnopolsky, Ruben" }, { "id": "/id/eprint/3735", "eprint_id": 3735, "rev_number": 10, "documents": [ { "id": "/id/document/6351", "doc_id": 6351, "rev_number": 3, "files": [ { "id": "/id/file/38116", "fileid": 38116, "datasetid": "document", "objectid": 6351, "filename": "Fassnacht_cd_1999.pdf", "mime_type": "application/pdf", "filesize": 8198528, "mtime": "2012-12-26 03:02:31", "url": "/3735/1/Fassnacht_cd_1999.pdf" } ], "eprint_id": 3735, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Fassnacht_cd_1999.pdf", "language": "en", "security": "public", "license": "other", "main": "Fassnacht_cd_1999.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22889" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22889" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22889" } ] } }, { "id": "/id/document/22889", "doc_id": 22889, "rev_number": 3, "files": [ { "id": "/id/file/38114", "fileid": 38114, "datasetid": "document", "objectid": 22889, "filename": "preview.png", "mime_type": "image/png", "hash": "46705d906a5b07164bc29b6a11a00e1f", "hash_type": "MD5", "filesize": 17946, "mtime": "2012-12-26 03:02:31", "url": "/3735/2/preview.png" } ], "eprint_id": 3735, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6351" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6351" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6351" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/35", "datestamp": "2008-10-24", "lastmod": "2021-11-05 22:40:18", "status_changed": "2009-09-25 03:04:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fassnacht-Christopher-D", "name": { "family": "Fassnacht", "given": "Christopher D." }, "show_email": "NO" } ] }, "title": "Determining the distance scale with CLASS: studies of two new gravitational lenses and a measurement of the Hubble constant", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\n\r\nGravitational lenses have the potential to be excellent tools for investigating the Universe. This thesis describes the Cosmic Lens All-Sky Survey (CLASS), a program to find new gravitational lenses, and presents data on two newly-discovered lenses, 1608+656 and 2045+265. One of the major goals of CLASS is to find \"golden lenses,\" which can be used to measure the Hubble Constant H[...]. A measurement of H[...] requires the redshifts of the lensing object and the background source, a well-constrained model of the gravitational potential of the lensing object, and a measurement of time delays between the images of the background source.\r\n\r\nThe 1608+656 system contains four images of the background source, which is the unresolved core of a classical radio double source. The lensing galaxy is at a redshift of [...] = 0.630, while the background source is at a redshift of [...] = 1.394. Interestingly, the spectrum of the background object indicates that it is an \"E + A\" galaxy. Ground-based optical and infrared images clearly show the lensing galaxy at the location predicted by the lens models. Images taken with instruments on the Hubble Space Telescope further resolve the lensing galaxy into two distinct objects, which may be a merging pair of galaxies.\r\n\r\nRadio maps of the 2045+265 system also show four images of the background source. In addition, a fifth component appears in the maps. The radio spectrum of the fifth component is significantly different from the spectra of the other four components, and its location matches that of the lensing galaxy to within the positional errors. Therefore, it appears that the fifth component is the flat-spectrum core of the lensing galaxy. The redshift of the lensing galaxy is [...] = 0.8673. The spectrum of the background source shows one broad emission line, which appears to be Mg II at a redshift of [...] = 1.28. However, this redshift implies that the lensing galaxy is unusually massive and would have a rotation velocity two to three times what is observed in nearby galaxies of the same type. There is either a significant contribution by dark (or underluminous) matter associated with the lensing object or the source redshift is incorrect. More sensitive spectroscopy is needed to resolve this issue.\r\n\r\nPreliminary observations of the 1608+656 system showed that the component flux densities varied by ~15% on time scales of months. For this reason, I conducted a dedicated monitoring program with the Very Large Array (VLA) from October 1996 to May 1997. The observations took place, on average, every four days. The calibrated light curves for components A, B, C, and D show variations in flux density at the 3-5% level. Although the fractional variations are small, the time delays between the curves can be measured. The final values are [...], and [...], where the 95% confidence levels have been obtained from Monte Carlo simulations. The model of the mass distribution of the lens correctly reproduces the image positions, flux ratios, and time delay ratios. The combination of the measured time delays with the lens model yields the first determination of H[...] from a CLASS lens: H[...] = [...] (statistical) \u00b1 15(systematic) km sec[superscript -1] Mpc[superscript -1].", "date": "1999", "date_type": "degree", "id_number": "CaltechETD:etd-09232008-094506", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232008-094506", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-24", "doi": "10.7907/pe8p-yc41", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-23", "thesis_defense_date": "1998-10-19", "thesis_approved_date": "2008-10-24", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1999", "author_list": "Fassnacht, Christopher D." }, { "id": "/id/eprint/7435", "eprint_id": 7435, "rev_number": 31, "documents": [ { "id": "/id/document/35012", "doc_id": 35012, "rev_number": 3, "files": [ { "id": "/id/file/110772", "fileid": 110772, "datasetid": "document", "objectid": 35012, "filename": "Kass 1999.pdf", "mime_type": "application/pdf", "hash": "4e89fd49a892a913b11a872673a9a1fe", "hash_type": "MD5", "filesize": 30724454, "mtime": "2013-01-25 16:28:32", "url": "/7435/8/Kass 1999.pdf" } ], "eprint_id": 7435, "pos": 8, "placement": 8, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Kass 1999.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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50, "dir": "disk0/00/00/74/35", "datestamp": "2013-01-25 23:32:53", "lastmod": "2023-11-08 00:36:10", "status_changed": "2013-01-25 23:32:53", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kass-David-M", "name": { "family": "Kass", "given": "David M." }, "show_email": "NO" } ] }, "title": "Change in the Martian Atmosphere", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Applied Computation", "abstract": "There are several lines of evidence that the atmosphere of Mars has significantly\r\nevolved over the history of the planet. Because Mars does not have a strong intrinsic\r\nmagnetic field, the atmosphere is eroded by interactions with the solar wind. Conditions\r\nin the early solar-system significantly enhanced this loss, notably the component\r\ndue to solar-wind induced sputtering away. Modeling indicates that, integrated over\r\nthe last 3.5 billion years, 0.8 bars of CO_2 have been sputtered. This is accompanied by\r\nthe loss of 50 m of water. The loss of CO_2 is a significant loss when compared to the\r\nestimates of the thickness of the early atmosphere. A simple model of the behavior of\r\nthe atmospheric \u03b4^(13)C, based on the expected Martian carbon \"cycle\" constrains the\r\nsize the current CO_2 reservoirs by putting the sputtering loss into the context of the\r\nevolution of the atmosphere. In order to balance the isotopic effects of the sputtering\r\nloss, it is necessary for there to be ~ 100 mbars of CO_2 trapped in the planet. This\r\nis quite reasonable given the ability of the regolith to hold adsorbed CO_2.
\r\n\r\nUsing a modified form of Optimal Interpolation, it is possible to assimilate Thermal\r\nEmission Spectrometer (TES) observations from the Mars Global Surveyor (MGS)\r\nspacecraft into the Ames Mars General Circulation Model (MGCM). The method is\r\noptimized for the assimilation of the irregular data obtained during the aerobraking\r\nphase of the mission. Based on 25 sols of data at L_s \u2248 200, the assimilation process\r\nreveals several interesting features of the Martian atmosphere. The assimilation indicates\r\nthat the lower atmosphere (up to ~ 0.1 mbar) in the northern polar regions is\r\nvery cold-probably at or close to the CO_2 condensation temperature. Furthermore,\r\nthe data imply that the midlatitudinal westerly jets extend poleward of the indicated\r\nMGCM locations. In addition to correcting the phasing of the Northern baroclinic\r\nstorm belt, the data indicate that the amplitude of the waves are stronger than expected\r\nand possibly with a lower zonal wavenumber. Thus the data and assimilation\r\nallows the MGCM to create the 1997 Martian Fall instead of a random Fall.
\r\n", "date": "1999", "date_type": "degree", "id_number": "CaltechTHESIS:01242013-162910396", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01242013-162910396", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_on": "2013-01-25 23:32:53", "doi": "10.7907/1mbp-xd62", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" }, { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1999-02-25", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "appliedmath" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1999", "author_list": "Kass, David M." }, { "id": "/id/eprint/3498", "eprint_id": 3498, "rev_number": 12, "documents": [ { "id": "/id/document/6055", "doc_id": 6055, "rev_number": 4, "files": [ { "id": "/id/file/36120", "fileid": 36120, "datasetid": "document", "objectid": 6055, "filename": "Oppenheimer_br_1999.pdf", "mime_type": "application/pdf", "filesize": 16237848, "mtime": "2012-12-26 03:00:28", "url": "/3498/1/Oppenheimer_br_1999.pdf" } ], "eprint_id": 3498, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Oppenheimer_br_1999.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22595" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22595" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22595" } ] } }, { "id": "/id/document/22595", "doc_id": 22595, "rev_number": 3, "files": [ { "id": "/id/file/36118", "fileid": 36118, "datasetid": "document", "objectid": 22595, "filename": "preview.png", "mime_type": "image/png", "hash": "c9e095bf028084581ac01d6877c82dfc", "hash_type": "MD5", "filesize": 12328, "mtime": "2012-12-26 03:00:28", "url": "/3498/2/preview.png" } ], "eprint_id": 3498, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6055" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6055" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6055" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/98", "datestamp": "2006-09-27", "lastmod": "2020-02-20 18:49:24", "status_changed": "2009-09-25 02:59:39", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "roppenheimer@amnh.org", "id": "Oppenheimer-Rebecca", "name": { "family": "Oppenheimer", "given": "Ben R." }, "orcid": "0000-0001-7130-7681", "show_email": "NO" } ] }, "title": "Direct Detection of Brown Dwarf Companions of Nearby Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy ; brown dwarf", "note": "Ben R. Oppenheimer is also known as Rebecca Oppenheimer.", "abstract": "This thesis presents the first direct detection of a substellar companion of a star other than the Sun. This object, a brown dwarf called Gliese 229B, presented a unique opportunity to characterize low-temperature brown dwarfs for the first time. The discovery and initial spectrum of Gliese 229B show that the object must be substellar based on its intrinsic luminosity of 6.4 x 10-6 L\u2609 and its cool surface temperature, 900 K. Detailed study of Gliese 229B includes extensive photometric measurements from 0.5 to 12 \u00b5m, high signal-to-noise ratio spectroscopy from 0.84 to 5.0 \u00b5m and the detection of 0\".1 yr -1 of orbital motion. These results are presented in Chapters 2 and 3.
\r\n\r\nA detailed review of brown dwarf science leads to a complete and scientifically meaningful definition of the classes \"planet\" and \"brown dwarf\" in Chapter 1.
\r\n\r\nAfter the discovery of Gliese 229B, which was found in a survey for companions of young stars, we began an extensive search for brown dwarf companions in orbit about all known stars within 8 pc of the Sun and with \u03b4 > -35\u00b0. The search includes optical coronagraphic and infrared direct imaging of these stars, conducted on the Palomar 60\" and 200\" telescopes respectively. The search was designed to find companions of each star without color bias. While the search revealed no other brown dwarf companions of these stars, it did uncover 6 new stellar companions. The sensitivity limits of the survey permit the detection of brown dwarfs up to four magnitudes fainter than Gliese 229B around 90% of the stars. The sensitivity is, however, not-uniform spatially or from star to star. This limits our ability to make strong statements about the prevalence of brown dwarf companions of nearby stars. The survey does have sensitivity to all stellar companions between 3 and 30\" from the survey stars, however.
\r\n\r\nChapter 5 describes related work on very low-mass stars in the Pleiades star cluster. This optical spectroscopy involved trying to find a brown dwarf member of the Pleiades by identifying lithium absorption features. We revealed no brown dwarf members of the Pleiades but did discover two members with ages much younger than the age of the Pleiades (120 Myr). We provide an adequate explanation for the presence of these stars.
\r\n\r\nThe three appendices summarize work conducted in association with the Palomar Adaptive Optics System. The work includes (1) the detailed study and characterization of the deformable mirror, (2) invention of a fast calibration scheme for the deformable mirror and (3) the design and implementation of the fast steering mirror.
\r\n", "date": "1999", "date_type": "degree", "id_number": "CaltechETD:etd-09122006-131150", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09122006-131150", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-09-27", "doi": "10.7907/5C8H-1A83", "alt_title": { "items": [ "Brown Dwarf Companions of Nearby Stars" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-09-12", "thesis_defense_date": "1999-04-30", "thesis_approved_date": "2006-09-27", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1999", "author_list": "Oppenheimer, Ben R." }, { "id": "/id/eprint/10396", "eprint_id": 10396, "rev_number": 19, "documents": [ { "id": "/id/document/82337", "doc_id": 82337, "rev_number": 3, "files": [ { "id": "/id/file/232605", "fileid": 232605, "datasetid": "document", "objectid": 82337, "filename": "Levin_y_1999.zip", "mime_type": "application/x-zip", "hash": "80d69e14e1422acbd906a5871531ab6d", "hash_type": "MD5", "filesize": 115201335, "mtime": "2017-08-31 15:56:29", "url": "/10396/1/Levin_y_1999.zip" } ], "eprint_id": 10396, "pos": 1, "placement": 1, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Levin_y_1999.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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"datestamp": "2017-08-31 17:17:26", "lastmod": "2021-04-16 22:33:42", "status_changed": "2017-08-31 17:17:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levin-Yuri", "name": { "family": "Levin", "given": "Yuri" } } ] }, "title": "Topics in Physics and Astrophysics of LIGO", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis deals with three topics, all of which are related to the generation or detection of gravitational waves:
\r\n\r\n(I) The Standard Quantum Limit (SQL) for LIGO and Quantum Non\u00ad demolition (QND) measurements, which allow one to overcome the SQL. Two particular QND measurement schemes are considered: (i) a Speed Meter, in which a small Fabry-Perot cavity attached to a LIGO test mass produces a phase shift proportional to the test mass's speed; and (ii) the Braginsky-Khalili nonlinear meter (BK-meter), in which a gravity-wave-induced motion of the nodes of the light beam inside a LIGO optical cavity is read out using a nonlinear medium which couples light to a microwave readout device. Our analysis shows that
\r\n\r\n(a) Using the Speed Meter one can perform naturally a broad-band QND mea\u00adsurement of a force acting on the test mass; however, this requires circulating light power which is unrealistically high for LIGO.
\r\n\r\n(b) The BK-meter can provide a natural way to perform a narrow-band QND measurement of a force acting on the mirrors of the optical cavity.
\r\n\r\nWhile neither of these QND measurement schemes can be immediately imple\u00ad mented for LIGO, they might provide conceptual steps towards the design of a prac\u00adtical QND interferometer.
\r\n\r\n(II) Mechanical thermal noise in LIGO. We develop a new method of calcu\u00ad lating thermal noise in mechanical systems, which is based on a direct application of the Fluctuation-Dissipation theorem. This method is capable of handling mechanical systems with inhomogeneous dissipation, by contrast with previous met hods (based on decomposing motion of the system into normal modes), which give incorrect results when the dissipation is inhomogeneous.
\r\n\r\nWe apply our direct method to an internal thermal noise in LIGO test masses.\r\nWe find that:
\r\n\r\n(a) The test-mass surface defects will make a larger contribution to thermal noise than was previously inferred by combining the (incorrect) mode-sum met hod with measurements of the Q's of the test masses' modes.
\r\n\r\n(b)Our direct met hod is more precise and computationally less expensive for small beam sizes than the previous mode-sum method.
\r\n\r\nWe also apply our direct method of analysis to suspension thermal noise in LIGO. We find that by careful positioning the laser beam spot on the mirror face and by monitoring independently the motion of the suspension wires, it may be possible to reduce the suspension thermal noise by a factor ~ 100 in spectral density.
\r\n\r\n(III) R-modes in Neutron Stars (NS) in Low-Mass X-ray Binaries (LMXBs). We study the suggestion that the accretion of gas onto a neutron star in an LMXB triggers an instability in which the star's r-modes are amplified by gravitational-wave emission. We find that if this is the case, then the subsequent neutron-star evolution depends critically on whether the neutron-star viscosity decreases with temperature, or is temperature-independent.
\r\n\r\nIn the former case, the Neutron Star goes through runaway cycles of rapid (~ 1 month) heating-rapid (~ 1 month) spindown-slow (~ 105 years) cooling-slow (~ 106 years) spin-up. In this scenario the duration of the gravitational radiation from the unstable r-modes is so short that even LIGO-III interferometers are unlikely to be able to catch a single LMXB in the throes of its gravitational-wave emission.
\r\n\r\nIn the latter (temperature-independent) case, however, the Neutron Star probably settles down into an equilibrium state with constant spin rate and temperature, and becomes a steady emitter of gravitational waves, which might be detectible by LIGO\u00ad II interferometers.
\r\n\r\nAll the capters in this thesis, except the introductory chapter I, have been published or are in press.
\r\n\r\n\r\n\r\n", "date": "1999", "date_type": "degree", "id_number": "CaltechTHESIS:08292017-115000442", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08292017-115000442", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-31 17:17:26", "doi": "10.7907/ped8-ec41", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1999-05-07", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1999", "author_list": "Levin, Yuri" }, { "id": "/id/eprint/2529", "eprint_id": 2529, "rev_number": 9, "documents": [ { "id": "/id/document/4788", "doc_id": 4788, "rev_number": 3, "files": [ { "id": "/id/file/27654", "fileid": 27654, "datasetid": "document", "objectid": 4788, "filename": "Benford_dj_1999.pdf", "mime_type": "application/pdf", "filesize": 41430897, "mtime": "2012-12-26 02:52:23", "url": "/2529/1/Benford_dj_1999.pdf" } ], "eprint_id": 2529, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Benford_dj_1999.pdf", "language": "en", "security": "public", "license": "other", "main": "Benford_dj_1999.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21340" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21340" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21340" } ] } }, { "id": "/id/document/21340", "doc_id": 21340, "rev_number": 3, "files": [ { "id": "/id/file/27652", "fileid": 27652, "datasetid": "document", "objectid": 21340, "filename": "preview.png", "mime_type": "image/png", "hash": "eaa99cb3436454e5a896039700a25fe2", "hash_type": "MD5", "filesize": 11898, "mtime": "2012-12-26 02:52:22", "url": "/2529/2/preview.png" } ], "eprint_id": 2529, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4788" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4788" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4788" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/25/29", "datestamp": "2008-06-09", "lastmod": "2021-04-16 22:25:23", "status_changed": "2009-09-25 02:39:54", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "dominic.benford@nasa.gov", "id": "Benford-D-J", "name": { "family": "Benford", "given": "Dominic James" }, "show_email": "NO" } ] }, "title": "Broadband submillimeter instrumentation for the detection of distant galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "bolometer; quasar; spectrometer; submillimeter", "abstract": "This research details my efforts to search the universe for the faint far-infrared emission of galaxies as far away as possible. I first describe the design, construction, use, and performance evaluation of the Submillimeter High Angular Resolution Camera (SHARC), a 24-element bolometer camera for imaging at 350 microns and 450 microns from the Caltech Submillimeter Observatory (CSO). This instrument achieves background-limited performance and has been available for use by the international community since 1996.\r\n\r\nIn the following two chapters, I detail the astronomical results attained with this instrument when used to observe the thermal dust emission from a sample of nearby galaxies (chapter 3) and a sample of sources as distant as 90% of the way across the spacetime universe (chapter 4). The nearby sample is well-characterized by a single-component greybody dust emission model with a temperature of 37 +/- 4K and a spectral emissivity index of beta = 1.7 +/- 0.4. Our cosmologically distant sample provides the first systematic study of these objects at wavelengths probing near the emission peak at a rest-frame wavelength of approximately 80 microns. We find an average temperature of 53 +/- 8K and determine a median luminosity of (2 +/- 1)x10^13 L_sun and a median dust mass of (3 +/- 2)x10^8 M_sun. This makes these objects some of the most massive and luminous ever observed, with an inferred star formation rate of 2000 M_sun per year.\r\n\r\nTo balance the continuum emission results described above, I have observed both local and high-redshift galaxies with the CSO facility heterodyne receivers in an effort to detect the emission lines of CO, Cii, and Nii. We have observed a sample of 22 nearby (0.02 < z < 0.13) ultraluminous infrared galaxies in the J = 2 to 1 and J = 3 to 2 transitions of CO. Using published 1 to 0 intensities, we find that the 3 to 2 emission most likely arises from an optically thick region, implying that future observations in the higher-J lines can be used to constrain the temperature of the molecular gas in these galaxies. We find a most likely temperature in the range 20 < T < 60K and a molecular gas density of n(H2) [approx] 1500 cm^-3. At high redshifts (z > 2), however, most of our observations have resulted in nondetections, but not without merit. The emission in the Nii 205 micron line from the Cloverleaf quasar is found to be below the amount predicted for a galaxy similar to M82. For two z > 4 quasars, our upper limits to the Cii 158 micron line emission show that the ratio of the line luminosity to the total luminosity is less than 0.01%, ten times smaller than has been observed locally.\r\n\r\nFinally, I shall detail our effort to design a novel submillimeter spectrometer using a linear bolometer array as a detector element and relying on Fabry-Perot or immersed grating optics to provide the spectral dispersion. This approach promises to provide bandwidths several times larger than are available with existing heterodyne spectrometers, making the detection of cosmologically distant galaxies in their submillimeter line emission a reality.", "date": "1999", "date_type": "degree", "id_number": "CaltechETD:etd-06092008-100026", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06092008-100026", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-06-09", "doi": "10.7907/7eha-q373", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-06-09", "thesis_defense_date": "1999-02-05", "thesis_approved_date": "2008-06-09", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1999", "author_list": "Benford, Dominic James" }, { "id": "/id/eprint/3733", "eprint_id": 3733, "rev_number": 24, "documents": [ { "id": "/id/document/6349", "doc_id": 6349, "rev_number": 3, "files": [ { "id": "/id/file/38104", "fileid": 38104, "datasetid": "document", "objectid": 6349, "filename": "Ogle_pm_1998.pdf", "mime_type": "application/pdf", "filesize": 8512124, "mtime": "2012-12-26 03:02:30", "url": "/3733/1/Ogle_pm_1998.pdf" } ], "eprint_id": 3733, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Scanned (no OCR) Ogle_pm_1998", "language": "en", "security": "internal", "license": "other", "main": "Ogle_pm_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/103824" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/103824" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/103824" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/33", "datestamp": "2008-10-08", "lastmod": "2019-12-21 01:58:25", "status_changed": "2009-09-25 03:04:22", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "pogle@stsci.edu", "id": "Ogle-Patrick-Michael", "name": { "family": "Ogle", "given": "Patrick Michael" }, "orcid": "0000-0002-3471-981X", "show_email": "YES" } ] }, "title": "Polarization and Structure of Broad Absorption Line Quasi-Stellar Objects", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "This thesis is a spectropolarimetric survey of broad absorption line quasi-stellar objects (BAL QSO). We observed 36 BAL QSO at low resolution with the 5 m Hale Telescope at Palomar Observatory and the 10 m Keck Telescopes at the W. M. Keck Observatory.
\r\n\r\nThe continuum, absorption trough, and emission line polarization of BAL QSO were studied in detail, yielding clues about the geometrical structure of gas in the inner regions of quasars. BAL QSO have, on average, higher polarization than other quasars, reinforcing the view that they are normal quasars viewed from a more equatorial aspect. However, there is a wide distribution of polarization values, which may be due to intrinsic differences in the geometry or optical depth to scattering. No correlations are found among emission line or broad absorption line properties and continuum polarization, suggesting that these properties are regulated by internal differences unrelated to viewing angle. The continuum polarization of BAL QSO is weakly wavelength dependent after correction for emission line dilution. In most objects, the polarization rises to the blue, suggesting that dust scattering or absorption may be important.
\r\n\r\nBroad emission line photons are polarized less than the continuum; and the position angle of the electric vector is rotated with respect to the continuum. The semi-forbidden C III] emission line is polarized differently than the C IV emission line in some cases, suggesting resonance scattering in the C III] emission line region. Resonantly scattered photons from the broad absorption line region are detected at high velocities red-ward and blue-ward of the C IV line center in the spectra of some objects. These photons are negatively polarized with respect to the continuum photons, showing that the broad absorption line region and the continuum scattering region are oriented perpendicular to each other.
\r\n\r\nThe polarization increases in the BAL troughs, due mainly to partial coverage of the central source by the broad absorption line region. Partial coverage of the continuum and broad emission line clouds leads to difficulties in determining the true optical depth of the BAL outflow. The geometry of the intervening BAL clouds is skewed with respect to the continuum scattering region, which results in position angle rotations in the BAL. The variation of polarization with velocity in the BAL is consistent with a non-radial, accelerating outflow of ionized gas. Our polarimetry observations are consistent with a model which unifies BAL QSO and non-BAL QSO. The BAL wind appears to occupy a narrow range of equatorial latitudes. When we view a QSO through this outflow, we see the characteristic troughs in BAL QSO.
\r\n", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-09232008-090917", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232008-090917", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-08", "doi": "10.7907/X967-5E39", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "advisor" }, { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "email": "bts@irastro.caltech.edu", "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" }, { "id": "Weymann-R-J", "name": { "family": "Weymann", "given": "Ray J." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-23", "thesis_defense_date": "1998-05-18", "thesis_approved_date": "2008-10-08", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Ogle, Patrick Michael" }, { "id": "/id/eprint/10402", "eprint_id": 10402, "rev_number": 19, "documents": [ { "id": "/id/document/82298", "doc_id": 82298, "rev_number": 3, "files": [ { "id": "/id/file/232498", "fileid": 232498, "datasetid": "document", "objectid": 82298, "filename": "Owen_BJ_1998.pdf", "mime_type": "application/pdf", "hash": "38fc877a0b1ad455ee0b2e80731be946", "hash_type": "MD5", "filesize": 62415783, "mtime": "2017-08-30 20:28:43", "url": "/10402/1/Owen_BJ_1998.pdf" } ], "eprint_id": 10402, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Owen_BJ_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 87, "dir": "disk0/00/01/04/02", "datestamp": "2017-08-30 21:04:41", "lastmod": "2021-04-16 23:24:45", "status_changed": "2017-08-30 21:04:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Owen-Benjamin-James", "name": { "family": "Owen", "given": "Benjamin James" } } ] }, "title": "Gravitational Waves from Compact Objects", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis addresses problems in the generation and detection of gravitational waves\r\nfrom two types of sources: inspiraling compact binaries and rapidly rotating young\r\nneutron stars.
\r\n\r\nChapters 2 and 3 estimate the computational costs of a basic matched filtering strategy to search for inspiraling compact binaries. Chapter 2 (written in 1995) sets up the machinery for calculating costs and makes a rough estimate based on the waveforms and noise spectra available at the time. It also systematizes previously published methods of choosing the filters. Chapter 3 (written with B. S. Sathyapra\u00ad kash in 1998) fine-tunes the machinery and updates the estimates of Chapter 2 using more current waveforms and noise spectra.
\r\n\r\nChapter 4 (written with Hideyuki Tagoshi and Akira Ohashi) concerns the post\u00ad Newtonian generation of gravitational waveforms from inspiraling compact binaries whose component objects spin about their own axes. It lays out a method of cal\u00ad culating post-Newtonian spin effects and calculates the lowest-order such effect not previously known (the second-post-Newtonian spin-orbit contribution to the wave\u00ad forms in the absence of precession).
\r\n\r\nChapters 5 and 6 concern the Chandrasekhar-Friedman-Schutz (CFS) gravita\u00adtional radiation instability as it applies to the \u03c4-modes of rapidly rotating young neutron stars. Chapter 5 (written with Lee Lindblom and Sharon M. Morsink) com\u00ad putes the viscous damping and gravitational radiation timescales of the \u03c4-modes and shows that viscosity does not suppress the CFS instability in hot young neutron stars. Chapter 6 (written with Lee Lindblom, Curt Cutler, Bernard F. Schutz, Alberto Vec\u00adchio, and Nils Andersson) computes approximate gravitational waveforms from young neutron stars spinning down due to the \u03c4-mode instability and estimates that these gravitational waves can be detected by the \"enhanced\" LIGO interferometers if a suitable data analysis strategy is developed.
", "date": "1998", "date_type": "degree", "id_number": "CaltechTHESIS:08302017-132619494", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08302017-132619494", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-30 21:04:41", "doi": "10.7907/63nf-9z58", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1998-05-12", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Owen, Benjamin James" }, { "id": "/id/eprint/3745", "eprint_id": 3745, "rev_number": 7, "documents": [ { "id": "/id/document/6362", "doc_id": 6362, "rev_number": 3, "files": [ { "id": "/id/file/38192", "fileid": 38192, "datasetid": "document", "objectid": 6362, "filename": "Bernstein_ra_1998.pdf", "mime_type": "application/pdf", "filesize": 13388741, "mtime": "2012-12-26 03:02:36", "url": "/3745/1/Bernstein_ra_1998.pdf" } ], "eprint_id": 3745, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Bernstein_ra_1998.pdf", "language": "en", "security": "public", "license": "other", "main": "Bernstein_ra_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22900" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22900" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22900" } ] } }, { "id": "/id/document/22900", "doc_id": 22900, "rev_number": 3, "files": [ { "id": "/id/file/38190", "fileid": 38190, "datasetid": "document", "objectid": 22900, "filename": "preview.png", "mime_type": "image/png", "hash": "94c1660f9549132083958208c27b111d", "hash_type": "MD5", "filesize": 11636, "mtime": "2012-12-26 03:02:35", "url": "/3745/2/preview.png" } ], "eprint_id": 3745, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6362" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6362" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6362" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/45", "datestamp": "2008-10-08", "lastmod": "2021-04-16 22:14:55", "status_changed": "2009-09-25 03:04:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bernstein-R-A", "name": { "family": "Bernstein", "given": "Rebecca A." }, "show_email": "NO" } ] }, "title": "The HST/LCO measurement of the mean flux of the extragalactic background light (3000-8000\u00c5)", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\n\r\nWe present the first detection of the optical extragalactic background light (EBL) at 3000, 5500, and 8000[...] using simultaneous observations taken from Hubble Space Telescope (HST) and the du Pont 2.5m telescope at Las Campanas Observatory (LCO). The total background flux of the night sky was measured from space using the Wide Field Planetary Camera 2 (WFPC2), thereby avoiding terrestrial airglow which is the dominant foreground component from the ground and the primary obstacle in previous efforts to measure the EBL. Foregrounds which contribute to the surface brightness of the night sky from HST are zodiacal light and diffuse galactic light. We have measured the absolute surface brightness of the zodiacal light using spectrophotometry taken with the du Pont 2.5m telescope at LCO and using the Faint Object Spectrograph (FOS) on HST. We minimize the contribution from diffuse galactic light by conducting the measurement in a target field with a low column density of galactic dust and neutral hydrogen, both of which are traced by 100\u03bc emission in the IRAS maps. The small remaining galactic contribution has been modeled using known correlations between the diffuse thermal emission from the dust at 100\u03bc and the diffuse optical light due to starlight scattered off the same dust. Because galaxies brighter than V = 23 AB mag are statistically poorly sampled in the WFPC2 field of view, we define the EBL as the total flux from objects fainter than V = 23 AB mag. We find the following mean levels for the EBL as a function of wavelength (in units of ergs s[superscript -1]cm[superscript -2]sr[superscript -1][...][superscript -1], with 1 \u03c3 rms errors): I\u03bb(3000[...])=4.0(\u00b11.9)x10[superscript -9], I\u03bb(5500[...])=2.8 (\u00b10.8)x10(superscript -9], I\u03bb(8000[...])=2.3 (\u00b10.6)x10[superscript -9], with systematic errors of 1-2x10[superscript -9] at each wavelength. The total flux detected at each wavelength is at least 2-3 times the integrated flux in published galaxy counts. The implications of this detection are discussed.\r\n", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-09242008-105539", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09242008-105539", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-08", "doi": "10.7907/4cy1-bw30", "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_committee": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "chair" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-24", "thesis_defense_date": "1997-10-28", "thesis_approved_date": "2008-10-08", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Bernstein, Rebecca A." }, { "id": "/id/eprint/3736", "eprint_id": 3736, "rev_number": 11, "documents": [ { "id": "/id/document/6352", "doc_id": 6352, "rev_number": 4, "files": [ { "id": "/id/file/38123", "fileid": 38123, "datasetid": "document", "objectid": 6352, "filename": "Wu_y_1998.pdf", "mime_type": "application/pdf", "filesize": 8367380, "mtime": "2012-12-26 03:02:32", "url": "/3736/1/Wu_y_1998.pdf" } ], "eprint_id": 3736, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Wu_y_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22890" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22890" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22890" } ] } }, { "id": "/id/document/22890", "doc_id": 22890, "rev_number": 3, "files": [ { "id": "/id/file/38121", "fileid": 38121, "datasetid": "document", "objectid": 22890, "filename": "preview.png", "mime_type": "image/png", "hash": "c80a3eff4a8c3cbc4eda2435a70310a1", "hash_type": "MD5", "filesize": 6681, "mtime": "2012-12-26 03:02:31", "url": "/3736/2/preview.png" } ], "eprint_id": 3736, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6352" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6352" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6352" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/36", "datestamp": "2008-10-08", "lastmod": "2023-01-18 22:55:04", "status_changed": "2009-09-25 03:04:25", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wu-Yanqin", "name": { "family": "Wu", "given": "Yanqin" }, "orcid": "0000-0003-0511-0893", "show_email": "NO" } ] }, "title": "Excitation and Saturation of White Dwarf Pulsation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Variable hydrogen white dwarfs (DAV) pulsate in a number of low-order gravity-modes with periods from 100 s to 1200 s and amplitudes no larger than a few percent. We answer two questions in this thesis: the driving for these pulsations, and the saturation of their amplitudes.
\r\n\r\nThe surface convection zone in these stars, which adjusts its entropy level instantaneously during the pulsation, can drive the observed modes. This mechanism (called 'convective driving') was discovered by Brickhill but has been largely neglected so far. We find that modes with periods shorter than the thermal adjustment time of the convection zone can become overstable, but those with very short periods are hardly visible at the surface. As the star cools and the convection zone deepens, longer period modes can be excited. The driving rates increase sharply with period. We relate these to the time-scale of mode variability. We include complications arising from nonadiabaticity in the radiative interior and turbulent damping at the convective-radiative boundary. The former limits the driving and damping rates for strongly nonadiabatic modes, and relates the phase and amplitude of surface horizontal velocity in a gravity-mode to those of its flux variation. The turbulent damping results from the horizontal velocity shear below the convection zone, inside which there is little velocity shear and negligible damping. This suppresses the amplitudes of long period modes to below detection. The width of the theoretical DAV instability strip is about 1000 K.
\r\n\r\nThe growth of an overstable mode can be saturated by parametric instability, where energy transfers resonantly into two damped modes of roughly half its frequency. This occurs above a critical amplitude which depends on the 3-mode coupling coefficient and the nonadiabatic damping rates. The critical amplitudes all fall below a few percent, with longer period modes having larger surface amplitudes. Combined with the amplitude limits due to turbulent damping, our estimates compare well with observations. Other types of mode couplings are needed to explain the observed 'mode selection'.
\r\n\r\nFinally, we show that the combination frequencies found in pulsation power spectra are produced by the time-varying convection zone which nonlinearly affects mode visibility.
", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-09232008-142919", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232008-142919", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-08", "doi": "10.7907/nc60-8v65", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Hoffmann-M-R", "name": { "family": "Hoffmann", "given": "Michael R." }, "orcid": "0000-0001-6495-1946", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Hoffmann-M-R", "name": { "family": "Hoffmann", "given": "Michael R." }, "orcid": "0000-0001-6495-1946", "role": "member" }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673", "role": "member" }, { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "member" }, { "id": "McCarthy-James-K", "name": { "family": "McCarthy", "given": "James K." }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-23", "thesis_defense_date": "1997-12-29", "thesis_approved_date": "2008-10-08", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Wu, Yanqin" }, { "id": "/id/eprint/3272", "eprint_id": 3272, "rev_number": 17, "documents": [ { "id": "/id/document/5775", "doc_id": 5775, "rev_number": 4, "files": [ { "id": "/id/file/34231", "fileid": 34231, "datasetid": "document", "objectid": 5775, "filename": "Koh_dt_1998.pdf", "mime_type": "application/pdf", "filesize": 7200302, "mtime": "2012-12-26 02:58:39", "url": "/3272/1/Koh_dt_1998.pdf" } ], "eprint_id": 3272, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Koh_dt_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22316" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22316" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22316" } ] } }, { "id": "/id/document/15329", "doc_id": 15329, "rev_number": 4, "files": [ { "id": "/id/file/204043", "fileid": 204043, "datasetid": "document", "objectid": 15329, "filename": "DannyKohpermission.txt", "mime_type": "text/plain", "filesize": 1832, "mtime": "2016-08-22 21:16:39", "url": "/3272/2/DannyKohpermission.txt" } ], "eprint_id": 3272, "pos": 2, "format": "text/plain", "format_desc": "author approval", "language": "en", "security": "internal", "license": "other", "main": "DannyKohpermission.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "metadata" }, { "id": "/id/document/22316", "doc_id": 22316, "rev_number": 2, "files": [ { "id": "/id/file/34229", "fileid": 34229, "datasetid": "document", "objectid": 22316, "filename": "preview.png", "mime_type": "image/png", "hash": "377bd67e1fba917d10a09e4cf3096ac0", "hash_type": "MD5", "filesize": 10636, "mtime": "2012-12-26 02:58:38", "url": "/3272/3/preview.png" } ], "eprint_id": 3272, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5775" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5775" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5775" } ] } }, { "id": "/id/document/123501", "doc_id": 123501, "rev_number": 1, "files": [ { "id": "/id/file/368916", "fileid": 368916, "datasetid": "document", "objectid": 123501, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "a87e15ead44f5784273709b25e646ebc", "hash_type": "MD5", "filesize": 920, "mtime": "2021-06-23 22:42:36", "url": "/3272/4/indexcodes.txt" } ], "eprint_id": 3272, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15329" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15329" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15329" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/72", "datestamp": "2008-09-10", "lastmod": "2021-10-26 18:54:15", "status_changed": "2009-09-25 02:55:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Koh-Danny-Towsian", "name": { "family": "Koh", "given": "Danny Towsian" }, "show_email": "NO" } ] }, "title": "Continuous Long Term Observations of Accreting Pulsars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "The all-sky monitoring ability of the BATSE instrument on the GRO has enabled the first uniform, continuous and long term observations of the torque and fluxes of many known accreting pulsars. In the first part of this thesis, I describe the capabilities of BATSE for detecting hard X-rays, the techniques developed to perform timing and flux measurements, and the steps involved in reducing the raw data sets to a standardized database of data products for each accreting pulsar monitored by BATSE.
\r\n\r\nIn the second part of this thesis, I describe several studies performed with this database. The first is a broad overview of all the accreting pulsars monitored by BATSE. For each source, I display the frequency and pulsed flux histories from \u2248 five years of BATSE observations, and provide a brief summary of the BATSE findings.
\r\n\r\nI then focus on the wind-fed accreting pulsar GX 301-2. The most striking features in the pulsar frequency history are two steady and rapid spin-up episodes, with v [over-dot] \u2248 (3-5) x 10\u207b\u00b9\u00b2 Hz s\u207b\u00b9, each lasting for about 30 days. They probably represent the formation of transient accretion disks in this wind-fed pulsar. Except for these spin-up episodes, there are virtually no net changes in the neutron star spin frequency on long time scales. We suggest that the long-term spin-up trend observed since 1984 (v [over-dot] \u2248 2 x 10\u207b\u00b9\u00b3 Hz s\u207b\u00b9) may be due entirely to brief (\u2248 20 d) spin-up episodes similar to those we have discovered.
\r\n\r\nNext, I highlight the most significant trends revealed by the BATSE observations and discuss their implications for our current understanding of the spin-evolution and torque-luminosity relations in accreting pulsars. Alternating episodes of steady spin-up and spin-down were found to be a surprisingly common characteristic of many persistent sources. Pulsed flux and accretion torque are strongly correlated in outbursts of transient accreting pulsars, but uncorrelated, or even anticorrelated, in persistent sources. I describe the various competing models that currently exist and critically assess each model within the context of the BATSE observations.
\r\n\r\nFinally, I describe how BATSE observations of the recurrence rate of transient systems can be used to infer the galactic population of high-mass Be-transient systems.
", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-08292008-082313", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08292008-082313", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/ch1h-0w87", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "chair" }, { "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-29", "thesis_defense_date": "1997-07-11", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Koh, Danny Towsian" }, { "id": "/id/eprint/3142", "eprint_id": 3142, "rev_number": 11, "documents": [ { "id": "/id/document/5587", "doc_id": 5587, "rev_number": 2, "files": [ { "id": "/id/file/33003", "fileid": 33003, "datasetid": "document", "objectid": 5587, "filename": "Leitch_em_1998.pdf", "mime_type": "application/pdf", "filesize": 9750136, "mtime": "2012-12-26 02:57:25", "url": "/3142/1/Leitch_em_1998.pdf" } ], "eprint_id": 3142, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Leitch_em_1998.pdf", "language": "en", "security": "public", "license": "other", "main": "Leitch_em_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22130" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22130" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22130" } ] } }, { "id": "/id/document/16152", "doc_id": 16152, "rev_number": 3, "files": [ { "id": "/id/file/203995", "fileid": 203995, "datasetid": "document", "objectid": 16152, "filename": "Leitch_Erik_M_1998.txt", "mime_type": "text/plain", "filesize": 1729, "mtime": "2016-08-22 21:16:33", "url": "/3142/2/Leitch_Erik_M_1998.txt" } ], "eprint_id": 3142, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Leitch_Erik_M_1998.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/22130", "doc_id": 22130, "rev_number": 2, "files": [ { "id": "/id/file/33001", "fileid": 33001, "datasetid": "document", "objectid": 22130, "filename": "preview.png", "mime_type": "image/png", "hash": "cf840ce7735e1b098ee1764016a2ffc4", "hash_type": "MD5", "filesize": 12903, "mtime": "2012-12-26 02:57:25", "url": "/3142/3/preview.png" } ], "eprint_id": 3142, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5587" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5587" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5587" } ] } }, { "id": "/id/document/123392", "doc_id": 123392, "rev_number": 1, "files": [ { "id": "/id/file/368804", "fileid": 368804, "datasetid": "document", "objectid": 123392, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "8ced33defff6a4ea4f2df2505c07ff71", "hash_type": "MD5", "filesize": 794, "mtime": "2021-06-23 22:37:22", "url": "/3142/4/indexcodes.txt" } ], "eprint_id": 3142, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16152" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16152" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16152" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/42", "datestamp": "2006-08-25", "lastmod": "2021-11-05 22:40:33", "status_changed": "2009-09-25 02:52:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "eml@astro.caltech.edu", "id": "Leitch-Erik-M", "name": { "family": "Leitch", "given": "Erik M." }, "show_email": "YES" } ] }, "title": "A measurement of anisotropy in the microwave background on 7'-22' scales", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nA measurement of the anisotropy of the cosmic microwave background radiation (CMBR) at 7'-22' scales is described. Observations of 36 blank fields near the North Celestial Pole (NCP) were made at 31.7 and 14.5 GHz, using two High Electron Mobility Transistor (HEMT) amplified radiometers. These observations were conducted at the Owens Valley Radio Observatory from 1993-1996.\r\n\r\nWe detect a significant signal, with temperature spectral index consistent with emission from a combination of a steep-spectrum foreground ([beta] < -2) and CMBR ([...]). Multi-epoch VLA observations at 8 and 15 GHz allow removal of any discrete source contamination at 14.5 and 31.7 GHz. On the basis of low-frequency maps of the NCP, we can rule out emission with [beta] < -2.2. Although the foreground signal dominates at 14.5 GHz, the extracted CMBR component contributes nearly 90% of the variance at 31.7 GHz, yielding an rms fluctuation amplitude of [...], including calibration uncertainty and sample variance. In terms of the angular power spectrum [...] averaged over a range of multipoles [...], we have [...].\r\n\r\nThe extracted foreground component is found to correlate significantly with IRAS 100 [mu] m dust emission. Lack of H [alpha] emission near the NCP suggests that the foreground is either high-temperature thermal bremsstrahlung [...], flat spectrum synchrotron, or an exotic component of dust emission.\r\n", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-08162006-081019", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08162006-081019", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-08-25", "doi": "10.7907/DRVA-T966", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-08-16", "thesis_defense_date": "1998-03-04", "thesis_approved_date": "2006-08-25", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Leitch, Erik M." }, { "id": "/id/eprint/1453", "eprint_id": 1453, "rev_number": 12, "documents": [ { "id": "/id/document/2214", "doc_id": 2214, "rev_number": 2, "files": [ { "id": "/id/file/13806", "fileid": 13806, "datasetid": "document", "objectid": 2214, "filename": "pahre-thesis-double.pdf", "mime_type": "application/pdf", "filesize": 6320571, "mtime": "2012-12-26 02:38:14", "url": "/1453/1/pahre-thesis-double.pdf" } ], "eprint_id": 1453, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "pahre-thesis-double.pdf", "language": "en", "security": "public", "license": "other", "main": "pahre-thesis-double.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2214" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2214" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2214" } ] } }, { "id": "/id/document/120768", "doc_id": 120768, "rev_number": 1, "files": [ { "id": "/id/file/366156", "fileid": 366156, "datasetid": "document", "objectid": 120768, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "7537b20ac56b1bba079939f564da13f3", "hash_type": "MD5", "filesize": 998, "mtime": "2021-06-23 21:05:06", "url": "/1453/8/indexcodes.txt" } ], "eprint_id": 1453, "pos": 8, "placement": 8, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16353" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16353" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16353" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/14/53", "datestamp": "2005-04-22", "lastmod": "2020-12-18 01:53:22", "status_changed": "2009-09-25 02:04:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mpahre@cfa.harvard.edu", "id": "Pahre-M-A", "name": { "family": "Pahre", "given": "Michael Andrew" }, "show_email": "YES" } ] }, "title": "Elliptical galaxies : structure, stellar content, and evolution", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nA near-infrared imaging survey of 341 nearby early-type galaxies, combined with optical imaging and spectroscopic data from the literature, are used to construct the global scaling relations for this population of galaxies. These data demonstrate a number of important features of the early-type galaxy sequence: (1) the slope of the Fundamental Plane (FP) correlations systematically increases with wavelength; (2) the slope of these FP correlations deviates from the virial expectation at all wavelengths, implying a breakdown of either or both of the assumptions of constant mass-to-light ratio and homology; (3) the intrinsic scatter of the FP correlations is small but resolved at all wavelengths, implying a small cosmic scatter of early-type galaxy properties at any position in the galaxy sequence and contradicting any model in which various stellar populations parameters \"conspire\" with each other to keep the correlations thin at optical wavelengths; (4) there is no correlation among residuals of the metallicity-independent near-infrared FP and the metallicity-sensitive [...] relation, implying that both age and metallicity variations contribute to the cosmic scatter of both correlations; and (5) the effective radii systematically decrease with increasing wavelength, fully consistent with the general presence of stellar populations gradients in early-type galaxies. A comprehensive and self-consistent model is described which simultaneously explains these and other global properties of the early-type galaxy sequence. This model demonstrates that age, metallicity, deviations from a dynamically homologous family, and populations gradients are all contributing to the form of the global scaling relations; the latter two effects are the least constrained by the observations and model, respectively.\r\n\r\nAdditional constraints on the role of age in the global scaling relations is obtained by observing early-type galaxies at higher redshifts. This has been studied using three approaches: color evolution, evolution of the slope and intercept of the K-band FP correlations, and evolution of the absorption line strengths. The galaxies in each cluster are identified in a systematic way using two color (three bandpass) imaging--sampling approximately the U, V, and I bandpasses in the rest frame--to eliminate late-type cluster member and general field interloper galaxies. This method is > 90% effective in identifying early-type galaxies at the target cluster redshift.\r\n\r\nWeak color evolution in rest-frame (U - V)[...] has been detected in 26 rich clusters of galaxies. The bluing trend in color is 0.05[...]0.03 mag at z = 0.2, 0.12+0.04 mag at z = 0.4, and ~0.23 [...] 0.05 mag at z = 0.54. Using stellar population synthesis models from the literature, this color evolution is fully consistent with the galaxy population as a whole having formed at 1 < [...] < 5.\r\n\r\nThe FP correlations are studied for 128 galaxies in eight rich clusters at 0.1 < z < 0.6 using moderate dispersion spectroscopy (110 of the measurements are new) and imaging in the near-infrared K-band. These data more than quadruple the data in the literature which can be used to study the FP at high redshift. The near-infrared FP is constructed at high redshifts for the first time. The intercept of the FP on the surface brightness axis is observed to dim with redshift, as expected for the Tolman signal in an expanding world model. A small amount of luminosity evolution [Delta]K [...] 2.5 log(1+z) mag is detected on top of the Tolman signal, which is consistent with the passive evolution of a stellar population that formed at high redshift. The slope of the near-infrared FP is observed to flatten with redshift, implying that the least luminous galaxies are evolving faster than the luminous galaxies. This is strong evidence that low luminosity ellipticals have a stellar content that is up to a factor of two times younger than high luminosity ellipticals, but age spreads much larger than this appear to be excluded, and age spreads somewhat smaller than this are still allowed depending on the choice of nearby galaxy sample used in the comparison.\r\n\r\nThe absorption line strengths of the galaxies are observed to evolve slowly with redshift: the Mg2 and (Fe) indices weaken while the H[Beta]G index strengthens. The latter effect in particular is another strong indication that the mean age of the stellar populations in early-type galaxies formed at redshifts 3 < [...] < 5. All of these properties are moderately consistent with the models derived above based on the samples of nearby galaxies, implying that age is an important physical parameter underlying the global scaling relations for early-type galaxies.", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-04222005-133013", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04222005-133013", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-04-22", "doi": "10.7907/PQ71-9E96", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "george@astro.caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "chair" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew E." }, "role": "member" }, { "id": "Steidel-C-C", "name": { "family": "Steidel", "given": "Charles C." }, "role": "member" }, { "id": "Persson-Eric", "name": { "family": "Persson", "given": "Eric" }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Shectman-S-A", "name": { "family": "Shectman", "given": "Stephen Alan" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-04-22", "thesis_defense_date": "1998-02-03", "thesis_approved_date": "2005-04-22", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Pahre, Michael Andrew" }, { "id": "/id/eprint/3734", "eprint_id": 3734, "rev_number": 7, "documents": [ { "id": "/id/document/6350", "doc_id": 6350, "rev_number": 3, "files": [ { "id": "/id/file/38109", "fileid": 38109, "datasetid": "document", "objectid": 6350, "filename": "Lyutikov_m_1998.pdf", "mime_type": "application/pdf", "filesize": 8871978, "mtime": "2012-12-26 03:02:31", "url": "/3734/1/Lyutikov_m_1998.pdf" } ], "eprint_id": 3734, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Lyutikov_m_1998.pdf", "language": "en", "security": "public", "license": "other", "main": "Lyutikov_m_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22888" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22888" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22888" } ] } }, { "id": "/id/document/22888", "doc_id": 22888, "rev_number": 3, "files": [ { "id": "/id/file/38107", "fileid": 38107, "datasetid": "document", "objectid": 22888, "filename": "preview.png", "mime_type": "image/png", "hash": "199a47cbef13ef02d0040e29db898f9b", "hash_type": "MD5", "filesize": 13922, "mtime": "2012-12-26 03:02:31", "url": "/3734/2/preview.png" } ], "eprint_id": 3734, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6350" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6350" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6350" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/34", "datestamp": "2008-10-30", "lastmod": "2021-04-16 23:04:46", "status_changed": "2009-09-25 03:04:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lyutikov-M", "name": { "family": "Lyutikov", "given": "Maxim" }, "show_email": "NO" } ] }, "title": "Coherent emission mechanisms in radio pulsars", "ispublished": "unpub", "full_text_status": "public", "abstract": "In this work we investigate some possible mechanisms for pulsar radio emission. First we analyze the normal modes of a strongly magnetized electron-positron plasma taking into account a possible difference in the distribution functions of electrons and positrons. The dispersion relations, polarization properties and various regimes of beam instabilities in pair plasma are considered. We argue that kinetic instabilities of electromagnetic modes are more promising candidates for the pulsar radio emission mechanism than electrostatic instabilities (which occur in the hydrodynamic regime). We elucidate the microphysical processes underlying cyclotron-Cherenkov and Cherenkov-drift emission, stressing the importance of collective plasma effects involving all the particles of a medium. We show that cyclotron-Cherenkov emission at the anomalous Doppler effect can account for various observed phenomena of the \"core\" emission. Cherenkov-drift emission is a likely candidate for the \"cone\" emission.\r\n\r\nWe developed a new description that treats Cherenkov-drift emission in cylindrical coordinates. This approach describes consistently the resonant wave-particle interaction and provides a link between the Cherenkov, curvature and drift emission mechanisms recovering them as a limiting cases of the Cherenkov-drift emission process.\r\n\r\nWe also consider two possible nonlinear stages of the development of the cyclotron-Cherenkov instability: quasilinear diffusion and induced Raman scattering. We calculate the asymptotic particle distribution and emerging spectra for the cyclotron-Cherenkov instability and also show that induced Raman scattering may be important for the wave propagation and nonlinear saturation of electromagnetic instabilities. Finally, we considered the escape of waves from a pulsar magnetosphere taking into account cyclotron, Cherenkov and Cherenkov-drift absorption processes.\r\n", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-09232008-092435", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232008-092435", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-30", "doi": "10.7907/3y39-fz45", "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_committee": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "chair" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-23", "thesis_defense_date": "1998-03-11", "thesis_approved_date": "2008-10-30", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Lyutikov, Maxim" }, { "id": "/id/eprint/10403", "eprint_id": 10403, "rev_number": 18, "documents": [ { "id": "/id/document/82306", "doc_id": 82306, "rev_number": 3, "files": [ { "id": "/id/file/232533", "fileid": 232533, "datasetid": "document", "objectid": 82306, "filename": "Hughes_SA_1998.pdf", "mime_type": "application/pdf", "hash": "eb56593883af7ae84727f91ad81904c3", "hash_type": "MD5", "filesize": 111910413, "mtime": "2017-08-30 21:05:32", "url": "/10403/1/Hughes_SA_1998.pdf" } ], "eprint_id": 10403, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Hughes_SA_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"archive", "userid": 87, "dir": "disk0/00/01/04/03", "datestamp": "2017-08-30 21:26:27", "lastmod": "2021-04-16 23:19:55", "status_changed": "2017-08-30 21:26:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hughes-Scott-Alexander", "name": { "family": "Hughes", "given": "Scott Alexander" } } ] }, "title": "Gravitational-Wave Astronomy: Aspects of the Theory of Binary Sources and Interferometric Detectors", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis presents a study of several problems and issues in the nascent field of gravitational-wave astronomy. Multi-kilometer baseline interferometers are being built in the United States [the LIGO (Laser Interferometer Gravitational-wave Observatory) project] and similar projects are underway in Europe (the VIRGO and GE0600 projects) and Japan (the TAMA300 project). LIGO will begin operations very soon (the first science run is scheduled for 2002), and detectors in other countries will begin soon as well. We are thus about 5 years from using gravitational waves as a new window to probe astrophysical processes in the universe.
\r\n\r\n\r\nChapters 2, 3, and 4 of this thesis study gravitational waves from coalescences of compact bi\u00adnaries. Chapters 2 and 3 are a detailed examination, in collaboration with \u00c9anna \u00c9. Flanagan, of binary black hole (BBH) coalescences. The birth rate of BBH systems in the universe is highly uncertain, so it is not immediately apparent how relevant they are to gravitational-wave astronomy. If such systems do in fact exist, we find that they will be visible to extremely large distances, far greater than the distances to which binary neutron star systems, for example, will be visible. This heightened visibility may compensate for the possible dearth of such binaries, making them an ex\u00adtremely important and interesting source. We suggest ways in which numerical modeling of BBHs may aid gravitational-wave data analysis, and techniques that can be used in BBH event searches and waveform analysis. Chapter 4 analyzes the measurement of gravitational waves from the final merger of binary neutron star systems. Such waves depend on details of the composition of neutron stars, such as their equation of state, and may be driven by hydrodynamic and nuclear processes that occur in the final merger. Unfortunately, these waves are emitted at high frequencies where LIGO\u00ad type detectors have poor sensitivity. Measuring such waves will require specialty \"narrow-band\" detectors. In this chapter, I present an algorithm for optimally configuring a network of multiple LIGO-type and narrow-band detectors to measure these merger waves. I find that improved \r\ntheoret\u00adical modeling of the final merger will play an important role in designing such networks and in the analysis of their data. In Chapter 5, in collaboration with Patrick R. Brady, I analyze the stability of binary neutron star systems as they coalesce. Some rather controversial numerical calculations have found that neutron stars in binary systems are rendered unstable by their companion, and may collapse into black holes long before their final merger. This would have a huge impact on the gravitational waves such systems emit. The claimed effect is first-order in a particular expansion. Motivated by this claim, Brady and I perform a first-order expansion of the fluid and field equations of general relativity, in the limit in which one star is much smaller than the other. We find that no such effect can exist. Finally, Chapter 6 is an analysis, in collaboration with Kip S. Thorne, of seismic gravity-gradient noise, a noise source that may be of concern to future detector designs. This noise source arises from fluctuations in the density of the earth near and below a LIGO-type interferometer's test masses. It is gravitational in origin, and thus cannot be shielded. By carefully studying the geological structures in the earth near the two LIGO sites, considering the propagation of elastodynamic waves in such structures, and computing the gravitational fluctuations such waves cause, we find seismic gravity-gradient noise is likely to become unavoidable at frequencies below roughly 5 Hertz. This has strong implications on plans to improve the low frequency sensitivity of the LIGO detectors.
\r\n \r\n\r\n\r\n\r\n", "date": "1998", "date_type": "degree", "id_number": "CaltechTHESIS:08302017-134937434", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08302017-134937434", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-9220644" }, { "agency": "NSF", "grant_number": "PHY-9408378" }, { "agency": "NSF", "grant_number": "PHY-9424337" }, { "agency": "NSF", "grant_number": "PHY-9514726" }, { "agency": "NSF", "grant_number": "AST-9417371" }, { "agency": "NASA", "grant_number": "NAGW-4628" }, { "agency": "NASA", "grant_number": "NAGW-2897" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-30 21:26:27", "doi": "10.7907/smxp-aw47", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1998-05-11", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Hughes, Scott Alexander" }, { "id": "/id/eprint/3602", "eprint_id": 3602, "rev_number": 14, "documents": [ { "id": "/id/document/6174", "doc_id": 6174, "rev_number": 3, "files": [ { "id": "/id/file/36943", "fileid": 36943, "datasetid": "document", "objectid": 6174, "filename": "Gizis_je_1998.pdf", "mime_type": "application/pdf", "filesize": 6041961, "mtime": "2012-12-26 03:01:16", "url": "/3602/1/Gizis_je_1998.pdf" } ], "eprint_id": 3602, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Gizis_je_1998.pdf", "language": "en", "security": "public", "license": "other", "main": "Gizis_je_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22712" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22712" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22712" } ] } }, { "id": "/id/document/22712", "doc_id": 22712, "rev_number": 3, "files": [ { "id": "/id/file/36941", "fileid": 36941, "datasetid": "document", "objectid": 22712, "filename": "preview.png", "mime_type": "image/png", "hash": "0968e7e8a372470439d4397db29beaa5", "hash_type": "MD5", "filesize": 9029, "mtime": "2012-12-26 03:01:15", "url": "/3602/2/preview.png" } ], "eprint_id": 3602, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6174" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6174" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6174" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/36/02", "datestamp": "2008-10-30", "lastmod": "2023-01-18 22:49:11", "status_changed": "2009-09-25 03:01:29", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gizis-John-Evangelos", "name": { "family": "Gizis", "given": "John Evangelos" }, "show_email": "NO" } ] }, "title": "M Subdwarfs and the Population II Luminosity Function", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nWe present a spectroscopic classification system for M-dwarfs and M-subdwarfs based on quantitative measures of TiO and CaH features in the region \u03bb\u03bb06200-7400[...]. Our sample of cool stars covers the range from solar metallicity stars to the most extreme subdwarfs known. Using synthetic spectra computed by Allard and Hauschildt (1995), we derive metallicities for the stars. Stars are classified as dwarfs (M V), subdwarfs (sdM), or extreme subdwarfs (esdM). These classifications correspond to [m/H] \u2248 0.0, -1.2, and -2.0 respectively. Our metallicity scale agrees with theoretical HR diagrams and HST globular cluster measurements. We discuss some nearby subdwarfs of particular interest in light of our metallicity scale.
\r\n\r\nWe present spectra of three M subdwarfs which are common proper motion companions to F or G subdwarfs of known metallicity. The assumption that the companions have the same composition allows us to test the Gizis (1997, AJ, 113, 806) M subdwarf classification system and its correspondence to metallicity. The results are in excellent agreement with the Gizis (1997) scale, thereby showing that the Allard Hauschildt (1995, ApJ, 445, 433) Extended model atmospheres agree well in the 6200 - 7400[...] region for cool metal-poor stars. We also show that the results are consistent with the main sequences of globular clusters using the Reid (1997, AJ, in press) distance scale.
\r\n\r\nWe use optical spectra as well as optical and infrared broadband photometry to constrain the effective temperatures of M subdwarfs. We show that the coolest subdwarfs known have T[subscript eff] \u2248 3000 K.
\r\n\r\nWe present spectroscopic observations of two halo M subdwarfs which have H\u03b1 emission lines. We show that in both cases close companions are the likely cause of the chromospheric activity in these old, metal-poor stars. We argue that GI 781 A's unseen companion is most likely a cool helium white dwarf. GI 455 is a near-equalmass M subdwarf system. G1 781 A is rapidly rotating with v sin i \u2248 30 km s[superscript -1]. The properties of the chromosphere and X-ray coronae of these systems are compared to M dwarfs with emission (dMe). Although the relative strength of the X-ray coronae to the H\u03b1 emission are similar to that seen in field and young cluster dMe, G1 781 A's activity level is weaker than the young cluster dMe. This suggests that different ages and/or metallicities can make two otherwise equally rapidly rotating, equal-mass stars have different activity levels.
\r\n\r\nUsing a proper motion survey based upon the two Palomar Sky Surveys, We measure the luminosity function of the low-mass end of the field Population II. We combine this with earlier measurements of higher mass stars to show that the luminosity function increases down to M[subscript I] \u2248 9.5, but may be flattening at the lowest luminosities M[subscript I] > 9.5. We discuss the constraints this puts on the mass function of metal-poor stars. The mass function is consistent with a power-law of slope \u03b1 \u2248 -1.35.
", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-152836", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-152836", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-30", "doi": "10.7907/pfke-c379", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Reid-N", "name": { "family": "Reid", "given": "Neill" }, "role": "advisor" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "id": "Reid-N", "name": { "family": "Reid", "given": "Neill" }, "role": "chair" }, { "id": "McCarthy-James-K", "name": { "family": "McCarthy", "given": "James K." }, "role": "member" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" }, { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "1997-10-17", "thesis_approved_date": "2008-10-30", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Gizis, John Evangelos" }, { "id": "/id/eprint/5338", "eprint_id": 5338, "rev_number": 27, "documents": [ { "id": "/id/document/8728", "doc_id": 8728, "rev_number": 5, "files": [ { "id": "/id/file/54165", "fileid": 54165, "datasetid": "document", "objectid": 8728, "filename": "Mahajan_s_1998.pdf", "mime_type": "application/pdf", "filesize": 8955378, "mtime": "2012-12-26 03:18:34", "url": "/5338/1/Mahajan_s_1998.pdf" } ], "eprint_id": 5338, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Mahajan_s_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": 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"mtime": "2021-06-24 00:08:07", "url": "/5338/9/indexcodes.txt" } ], "eprint_id": 5338, "pos": 9, "placement": 9, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/103371" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/103371" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/103371" } ] } } ], "eprint_status": "archive", "userid": 51, "dir": "disk0/00/00/53/38", "datestamp": "2009-11-17 23:57:06", "lastmod": "2020-03-10 23:05:33", "status_changed": "2009-11-17 23:57:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "sanjoy@mit.edu", "id": "Mahajan-Sanjoy-Sondhi", "name": { "family": "Mahajan", "given": "Sanjoy Sondhi" }, "show_email": "YES" } ] }, "title": "Order of Magnitude Physics: A Textbook with Applications to the Retinal Rod and the Density of Prime Numbers", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics ; approximation, back of the envelope", "note": "From author: [Thesis] eventually became a textbook, which is also freely available from MIT Press (CC-BY-NC-SA): \"The Art of Insight in Science and Engineering: Mastering Complexity\" (MIT Press, 2014).", "abstract": "I develop tools to amplify our mental senses: our intuition and reasoning abilities. The first five chapters\u2014based on the Order of Magnitude Physics class taught at Caltech by Peter Goldreich and Sterl Phinney\u2014form part of a textbook on dimensional analysis, approximation, and physical reasoning. The text is a resource of intuitions, problem-solving methods, and physical interpretations. By avoiding mathematical complexity, order-of-magnitude techniques increase our physical understanding, and allow us to study otherwise difficult or intractable problems. The textbook covers: (1) simple estimations, (2) dimensional analysis, (3) mechanical properties of materials, (4) thermal properties of materials, and (5) water waves.
\r\n\r\nAs an extended example of order-of-magnitude methods, I construct an analytic model for the flash sensitivity of a retinal rod. This model extends the flash-response model of Lamb and Pugh with an approximate model for steady-state response as a function of background light Ib. The combined model predicts that the flash sensitivity is proportional to Ib-1.3. This result roughly agrees with experimental data, which show that the flash sensitivity follows the Weber-Fechner behavior of Ib-1 over an intensity range of 100. Because the model is simple, it shows clearly how each biochemical pathway determines the rod's response.
\r\n\r\nThe second example is an approximate model of primality, the square-root model. Its goal is to explain features of the density of primes. In this model, which is related to the Hawkins' random sieve, divisibility and primality are probabilistic. The model implies a recurrence for the probability that a number n is prime. The asymptotic solution to the recurrence is (log n)-1, in agreement with the prime-number theorem. The next term in the solution oscillates around (log n)-1 with a period that grows superexponentially. These oscillations are a model for oscillations in the density of actual primes first demonstrated by Littlewood, who showed that the number of primes \u2264 n crosses its natural approximator, the logarithmic integral, infinitely often. No explicit crossing is known; the best theorem, due to to Riele, says that the first crossing happens below 7 x 10370. A consequence of the square-root model is the conjecture that the first crossing is near 1027.
\r\n", "date": "1998", "date_type": "degree", "id_number": "CaltechTHESIS:10302009-110303489", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10302009-110303489", "related_url": { "items": [ { "description": "Thesis became a textbook", "type": "pub", "url": "https://mitpress.mit.edu/books/art-insight-science-and-engineering" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Tony Diaz", "deposited_on": "2009-11-17 23:57:06", "doi": "10.7907/8MJZ-A984", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "chair" }, { "id": "Frautschi-S-C", "name": { "family": "Frautschi", "given": "Steven C." }, "role": "member" }, { "id": "Hopfield-J-J", "name": { "family": "Hopfield", "given": "John J." }, "role": "member" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Mead-C", "name": { "family": "Mead", "given": "Carver" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1998-05-19", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Mahajan, Sanjoy Sondhi" }, { "id": "/id/eprint/7447", "eprint_id": 7447, "rev_number": 18, "documents": [ { "id": "/id/document/35070", "doc_id": 35070, "rev_number": 3, "files": [ { "id": "/id/file/110981", "fileid": 110981, "datasetid": "document", "objectid": 35070, "filename": "Vasavada_ar_1998.pdf", "mime_type": "application/pdf", "hash": "49c2a1e4c2d1571e909b1e8ea6790203", "hash_type": "MD5", "filesize": 17515409, "mtime": "2013-01-28 16:40:05", "url": "/7447/1/Vasavada_ar_1998.pdf" } ], "eprint_id": 7447, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Vasavada_ar_1998.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"dir": "disk0/00/00/74/47", "datestamp": "2013-01-28 17:07:40", "lastmod": "2021-04-16 22:21:48", "status_changed": "2013-01-28 17:07:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vasavada-Ashwin-R", "name": { "family": "Vasavada", "given": "Ashwin R." }, "orcid": "0000-0003-2665-286X", "show_email": "NO" } ] }, "title": "I. Temperatures of polar ice deposits on mercury and the moon. II. Jovian atmospheric dynamics from Galileo imaging", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Electrical Engineering", "abstract": "Locations on Mercury that produce ice-like radar responses lie within\r\nimpact craters that have very cold, permanently shaded floors. The retention of\r\npossible ice deposits is determined largely by their temperature. We present model-\r\ncalculated temperatures of flat surfaces and surfaces within bowl-shaped and flatfloored\r\npolar impact craters. Our model includes appropriate insolation cycles,\r\nrealistic crater shapes, multiple scattering of sunlight and infrared radiation, and\r\ndepth and temperature-dependent regolith thermophysical properties. Unshaded\r\nwater ice deposits are rapidly lost to sublimation on Mercury and the Moon.\r\nMeter-thick deposits of water ice are stable to evaporation over the age of the\r\nsolar system if located in the permanently shaded portions of flat-floored craters\r\nwithin 10\u00b0 latitude of the poles of either planet. Results for craters associated with\r\nradar features on Mercury are consistent with stable water ice deposits if a thin\r\nregolith layer thermally insulates the lowest latitude deposits, reducing sublimation\r\nrates. A regolith cover also is a diffusion barrier, reduces losses from sputtering,\r\nimpact vaporization, and exposure to H Ly\u03b1, and is implied independently by the\r\nradar observations. Impact craters near the lunar poles contain colder permanently\r\nshaded regions than those on Mercury.
\r\n\r\nDuring the first six orbits of the Galilee spacecraft's prime mission, the\r\nSolid State Imaging system acquired multispectral image mosaics of Jupiter's\r\nGreat Red Spot, an equatorial belt/zone boundary, a \"5-\u00b5m hotspot\" similar to the\r\nGalilee Probe entry site, and two of the classic White Ovals. We present mosaics\r\nof each region approximating their appearance at visible wavelengths and showing\r\ncloud height and opacity variations. The local wind field is derived by tracking\r\ncloud motions between multiple observations of each region with time separations\r\nof roughly one and ten hours. Vertical cloud structure is derived in a companion\r\npaper by Banfield et al.(1998). Galilee's brief, high-resolution observations\r\ncomplement Earth-based and Voyager studies, and offer local meteorological\r\ncontext for the Galileo Probe results. Images taken one hour apart reveal small,\r\nrapidly changing, high cloud features possibly analogous to terrestrial\r\nthunderstorms. Our results show that the dynamics of the zonal jets and large\r\nvortices have changed little since Voyager, with a few exceptions. We detect a\r\ncyclonic current within the center of the predominantly anticyclonic Great Red\r\nSpot. The zonal velocity difference between 0\u00b0s and 6\u00b0S has increased by 20 m s^(-1).\r\nWe measure a strong northeast flow approaching the hotspot. This flow indicates\r\neither massive horizontal convergence or the presence of a large anticyclonic\r\nvortex southeast of the hotspot. The current compact arrangement of two White\r\nOvals and a cyclonic structure greatly perturbs the zonal jets in that region.
", "date": "1998", "date_type": "degree", "id_number": "CaltechTHESIS:01282013-083854060", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01282013-083854060", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2013-01-28 17:07:40", "doi": "10.7907/ps1y-d710", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1998-05-18", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "eleceng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1998", "author_list": "Vasavada, Ashwin R." }, { "id": "/id/eprint/1918", "eprint_id": 1918, "rev_number": 8, "documents": [ { "id": "/id/document/3303", "doc_id": 3303, "rev_number": 3, "files": [ { "id": "/id/file/19689", "fileid": 19689, "datasetid": "document", "objectid": 3303, "filename": "Hunter_tr_1997.pdf", "mime_type": "application/pdf", "filesize": 12791094, "mtime": "2012-12-26 02:44:10", "url": "/1918/1/Hunter_tr_1997.pdf" } ], "eprint_id": 1918, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Hunter_tr_1997.pdf", "language": "en", "security": "public", "license": "other", "main": "Hunter_tr_1997.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19994" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19994" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19994" } ] } }, { "id": "/id/document/19994", "doc_id": 19994, "rev_number": 3, "files": [ { "id": "/id/file/19687", "fileid": 19687, "datasetid": "document", "objectid": 19994, "filename": "preview.png", "mime_type": "image/png", "hash": "8a849740c3f0a4df87a6f2d7bb9d5bd6", "hash_type": "MD5", "filesize": 11778, "mtime": "2012-12-26 02:44:10", "url": "/1918/2/preview.png" } ], "eprint_id": 1918, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3303" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3303" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3303" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/19/18", "datestamp": "2007-05-24", "lastmod": "2021-04-16 23:18:21", "status_changed": "2009-09-25 02:19:51", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hunter-T-R", "name": { "family": "Hunter", "given": "Todd Russell" }, "show_email": "NO" } ] }, "title": "A submillimeter imaging survey of ultracompact HII regions", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThis research explores the process of massive star formation in the Galaxy through submillimeter continuum and spectral line observations of ultracompact HII (UCHII) regions. First, I describe the design and operation of the Submillimeter High Angular Resolution Camera (SHARC)-a 24-pixel bolometer array camera for broadband continuum imaging at 350 and 450\u00b5m at the Caltech Submillimeter Observatory (CSO). Detailed information is included on the reflective off-axis optical design and the instrument control software interface. Second, I present 10\" to 12\" resolution SHARC images of 350 and 450\u00b5m continuum emission from a sample of 17 UCHII regions with different radio morphologies. Although the dust emission typically peaks at or near the UCHII region, additional sources are often present, sometimes coincident with the position of H2O masers. The combination of submillimeter, millimeter and IRAS far-infrared flux densities forms the basis of greybody models of the spectral energy distributions. The average dust temperature is 40 \u00b1 10 K and the average grain emissivity index ([beta]) is 2.00 \u00b1 0.25. Using a radiative transfer program that solves for the dust temperature versus radius, the distribution of dust around UCHII regions is modeled with a power-law spherical density profile to match the observed radial flux density profiles. By fixing the source boundary at the outer limit of the submillimeter emission, the resulting density profiles n(r) [...] can be classified into four categories: 3 regions exhibit p = 2 (isothermal sphere), 4 exhibit p = 1.5 (dynamical collapse), 2 exhibit p = 2 in the outer regions and p = 1.5 in the inner regions, and 6 exhibit p = 1 (logatropic). Although these simplified models may not be unique, a good correlation between the dust luminosity-to-mass ratio and the temperature indicates that the more centrally-condensed sources exhibit higher star formation rates. Third, I present 20\" to 30\" resolution CO maps which reveal bipolar outflows from 15 out of 17 UCHII regions. The outflow mechanical luminosities and mass ejection rates follow the scaling relations with bolometric luminosity established for less luminous pre-main sequence stars. However, in contrast to lower luminosity sources, the momentum from stellar radiation pressure is comparable to that required to drive the outflows. Many regions show evidence of separate, overlapping outflows. In a final detailed study, 2\" resolution images obtained with the Owens Valley Millimeter Array reveal multiple outflows emanating from the molecular core containing the UCHII region G45.12+0.13, while simultaneous outflow and infall motion is seen toward the neighboring, less-evolved core containing G45.07+0.13.", "date": "1997", "date_type": "degree", "id_number": "CaltechETD:etd-05212007-111551", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05212007-111551", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-24", "doi": "10.7907/9k2a-vf26", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-21", "thesis_defense_date": "1996-09-17", "thesis_approved_date": "2007-05-24", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Hunter, Todd Russell" }, { "id": "/id/eprint/8552", "eprint_id": 8552, "rev_number": 19, "documents": [ { "id": "/id/document/50901", "doc_id": 50901, "rev_number": 5, "files": [ { "id": "/id/file/147333", "fileid": 147333, "datasetid": "document", "objectid": 50901, "filename": "Bin-m-1997.pdf", "mime_type": "application/pdf", "hash": "5045af4bbdd177afe986c53feb76c9c4", "hash_type": "MD5", "filesize": 31818985, "mtime": "2014-07-17 20:22:04", "url": "/8552/1/Bin-m-1997.pdf" } ], "eprint_id": 8552, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Bin-m-1997.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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tunneling junctions. The mixers utilize a quasi-optical configuration which consists of a planar twin-slot antenna and antisymmetrically-fed two-junctions on an antireflection-coated silicon hyperhemispherical lens. On-chip integrated tuning circuits, in the form of microstrip lines, are used to obtain maximum coupling efficiency in the designed frequency band. To reduce the rf losses in the integrated tuning circuits above the superconducting Nb gap frequency (~ 700 GHz), normal-metal Al is used to replace Nb as the tuning circuits.
\r\n\r\nTo account the rf losses in the micros trip lines, we calculated the surface impedance of the AI films using the nonlocal anomalous skin effect for finite thickness films. Nb films were calculated using the Mattis-Bardeen theory in the extreme anomalous limit. Our calculations show that the losses of the Al and Nb microstrip lines are about equal at 830 GHz. For Al-wiring and Nb-wiring mixers both optimized at 1050 GHz, the RF coupling efficiency of Al-wiring mixer is higher than that of Nb-wiring one by almost 50%. We have designed both Nb-wiring and Al-wiring mixers below and above the gap frequency.
\r\n\r\nA Fourier transform spectrometer (FTS) has been constructed especially for the study of the frequency response of SIS receivers. This FTS features large aperture size (10 inch) and high frequency resolution (114 MHz). The FTS spectra, obtained using the SIS receivers as direct detectors on the FTS, agree quite well with our theoretical simulations. We have also, for the first time, measured the FTS heterodyne response of an SIS mixer at sufficiently high resolution to resolve the LO and the sidebands. Heterodyne measurements of our SIS receivers with Nb-wiring or Al-wiring have yielded results which arc among the best reported to date for broadband heterodyne receivers. The Nb-wiring mixers, covering 400 - 850 GHz band with four separate fixed-tuned mixers, have uncorrected DSB receiver noise temperature around 5hv/kb to 700 GHz, and better than 540 K at 808 GHz. An Al-wiring mixer designed for 1050 GHz band has an uncorrected DSB receiver noise temperature 840 K at 1042 GHz and 2.5 K bath temperature. Mixer performance analysis shows that Nb junctions can work well up to twice the gap frequency and the major cause of loss above the gap frequency is the rf losses in the microstrip tuning structures. Further advances in THz SIS mixers may be possible using circuits fabricated with higher-gap superconductors such as NbN. However, this will require high-quality films with low RF surface resistance at THz frequencies.
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Microwave Theory Tech., vol. 42, pp. 698-706,\r\n1994.\r\nZmuidzinas, J. and H. G. LeDuc, \"Quasi-Optical Slot Antenna SIS Mixers,\" IEEE TI-ans. Microwave\r\nTheory Tech., vol. 40, pp. 1797-1804, 1992." ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Joy Painter", "deposited_on": "2014-07-18 16:55:00", "doi": "10.7907/AZYZ-XP41", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1996-10-03", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Bin, Mei" }, { "id": "/id/eprint/7434", "eprint_id": 7434, "rev_number": 26, "documents": [ { "id": "/id/document/34991", "doc_id": 34991, "rev_number": 3, "files": [ { "id": "/id/file/110721", "fileid": 110721, "datasetid": "document", "objectid": 34991, "filename": "Jiang_y_1997.zip", "mime_type": "application/x-zip", "hash": "f04148a160424b9446ad83252600fa98", "hash_type": "MD5", "filesize": 97983862, "mtime": "2013-01-24 22:20:32", "url": "/7434/1/Jiang_y_1997.zip" } ], "eprint_id": 7434, "pos": 1, "placement": 1, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Jiang_y_1997.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"datestamp": "2013-01-24 23:42:07", "lastmod": "2023-11-08 00:36:10", "status_changed": "2013-01-24 23:42:07", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jiang-Yibo", "name": { "family": "Jiang", "given": "Yibo" }, "orcid": "0000-0001-6711-7260", "show_email": "NO" } ] }, "title": "Decadal evolution of atmospheric ozone and remote sensing of tropospheric ozone", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Applied Mathematics", "abstract": "Monitoring and preservation of the Earth's ozone layer has engaged scientists intensively\r\nin the 20th century especially after the discovery of the Antarctic ozone hole by\r\nFarman et al. (1985). There is increasing evidence that ozone depletion occurs on a\r\nglobal scale such as in the Arctic and at midlatitudes. Following the understanding\r\nof the the catalytic destruction of ozone in the stratosphere by chlorine derived from\r\nchlorofluorocarbons (CFC's), there is a growing realization that the consequences of\r\nanthropogenic pollution can be felt in unpredictable ways in near and faraway places.
\r\n\r\nThe atmosphere is a complex mixture of more than a thousand trace chemicals\r\nthat are constantly reacting and redistributing. The need to understand the sources\r\nand distribution of these chemicals, along with the mechanisms by which they are\r\ntransformed, transported, and ultimately removed from the atmosphere, has grown in\r\nparallel with the increased concern about air pollution and its consequences. Therefore,\r\nthe exploration of the mechanism controlling both spatial and temporal variation of\r\nthe atmosphere is a key component of the atmosphere science research (as part\r\nof the global change) and it requires an interdisciplinary approach and innovative\r\napplication of the traditional techniques of chemistry, physics, and meteorology.
\r\n\r\nMonitoring the composition of the troposphere and stratosphere globally is particularly\r\ninteresting in this context for ozone which is the key component regulating\r\nthe photochemistry of the atmosphere.
\r\n\r\nIn chapter 1, the decadal evolution of the Antarctic ozone hole is studied by using\r\nozone column amounts obtained by the total ozone mapping spectrometer (TOMS) in\r\nthe southern polar region during late austral winter and spring (Days 240 - 300) for\r\n1980 - 1991 using area-mapping techniques and area-weighted vortex averages. The\r\nvortex here is defined using the -50 PVU (1 PVU = 1.0 x 10^(-6)K kg^(-1) m^2 s^(-1)) contour\r\non the 500 K isentropic surface. The principal result is that there is a distinct change\r\nafter 1985 in the vortex averaged column ozone depletion rate during September and\r\nOctober, the period of maximum ozone loss. The mean ozone depletion rate in the\r\nvortex between Day 240 and the day of minimum vortex-averaged ozone is about 1\r\nDU/day at the beginning of the decade, increasing to about 1.8 DU /day by 1985,\r\nand then apparently saturating thereafter. The vortex-average column ozone during\r\nSeptember and October has declined at the rate of 11.3 DU / yr (3.8%) from 1980\r\nto 1987 (90 DU over 8 yrs), and at a smaller rate of 2 DU / yr (0.9%) from 1987 to\r\n1991 (10 DU over 5 years, excluding the anomalous year 1988). We interpret the\r\nyear-to-year trend in the ozone depletion rate during the earlier part of the decade\r\nas due to the rise of anthropogenic chlorine in the atmosphere. The slower trend at\r\nthe end of the decade indicates saturation of ozone depletion in the vortex interior, in\r\nthat chlorine amounts in the mid-80s were already sufficiently high to deplete most of\r\nthe ozone in air within the isolated regions of the lower stratospheric polar vortex. In\r\nsubsequent years, increases in stratospheric chlorine may have enhanced wintertime\r\nchemical loss of ozone in the south polar vortex even before major losses during the\r\nAntarctic spring.
\r\n\r\nIn chapter 2, we will show that standard deviation of column ozone from the zonal\r\nmean (COSDZ) provides a measure of the longitudinal inhomogeneity in column ozone\r\nand dynamical wave activities in the atmosphere. We point out that simulation of this\r\nquantity by three-dimensional (3-D) models could provide a sensitive check on the\r\nwave activities in the stratosphere that are responsible for ozone transport. Analysis\r\nof the Total Ozone Mapping Spectrometer (TOMS) data shows a profound secular\r\nchange in COSDZ from 1979 to 1992. The changes are not symmetric between the\r\nsouthern and northern atmospheres. In the southern higher latitudes, COSDZ shows\r\na significant increase around 65\u00b0 in August and September, while the changes are\r\nmuch smaller in the northern higher latitudes in the boreal spring. We interpret most\r\nof the observed changes to be caused by enhanced ozone losses in the polar vortices in\r\nthe springtime of the two respective hemispheres. There is also evidence for secular\r\ndynamical changes at mid-latitudes.
\r\n\r\nIn chapter 3, an estimate of tropospheric ozone levels over tropical pacific south\r\nAmerica is obtained from the difference in the TOMS (Total Ozone Mapping Spectrometer)\r\ndata between the high Andes and the Pacific Ocean. From 1979 to 1992\r\ntropospheric ozone apparently increased by 1.47 \u00b1 0.40 %/yr or 0.21 \u00b1 0.06 DU / yr\r\nover South America and the surrounding oceans. An increase in biomass burning in\r\nthe Southern Hemisphere can account for this trend in tropospheric ozone levels.
\r\n\r\nDue to larger multiple scattering effects in the troposphere compared to that in\r\nthe stratosphere, the optical path of tropospheric ozone is markedly enhanced (as\r\ncompared with that of stratospheric ozone) in the Huggins bands from 310 nm to\r\n345 nm. By using this principle, we model the direct and diffuse solar fluxes on the\r\nground shows differences between tropospheric and stratospheric ozone in chapter 4.\r\nThe characteristic signature of tropospheric ozone enables us to distinguish a change\r\nin tropospheric ozone from that of stratospheric ozone. A simple retrieval algorithm\r\nis used to recover the tropospheric column ozone from simulated data.
\r\n\r\nLight reflected or transmitted by a planetary atmosphere contains information\r\nabout the particles and molecules in the atmosphere. Therefore, accurately calculating\r\nthe radiation field is necessary. In the appendix, the doubling-adding method for\r\nplane-parallel polarized radiative transfer model is studied in detail. A special Fourier\r\nexpansion leading to a compact notation is developed for the azimuth-dependent\r\nquantities. The multi-layer model for a vertically inhomogeneous atmosphere is implemented and several numerical results are presented for verification and comparison.\r\nPreliminary runs from this model in the Huggins bands show the distinct features of\r\nlinear polarization in the reflection spectrum due to the multiple Rayleigh scattering\r\nin the troposphere.
\r\n\r\n", "date": "1997", "date_type": "degree", "id_number": "CaltechTHESIS:01242013-141747377", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01242013-141747377", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2013-01-24 23:42:07", "doi": "10.7907/40ec-pk63", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "advisor" }, { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1997-05-20", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "appmath" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Jiang, Yibo" }, { "id": "/id/eprint/3598", "eprint_id": 3598, "rev_number": 14, "documents": [ { "id": "/id/document/6170", "doc_id": 6170, "rev_number": 3, "files": [ { "id": "/id/file/36915", "fileid": 36915, "datasetid": "document", "objectid": 6170, "filename": "Akeson_rl_1997.pdf", "mime_type": "application/pdf", "filesize": 6431972, "mtime": "2012-12-26 03:01:14", "url": "/3598/1/Akeson_rl_1997.pdf" } ], "eprint_id": 3598, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Akeson_rl_1997.pdf", "language": "en", "security": "public", "license": "other", "main": "Akeson_rl_1997.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22708" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22708" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22708" } ] } }, { "id": "/id/document/22708", "doc_id": 22708, "rev_number": 3, "files": [ { "id": "/id/file/36913", "fileid": 36913, "datasetid": "document", "objectid": 22708, "filename": "preview.png", "mime_type": "image/png", "hash": "7e73e97e310a1604f2ae60222f46fd50", "hash_type": "MD5", "filesize": 10982, "mtime": "2012-12-26 03:01:14", "url": "/3598/2/preview.png" } ], "eprint_id": 3598, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6170" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6170" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6170" } ] } }, { "id": "/id/document/77869", "doc_id": 77869, "rev_number": 3, "files": [ { "id": "/id/file/220913", "fileid": 220913, "datasetid": "document", "objectid": 77869, "filename": "Akesonauthorok05152017.txt", "mime_type": "message/rfc822\\0117bit", "hash": "e6023c1364fdd6984b77ca18fb998a87", "hash_type": "MD5", "filesize": 940, "mtime": "2017-05-15 19:02:12", "url": "/3598/3/Akesonauthorok05152017.txt" } ], "eprint_id": 3598, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "authr ok 05/15/2017", "language": "en", "security": "internal", "license": "other", "main": "Akesonauthorok05152017.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/98", "datestamp": "2008-10-31", "lastmod": "2019-12-21 04:34:45", "status_changed": "2009-09-25 03:01:25", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "rla@ipac.caltech.edu", "id": "Akeson-Rachel-Lynn", "name": { "family": "Akeson", "given": "Rachel Lynn" }, "orcid": "0000-0001-9674-1564", "show_email": "NO" } ] }, "title": "Millimeter Interferometric Polarimetry of Magnetic Field Structure in Protostellar Condensations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Images of the linearly polarized emission from magnetically aligned dust grains have been used to investigate the magnetic field structure in the dense environments of young stellar objects. These observations provide constraints for theoretical modeling on scales relevant to protostellar disks, envelopes and outflows. Adjustable reflecting polarizers were installed at the Owens Valley Radio Observatory millimeter array to allow observations of polarized emission.
\r\n\r\nPolarized emission was detected toward two young stellar objects NGC 1333/ IRAS 4A and IRAS 16293-2422. Both sources are highly embedded and considered among the youngest objects known. The strong sub-millimeter and millimeter fluxes indicate a large amount of circumstellar material which may correspond to the magnetically supported envelopes predicted by theoretical models. Toward IRAS 4A, the magnetic field direction implied by the polarization position angle is parallel to the bipolar molecular outflow. Radiative transfer models were calculated and the offset of the polarized emission toward red-shifted outflow is consistent with an hourglass field morphology in the envelope.
\r\n\r\nThe polarized emission toward IRAS 16293 is located between the two binary components. The magnetic field direction coincides with directions seen in one of the four outflow lobes. However, the field direction is perpendicular to the rotation axis of the circumbinary disk. Given the complicated outflow and circumbinary disk structure of the source, a simple model can not explain the implied magnetic field direction or the offset of the polarized emission from the total intensity.
\r\n\r\nObservations were also made of the Orion KL region, though no polarization was detected. The upper limit to the polarized emissions suggests that the decrease in polarization seen by single-dish surveys toward the high mass young stellar object IRc2, is not due to field tangling.
\r\n\r\nThe implications of significant polarized emission as detected in the envelopes of IRAS 4A and IRAS 16293 are considered for several alignment mechanisms. Alignment by paramagnetic relaxation of thermally rotating grains will not be efficient in these dense, warm regions, and some mechanism for suprathermal grain rotation may be necessary to explain the observations.
\r\n\r\nThese observations clearly demonstrate the power of interferometric millimeter polarimetry in the study of the role of magnetic fields in protostellar condensations.
\r\n", "date": "1997", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-132123", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-132123", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-31", "doi": "10.7907/RGCX-HK35", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Carlstrom-J-E", "name": { "family": "Carlstrom", "given": "John E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "1996-07-19", "thesis_approved_date": "2008-10-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Akeson, Rachel Lynn" }, { "id": "/id/eprint/3668", "eprint_id": 3668, "rev_number": 10, "documents": [ { "id": "/id/document/6270", "doc_id": 6270, "rev_number": 3, "files": [ { "id": "/id/file/37565", "fileid": 37565, "datasetid": "document", "objectid": 6270, "filename": "Bryant_pm_1997.pdf", "mime_type": "application/pdf", "filesize": 8999590, "mtime": "2012-12-26 03:01:57", "url": "/3668/1/Bryant_pm_1997.pdf" } ], "eprint_id": 3668, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Bryant_pm_1997.pdf", "language": "en", "security": "public", "license": "other", "main": "Bryant_pm_1997.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22808" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22808" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22808" } ] } }, { "id": "/id/document/22808", "doc_id": 22808, "rev_number": 3, "files": [ { "id": "/id/file/37563", "fileid": 37563, "datasetid": "document", "objectid": 22808, "filename": "preview.png", "mime_type": "image/png", "hash": "0ef8b3aba97c99661ab7b9122ac88707", "hash_type": "MD5", "filesize": 9563, "mtime": "2012-12-26 03:01:56", "url": "/3668/2/preview.png" } ], "eprint_id": 3668, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6270" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6270" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6270" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/36/68", "datestamp": "2008-11-06", "lastmod": "2021-04-16 23:05:00", "status_changed": "2009-09-25 03:03:09", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bryant-P-M", "name": { "family": "Bryant", "given": "Peter M." }, "show_email": "NO" } ] }, "title": "High-resolution observations of the molecular gas in luminous infrared galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "I have performed a high-resolution imaging survey of the molecular gas in seven luminous infrared galaxies using the Owens Valley millimeter array. This work has produced 2\"-resolution maps of the CO 1\u21920 emission. Further high-resolution data has been obtained for subsets of these galaxies in CO 2\u21921, HCN 1\u21920, HCO[superscript +] 1\u21920 and CS 1\u21920.\r\n\r\nThe CO maps reveal a systematic variation in the morphology of the molecular gas with the interaction state of the system. The three mergers with a single IR/radio nucleus show very bright and compact CO cores that peak at the stellar nucleus. The two mergers with double IR/radio nuclei also possess bright CO cores, but these peak roughly midway between the nuclei and show an extent nearly equal to the nuclear separation. In these objects, the gas cores of the individual merging galaxies appear to be coalescing while the stellar nuclei still remain distinct.\r\n\r\nBased on dynamical arguments, the Galactic conversion factor from CO luminosity to molecular gas mass is overestimating the gas mass in Mrk 231 by at least a factor of 3.6 and in NGC 6240 by at least a factor of 1.5. Nonetheless, the molecular gas likely dominates the nuclear gravitational potential. The probable cause of the severe overestimate in Mrk 231 is the high brightness temperature of the CO 1\u21920 emission (T[subscript b] > 34 K).\r\n\r\nStarbursts remain a viable explanation for the powerful output of luminous infrared galaxies. Upper limits to the free-free mm-wave continuum are used to constrain a starburst model from the literature, with the result that starbursts can reasonably explain all the systems studied here except perhaps Mrk 231. In several cases, though, they are required to be older than several 10[superscript 7] yr. Furthermore, the extreme mid-IR optical depths implied by the CO surface brightnesses confirm a prediction of the compact starburst model of Condon et al. (1991).\r\n\r\nThe trend of increasing L[subscript FIR]/L[subscript CO] ratio with increasing CO surface brightness is confirmed. The high concentrations of molecular gas thus appear intimately related to the high luminosities of these systems.\r\n\r\nThe CO/HCN ratio varies by an order of magnitude even in this small sample of luminous mergers, suggesting that the gas properties are dramatically variable.\r\n", "date": "1997", "date_type": "degree", "id_number": "CaltechETD:etd-09202008-104546", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09202008-104546", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-06", "doi": "10.7907/0rav-qq54", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-20", "thesis_defense_date": "1996-09-16", "thesis_approved_date": "2008-11-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Bryant, Peter M." }, { "id": "/id/eprint/4607", "eprint_id": 4607, "rev_number": 16, "documents": [ { "id": "/id/document/7446", "doc_id": 7446, "rev_number": 2, "files": [ { "id": "/id/file/45513", "fileid": 45513, "datasetid": "document", "objectid": 7446, "filename": "Asimow_pd_1997.pdf", "mime_type": "application/pdf", "filesize": 19908356, "mtime": "2012-12-26 03:10:13", "url": "/4607/1/Asimow_pd_1997.pdf" } ], "eprint_id": 4607, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Asimow_pd_1997.pdf", "language": "en", "security": "public", "license": "other", "main": "Asimow_pd_1997.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23971" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23971" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23971" } ] } }, { "id": "/id/document/23971", "doc_id": 23971, "rev_number": 2, "files": [ { "id": "/id/file/45511", "fileid": 45511, "datasetid": "document", "objectid": 23971, "filename": "preview.png", "mime_type": "image/png", "hash": "0e1b6fad2f9aacae892bca137e2b9163", "hash_type": "MD5", "filesize": 8170, "mtime": "2012-12-26 03:10:13", "url": "/4607/2/preview.png" } ], "eprint_id": 4607, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7446" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7446" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7446" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/46/07", "datestamp": "2003-11-21", "lastmod": "2023-11-08 00:16:43", "status_changed": "2009-09-25 03:21:53", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "asimow@caltech.edu", "id": "Asimow-Paul-David", "name": { "family": "Asimow", "given": "Paul David" }, "orcid": "0000-0001-6025-8925", "show_email": "NO" } ] }, "title": "A Thermodynamic Model of Adiabatic Melting of the Mantle", "ispublished": "unpub", "full_text_status": "public", "keywords": "Geology", "abstract": "Mid-ocean ridge basalts (MORB) are mixtures of melts produced over a range of pressure and temperature in a nearly adiabatic open system undergoing changes in composition as melting proceeds. Interpretation of the compositional variations observed in MORB and their correlation with geophysical aspects of the ridge therefore requires complex forward models to connect experimental observations of isothermal, isobaric batch melting of peridotite to natural compositions. Previous attempts to construct such models have relied on parameterizations of melt composition or partition coefficients and extent of melting in pressure-temperature space from experimental batch melting data. This thesis undertakes the examination of an alternative approach using thermodynamic models of silicate minerals and melts to predict equilibria under quite arbitrary constraints, including variable bulk composition and constant entropy. The liquids predicted from the thermodynamic models along polybaric paths can then be integrated to produce comprehensive forward models of MORB genesis.
\r\n \r\nChapter 1 introduces the nature of the MORB modeling problem and the motivation of the thermodynamic approach in greater detail. Chapter 2 illustrates the thermodynamic approach by demonstrating that the effect of the garnet-spinel and spinelplagioclase peridotite transitions, which retard or reverse isentropic melting, can be easily understood. Chapter 3 looks at the variables affecting isentropic melt productivity (i.e., the increment of additional melting per decrement of pressure at constant entropy). I find that this quantity is likely to increase during progressive melting, punctuated by drops where phases are exhausted from the residuum. Chapter 4 extends this approach to issues of melt transport in one dimension and steady state; I evaluate the magnitude of entropy production due to gravitational dissipation and thermal interactions with migrating fractional melts and examine the effect of focused melt flow. Finally, chapter 5 deals with the compositions and mean properties of MORB obtained by integrating the compositions and melt fractions predicted by our models. We compare our results to published models of MORB compositions and consider the implications. The algorithms and source code, including subsolidus capability, added to the MELTS package of Ghiorso and Sack for these calculations are included as appendices.
", "date": "1997", "date_type": "degree", "id_number": "CaltechETD:etd-11202003-144820", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-11202003-144820", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "suggestions": "Caltech faculty", "deposited_by": "Imported from ETD-db", "deposited_on": "2003-11-21", "doi": "10.7907/93RY-AN70", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stolper-E-M", "name": { "family": "Stolper", "given": "Edward M." }, "orcid": "0000-0001-8008-8804", "role": "advisor" }, { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "chair" }, { "id": "Gurnis-M-C", "name": { "family": "Gurnis", "given": "Michael C." }, "orcid": "0000-0003-1704-597X", "role": "member" }, { "id": "Wyllie-P-J", "name": { "family": "Wyllie", "given": "Peter J." }, "role": "member" }, { "id": "Stolper-E-M", "name": { "family": "Stolper", "given": "Edward M." }, "orcid": "0000-0001-8008-8804", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-11-20", "thesis_defense_date": "1997-05-28", "thesis_approved_date": "2003-11-21", "review_status": "approved", "option_major": { "items": [ "geol" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Asimow, Paul David" }, { "id": "/id/eprint/8666", "eprint_id": 8666, "rev_number": 36, "documents": [ { "id": "/id/document/52269", "doc_id": 52269, "rev_number": 3, "files": [ { "id": "/id/file/151130", "fileid": 151130, "datasetid": "document", "objectid": 52269, "filename": "Labrador.pdf", "mime_type": "application/pdf", "hash": "8a00357b1f7c74e59454f4c1ccffe271", "hash_type": "MD5", "filesize": 45698731, "mtime": "2014-09-29 16:16:13", "url": "/8666/1/Labrador.pdf" } ], "eprint_id": 8666, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Labrador.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/52270", 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"type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "labrador@srl.caltech.edu", "id": "Labrador-Allan-Wayne", "name": { "family": "Labrador", "given": "Allan Wayne" }, "orcid": "0000-0001-9178-5349", "show_email": "NO" } ] }, "title": "Measurement of the Galactic Cosmic Ray Antiproton Flux from 0.25 GeV to 3.11 GeV with the Isotope Matter Antimatter Experiment (IMAX)", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmic Rays, Antiprotons, Antimatter, Experiment", "abstract": "The intensities and relative abundances of galactic cosmic ray protons and antiprotons have been measured with the Isotope Matter Antimatter Experiment (IMAX), a balloon-borne magnet spectrometer. The IMAX payload had a successful flight from Lynn Lake, Manitoba, Canada on July 16, 1992. Particles detected by IMAX were identified by mass and charge via the Cherenkov-Rigidity and TOP-Rigidity techniques, with measured rms mass resolution \u22640.2 amu for Z=1 particles.
\r\n\r\nCosmic ray antiprotons are of interest because they can be produced by the interactions of high energy protons and heavier nuclei with the interstellar medium as well as by more exotic sources. Previous cosmic ray antiproton experiments have reported an excess of antiprotons over that expected solely from cosmic ray interactions.
\r\n\r\nAnalysis of the flight data has yielded 124405 protons and 3 antiprotons in the energy range 0.19-0.97 GeV at the instrument, 140617 protons and 8 antiprotons in the energy range 0.97-2.58 GeV, and 22524 protons and 5 antiprotons in the energy range 2.58-3.08 GeV. These measurements are a statistical improvement over previous antiproton measurements, and they demonstrate improved separation of antiprotons from the more abundant fluxes of protons, electrons, and other cosmic ray species.
\r\n\r\nWhen these results are corrected for instrumental and atmospheric background and losses, the ratios at the top of the atmosphere are p̅/p=3.21(+3.49, -1.97)x10\u207b\u2075 in the energy range 0.25-1.00 GeV, p̅/p=5.38(+3.48, -2.45)x10\u207b\u2075 in the energy range 1.00-2.61 GeV, and p̅/p=2.05(+1.79, -1.15)x10\u207b\u2074 in the energy range 2.61-3.11 GeV. The corresponding antiproton intensities, also corrected to the top of the atmosphere, are 2.3(+2.5, -1.4) x10\u207b\u00b2 (m\u00b2 s sr GeV)\u207b\u00b9, 2.1(+1.4, -1.0)x10\u207b\u00b2 (m\u00b2 s sr GeV)\u207b\u00b9, and 4.3(+3.7, -2.4) x10\u207b\u00b2 (m\u00b2 s sr GeV)\u207b\u00b9 for the same energy ranges.
\r\n\r\nThe IMAX antiproton fluxes and antiproton/proton ratios are compared with recent Standard Leaky Box Model (SLBM) calculations of the cosmic ray antiproton abundance. According to this model, cosmic ray antiprotons are secondary cosmic rays arising solely from the interaction of high energy cosmic rays with the interstellar medium. The effects of solar modulation of protons and antiprotons are also calculated, showing that the antiproton/proton ratio can vary by as much as an order of magnitude over the solar cycle. When solar modulation is taken into account, the IMAX antiproton measurements are found to be consistent with the most recent calculations of the SLBM. No evidence is found in the IMAX data for excess antiprotons arising from the decay of galactic dark matter, which had been suggested as an interpretation of earlier measurements. Furthermore, the consistency of the current results with the SLBM calculations suggests that the mean antiproton lifetime is at least as large as the cosmic ray storage time in the galaxy (~10\u2077 yr, based on measurements of cosmic ray \u00b9\u2070Be). Recent measurements by two other experiments are consistent with this interpretation of the IMAX antiproton results.
\r\n", "date": "1997", "date_type": "degree", "id_number": "CaltechTHESIS:09292014-084326709", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09292014-084326709", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department", "Space Radiation Laboratory" ] }, "deposited_on": "2014-09-29 17:26:43", "doi": "10.7907/92WC-0T91", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "advisor" }, { "email": "rmewaldt@caltech.edu", "id": "Mewaldt-R", "name": { "family": "Mewaldt", "given": "Richard" }, "role": "advisor" }, { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "chair" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "email": "rmewaldt@caltech.edu", "id": "Mewaldt-R-A", "name": { "family": "Mewaldt", "given": "Richard A." }, "role": "member" }, { "email": "newman@hep.caltech.edu", "id": "Newman-H-B", "name": { "family": "Newman", "given": "Harvey B." }, "role": "member" }, { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1996-09-03", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Labrador, Allan Wayne" }, { "id": "/id/eprint/10416", "eprint_id": 10416, "rev_number": 18, "documents": [ { "id": "/id/document/82642", "doc_id": 82642, "rev_number": 3, "files": [ { "id": "/id/file/233556", "fileid": 233556, "datasetid": "document", "objectid": 82642, "filename": "Ryan_fd_1997.zip", "mime_type": "application/x-zip", "hash": "ddec03bb995ae2c415c93869ee49a62c", "hash_type": "MD5", "filesize": 94199673, "mtime": "2017-09-12 20:34:36", "url": "/10416/1/Ryan_fd_1997.zip" } ], "eprint_id": 10416, "pos": 1, "placement": 1, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Ryan_fd_1997.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", 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"datestamp": "2017-09-12 20:44:04", "lastmod": "2021-04-16 23:24:47", "status_changed": "2017-09-12 20:44:04", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ryan-Fintan-Danh", "name": { "family": "Ryan", "given": "Fintan Danh" } } ] }, "title": "Searching for Black Holes and Other Massive, Compact Bodies Using the Gravitational Waves from Binary Inspirals", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "We consider several issues involved with searching for and studying different types of compact bodies using the gravitational waves from binary inspirals. In Chapter 2, we use a radiation\u00ad reaction force formalism to compute (to leading post-Newtonian order) the inspiral evolution of a circular, nonequatorial orbit around a spinning black hole. We find that an initially circular orbit remains circular under radiation reaction and is driven towards anti-alignment with the black hole's spin direction. In Chapter 3, we apply this same formalism to orbits which are elliptical as well as nonequatorial. In addition, we prove that circular orbits remain circular exactly. In Chapter 4, we show that all the multipole moments of a massive, compact body (whose gravita\u00adtional field is stationary, axially symmetric, and reflection symmetric across the equatorial plane) can be determined from the gravitational waves produced by a much less massive, compact object inspiraling in a contracting circle in the equatorial plane. We show that the moments are encoded in the waves' evolution in (at least) four independent functions of the gravitational-wave frequency: the gravitational-wave energy, the precession frequency of the orbit when slightly eccentric, the precession frequency of the orbit when slightly nonequatorial, and the gravitational-wave phase evolution. In Chapter 5, we compute the structure and the multipole moments of a spinning boson star with large self-interaction. We find that only three moments are needed to specify all the star's properties, and that the pattern of moments is very different from that for black holes. In Chapter 6, we estimate how accurately a gravitational-wave detector can estimate the multipole moments of the central body from the gravitational waves produced by an inspiraling compact object. We find that, typically, a space-based detector such as LISA (as opposed to an Earth-based detector such as LIGO) is necessary to get accurate enough measurements of the multipole moments so as to search for massive, compact, non-black-hole objects. In Chapter 7, as a model for computing the full details of the gravitational waves from an orbital inspiral, we compute the scalar waves produced by a scalar charge in a circular, equatorial orbit around a body with arbitrary multipole moments.", "date": "1997", "date_type": "degree", "id_number": "CaltechTHESIS:09062017-160111338", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09062017-160111338", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-09-12 20:44:04", "doi": "10.7907/3n38-zg42", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1997-05-16", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Ryan, Fintan Danh" }, { "id": "/id/eprint/10384", "eprint_id": 10384, "rev_number": 19, "documents": [ { "id": "/id/document/82150", "doc_id": 82150, "rev_number": 3, "files": [ { "id": "/id/file/231958", "fileid": 231958, "datasetid": "document", "objectid": 82150, "filename": "Kennefick_d_1997.zip", "mime_type": "application/x-zip", "hash": "99bfe33ac0e6140f066bf24e0130fd51", "hash_type": "MD5", "filesize": 284505601, "mtime": "2017-08-22 23:02:20", "url": "/10384/1/Kennefick_d_1997.zip" } ], "eprint_id": 10384, "pos": 1, "placement": 1, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Kennefick_d_1997.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": 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"userid": 87, "dir": "disk0/00/01/03/84", "datestamp": "2017-08-25 14:41:56", "lastmod": "2021-04-16 23:03:31", "status_changed": "2017-08-25 14:41:56", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kennefick-Daniel-John", "name": { "family": "Kennefick", "given": "Daniel John" } } ] }, "title": "Radiation Reaction in Binary Systems in General Relativity", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis is concerned with current problems in, and historical aspects of, the problem of radiation reaction in stellar binary systems in general relativity. Part I addresses current issues in the orbital evolution due to gravitational radiation damping of compact binaries. A particular focus is on the inspiral of small bodies orbiting large black holes, employing a perturbation formalism. In addition, the merger, at the end of the insprial, of comparable mass compact binaries, such as neutron star binaries is also discussed. The emphasis of Part I is on providing detailed descriptions of sources and signals with a view to optimising signal analysis in gravitational wave detectors, whether ground- or space-based interferometers, or resonant mass detectors.
\r\n\r\n\r\nPart II of the thesis examines the historical controversies surrounding the prob\u00adlem of gravitational waves, and gravitational radiation damping in stellar binaries. In particular, it focuses on debates in the mid 20th-century on whether binary star systems would really exhibit this type of damping and emit gravitational waves, and on the \"quadrupole formula controversy\" of the 1970s and 1980s, on the question whether the standard formular describing energy loss due to emission of gravita\u00adtional waves was correctly derived for such systems. The study sheds light on the role of analogy in science, especially where its use is controversial, on the importance of style in physics and on the problem of identity in science, as the use of history as a rhetorical device in controversial debate is examined. The concept of the Theo\u00adretician's Regress is introduced to explain the difficulty encountered by relativists in closing debate in this controversy, which persisted in one form or another for several decades.
", "date": "1997", "date_type": "degree", "id_number": "CaltechTHESIS:08222017-154459722", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08222017-154459722", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "SBR-9412026" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-25 14:41:56", "doi": "10.7907/jzcp-a525", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1996-12-09", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Kennefick, Daniel John" }, { "id": "/id/eprint/10969", "eprint_id": 10969, "rev_number": 21, "documents": [ { "id": "/id/document/90435", "doc_id": 90435, "rev_number": 3, "files": [ { "id": "/id/file/255623", "fileid": 255623, "datasetid": "document", "objectid": 90435, "filename": "Knop_RA_1997.pdf", "mime_type": "application/pdf", "hash": "bac3fe16643810148417f19168be248c", "hash_type": "MD5", "filesize": 63346835, "mtime": "2018-05-30 15:46:55", "url": "/10969/1/Knop_RA_1997.pdf" } ], "eprint_id": 10969, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Knop_RA_1997.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/90588" } ] } } ], "eprint_status": "archive", "userid": 1660, "dir": "disk0/00/01/09/69", "datestamp": "2018-05-30 16:04:49", "lastmod": "2020-03-10 23:22:59", "status_changed": "2018-05-30 16:04:49", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "knopra@westminster.edu", "id": "Knop-Robert-A-Jr", "name": { "family": "Knop", "given": "Robert A., Jr." }, "show_email": "YES" } ] }, "title": "Spatially Resolved Infrared Spectroscopy of Seyfert Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis presents infrared spectroscopy of the circumnuclear regions of 23 Seyfert galaxies. Observations are spectrally resolved with a resolution of \u03bb/\u0394\u03bb ~ 1000 and spatially resolved to ~ 1\", corresponding to ~ 102 pc for the objects in the sample. The instrument used for the observations, the Palomar Near-Infrared Spectrometer, is described, and problems peculiar to reduction of data from it are discussed. The lines observed include Pa\u03b2, Br\u03b3, [FeII] (\u03bb=l.2567\u03bcm), and H2 (\u03bb=2.1213\u03bcm). In nine objects, the coronal line [SIX] (\u03bb=l.2524\u03bcm) is also detected. Spatially resolved line emission is clearly visible in approximately half of the objects observed. The data for five of the objects showing the best spatially resolved infrared line emission are analyzed in detail. These objects include Seyfert 1.5 galaxy NGC 4151 and Seyfert 2 galaxies Mk 1066, NGC 2110, NGC 4388, and Mk 3. The data for the remaining objects is presented in tabular form, and each object is discussed briefly. The data argue that processes associated with the Seyfert nucleus are responsible for the bulk of the observed [FeII] emission. Kinematic and spatial associations can be drawn between features in the [FeII] line profiles and other processes associated with the active nucleus, such as outflows seen in ionized optical emission and radio lobes. Most of the [FeII] appears to emerge from partially ionized regions excited by nuclear x-rays, with an additional contribution from fast shocks. Some of the H2 emission also appears to be associated with the nuclear activity. However, in some cases the H2 emission is observed to have a different spatial distribution from [FeII] and the H+ emission. The H2 emission is probably thermally excited. No significant differences are found between the infrared line emission of Seyfert and Seyfert l.x galaxies.
", "date": "1997", "date_type": "degree", "id_number": "CaltechTHESIS:05302018-084028309", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05302018-084028309", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Bianca Rios", "deposited_on": "2018-05-30 16:04:49", "doi": "10.7907/GZ2H-3X10", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "member" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1997-05-20", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1997", "author_list": "Knop, Robert A., Jr." }, { "id": "/id/eprint/3441", "eprint_id": 3441, "rev_number": 10, "documents": [ { "id": "/id/document/5976", "doc_id": 5976, "rev_number": 3, "files": [ { "id": "/id/file/35606", "fileid": 35606, "datasetid": "document", "objectid": 5976, "filename": "Small_ta_1996.pdf", "mime_type": "application/pdf", "filesize": 9472393, "mtime": "2012-12-26 02:59:56", "url": "/3441/1/Small_ta_1996.pdf" } ], "eprint_id": 3441, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Small_ta_1996.pdf", "language": "en", "security": "public", "license": "other", "main": "Small_ta_1996.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22516" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22516" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22516" } ] } }, { "id": "/id/document/22516", "doc_id": 22516, "rev_number": 3, "files": [ { "id": "/id/file/35604", "fileid": 35604, "datasetid": "document", "objectid": 22516, "filename": "preview.png", "mime_type": "image/png", "hash": "54d3615d24ead2bc0163a73977b34d3a", "hash_type": "MD5", "filesize": 8922, "mtime": "2012-12-26 02:59:56", "url": "/3441/2/preview.png" } ], "eprint_id": 3441, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5976" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5976" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5976" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/41", "datestamp": "2008-09-26", "lastmod": "2021-04-16 23:00:11", "status_changed": "2009-09-25 02:58:28", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Small-T-A", "name": { "family": "Small", "given": "Todd Andrew" }, "show_email": "NO" } ] }, "title": "The Norris survey of the Corona Borealis supercluster", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nWe describe the design, construction, and first results of the Norris Survey of the Corona Borealis Supercluster, a redshift survey of a 6[...] x 6[...] region in the core of the Corona Borealis supercluster.\r\n\r\nThe redshift survey has been conducted with the 176-fiber Norris Spectrograph on the Hale 5m telescope. The input catalog is based on machine scans of Schmidt plates and consists of over 5 x 10[...] objects calibrated in the Gunn g and r bands. We chose to observe 36 20' diameter fields arranged in a 6 x 6 grid across the core of the supercluster. We have completed observations of 23 of these fields, plus an additional 9 fields which were closely spaced along the ridge of galaxies between Abell 2061 and Abell 2067. We have measured redshifts for 1491 extragalactic objects, 420 with [...] 8[...] resolution and the remainder with [...] 4[...] resolution. Our newly measured redshifts were augmented with 163 from the literature, yielding 1654 redshifts for the entire survey. The faintest galaxies in the survey have magnitudes of [...] 22.5[...], and the most distant galaxies have redshifts of [...] 0.7.\r\n\r\nWe have measured an unexpectedly small number of redshifts (528) in the Corona Borealis supercluster since the supercluster is not as dense as originally believed and since a background supercluster at [...] 0.11 makes a substantial contribution to the projected surface density of galaxies. Despite the small number of redshifts for galaxies in the supercluster, we are able to draw the following conclusions about the dynamics and structure of the Corona Borealis supercluster. (1) The galaxy distribution within the supercluster is far from smooth. The galaxy density falls rapidly away from the Abell cluster cores. (2) The virial mass of the supercluster is [...], which yields a B band mass-to-light ratio of [...]. (3) The dynamics of the supercluster, as revealed through an analysis of the two-point correlation function, suggest that the supercluster has not yet generated large mean flows towards itself and that, therefore, the supercluster has only recently begun to break away from the Hubble expansion.\r\n\r\nSince the sample of redshifts extends to z = 0.5, we have been able to investigate the evolution of large-scale structure and of the galaxy population. By computing the projected two-point spatial correlation function [...], we have measured the correlation length [...] and the power-law index [...] of the real space correlation function [...] as a function of redshift. We find that the correlation length declines dramatically with increasing redshift. Incorporating measurements of [...] from other surveys, we measure the evolutionary parameter [...] to be 2.25 [...] 0.1 for [...] = 1.7, well in excess of the linear theory prediction [...] = [...] - 1. We do not see evolution in the clustering of red galaxies; the clustering evolution is limited to the blue galaxies.\r\n\r\nWe have also measured the pairwise velocity dispersion [...] on a scale of [...] Mpc through an analysis of the two-point spatial correlation function computed as a function of pair separations along and perpendicular to the line-of-sight. Although [...] is quite sensitive to the treatment of rich clusters in the survey, we conclude that [...] is significantly larger than the canonical value of 340 [...] 40 [...] computed by Davis and Peebles (1983). This result is in accord with other recent estimates of [...].\r\n\r\nWe have characterized structure on scales of [...] Mpc by measuring the one-dimensional power spectrum of our survey. We measure a significant peak on scales of [...] Mpc. The structures responsible for the peak are readily identifiable in redshift-right- ascension cone diagrams: superclusters are separated by large underdense regions.\r\n\r\nUsing 598 field galaxies with [...] from our survey, we have computed the field galaxy luminosity function as a function of color and redshift. We find compelling evidence that the B band field galaxy luminosity function evolves with redshift. The evolution is limited to blue galaxies; the red galaxies show no sign of change to z = 0.5. The evolution of the luminosity function of blue galaxies, which is corroborated by a [...] test, is reflected in the blueward shift of the median galaxy color with redshift and in the increasing fraction of galaxies displaying the star-formation indicators [0 II] and [...] with redshift.\r\n", "date": "1996", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-111656", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-111656", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-26", "doi": "10.7907/sy8m-7r36", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1995-12-06", "thesis_approved_date": "2008-09-26", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1996", "author_list": "Small, Todd Andrew" }, { "id": "/id/eprint/10964", "eprint_id": 10964, "rev_number": 26, "documents": [ { "id": "/id/document/90382", "doc_id": 90382, "rev_number": 3, "files": [ { "id": "/id/file/255464", "fileid": 255464, "datasetid": "document", "objectid": 90382, "filename": "Larkin_JE_1996.pdf", "mime_type": "application/pdf", "hash": "44051346254b872234fb890ce6564f9b", "hash_type": "MD5", "filesize": 44533337, "mtime": "2018-05-29 23:31:57", "url": "/10964/1/Larkin_JE_1996.pdf" } ], "eprint_id": 10964, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Larkin_JE_1996.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 87, "dir": "disk0/00/01/09/64", "datestamp": "2018-05-30 15:58:24", "lastmod": "2020-03-10 23:23:13", "status_changed": "2018-05-30 15:58:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "larkin@astro.ucla.edu", "id": "Larkin-James-Edwin", "name": { "family": "Larkin", "given": "James Edwin" }, "show_email": "YES" } ] }, "title": "Near Infrared Spectroscopy of LINER Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Infrared Spectroscopy Active Galactic Nuclei", "abstract": "This thesis reports the design and operation of a new near infrared spectrograph \r\nfor the 5 m Hale telescope and its use to observe a sample of LINER galaxies. The \r\nspectrograph operates between 1 and 5 microns using existing infrared array cameras.\r\nIt has two long-slit spectroscopy modes yielding resolutions (\u03bb/\u0394\u03bb) of ~850 and\r\n~3300 with a 0.75\" wide by 40\" long slit. The spectrograph also has a direct imaging \r\nmode giving a 10\"x40\" field of view.
\r\n\r\nThe galaxy sample includes 15 LINERs with spectra covering the [Fell](1.2567 \u00b5m), \r\nPa\u03b2 (1.2818 \u00b5m), H2 (1-0 S(1), 2.1218 \u00b5m) and Br\u03b3 (2.1655 \u00b5m) near infrared \r\nemis\u00adsion lines, and one additional galaxy with only [FeII] and Pa\u03b2 line coverage. The\r\nsample included, twelve low luminosity objects (classical LINERs) selected from sur\u00adveys \r\nof nearby galaxies, and four high luminosity multiple nuclei systems.
\r\n\r\nAll of the classical LINERs with infrared line detections have strong [FeII] and/or \r\nH2 emission, with about half (4 out of 9) having extremely high ratios (>2) of [FeII] \r\nto Pa\u03b2. The strength of the H2 and [FeII] lines is well correlated with the optical [OI] \r\nline, with many LINERs having higher ratios of [FeII]/Pa\u03b2, H2/Br\u03b3 and [OI]/H\u03b1\r\ncompared to other galaxy types. The LINERs with the highest [Fell]/Pa\u03b2 ratios \r\n(termed \"strong\" [FeII] LINERs) show evidence for recent star formation. Shocks \r\nfrom compact supernova remnants may enhance the [FeII] emission in these \"strong\" \r\n[FeII] LINERs. The LINERs with lower [FeII]/Pa\u03b2 ratios (termed \"weak\" [FeII] \r\nLINERs) are more consistent with Seyfert-like activity, including higher ionization \r\nstates, some strong x-ray sources and some broad H\u03b1 detections. The [FeII] luminosity \r\nand the [FeII]/ Pa\u03b2 ratio in these objects is more easily explained by hard x-ray \r\nexcitation than in the \"strong\" [FeII] LINERs. These \"weak\" [FeII] LINERs are \r\nconsidered prime candidates for being low luminosity Seyfert nuclei.
\r\n\r\nThe two multiple nuclei LINERs with line detections, IRAS 17132+5313 and \r\nArp 220, had lower ratios of [Fell]/Pa\u03b2 and/or H2/Br\u03b3 than the classical LIN\u00adERs. \r\nThe spectra of Arp 220 show that the extended emission has higher ratios \r\nof [Fell]/Pa\u03b2 and H2/Br\u03b3 than found on the nuclei. It is suggested that in these \r\nmerging systems, the low ionization line emission probably results from shocks, \r\nei\u00adther from cloud-cloud collisions or winds in the gas surrounding the nuclei.
\r\n\r\n\r\n", "date": "1996", "date_type": "degree", "id_number": "CaltechTHESIS:05292018-163017352", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05292018-163017352", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2018-05-30 15:58:24", "doi": "10.7907/0G7Z-BS49", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "chair" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1995-10-09", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "paul.alan.stockman@gmail.com.", "id": "Stockman-Paul-Alan", "name": { "family": "Stockman", "given": "Paul Alan" }, "show_email": "NO" } ] }, "title": "Microwave and Far-Infrared Spectroscopy of Water-Containing, Hydrogen-Bonded Dimers: Vibrational, Rotational, and Tunneling Dynamics", "ispublished": "unpub", "full_text_status": "public", "keywords": "Chemistry", "abstract": "Microwave and far-infrared high-resolution spectroscopies have been used to investigate\r\nthe vibrational, rotational, and tunneling dynamics of water-containing, hydrogenbonded\r\ndimers, towards the goal of converting the recorded spectra into intermolecular\r\npotential energy surfaces (IPSs). Such intermolecular interactions are the basis for\r\nmuch of biological structure and function, as well as reaction and solution dynamics,\r\nand a comprehensive set of key IPSs can form the basis set for molecular modeling of\r\nthese complex phenomena. Specifically studied in this work are the following dimers\r\nand some of their isotopomers: N_2\u2022\u2022\u2022H_2O, OC\u2022\u2022\u2022H_2O, H_3N\u2022\u2022\u2022H_2O, CH_3OH\u2022\u2022\u2022H_2O.\r\nThese dimers constitute a series of increasing binding energy, dynamical complexity,\r\nand chemical and biological importance.
\r\n\r\nThe dimers of water with isoelectronic N_2 and CO are treated jointly because\r\nof their similar properties and level of study. The b-type K = 0 \u2192 1 rotational\r\nspectra for N_2\u2022\u2022\u2022H_2O and OC\u2022\u2022\u2022H_2O, as well as isotopomers containing HOD, D_2O,\r\nand ^(13)CO, were recorded between 325 and 661 GHz and measurements were also\r\nextended for the a-type spectra of the N_2\u2022\u2022\u2022H_2O and OC\u2022\u2022\u2022H_2O isotopomers. Each\r\nrotational transition was split by the effects of large-amplitude tunneling of the hydrogen\r\nand nitrogen nuclei, and the number of tunneling components corresponded\r\nwith that predicted from PI theory. After the effects of tunneling had been removed\r\nfrom the rotational constants, the structures of the two different complexes were fit\r\nto the rotational moments of inertia. These structures correspond to a nearly linear\r\nhydrogen bond and alignment of heavy atoms. The tunneling selection rules for\r\nOC\u2022\u2022\u2022H_2O were confirmed to be \"top-to-bottom, bottom-to-top,\" and the tunneling\r\nsplittings were obtained from the difference in the A_(eff) rotational constants. Using\r\ntwo- and three-term Fourier expansions, the one-dimensional tunneling coordinate\r\nwas fit to the tunneling splittings for OC\u2022\u2022\u2022H_2O and OC\u2022\u2022\u2022D_2O. Ab initio surfaces\r\nare used both to visualize the tunneling modes and as a basis for normal mode analyses. \r\nA reasonable and justified normal mode separation is presented, with the five\r\nintermolecular degrees of freedom separated into geared and anti-geared in-plane and\r\nout-of-plane motions of the the subunits as well as the intermolecular stretch. Finally,\r\npartial VRT spectra for both complexes recorded between 42 and 53 cm^(-1) are\r\npresented and preliminarily assigned to the in-plane geared motion.
\r\n\r\nMicrowave and far-infrared spectra of the H_3N\u2022\u2022\u2022H_2O dimer were recorded from\r\n36 to 86 GHz and 520 to 800 GHz. The a-type pure rotational microwave data extend\r\nthe previous m = 0,K = 0 A-symmetry manifold measurements of Herbine and Dyke\r\n[J. Chem. Phys. 83, 3768 (1980)] to higher frequency and also provide an additional\r\nset of microwave transitions in the mK = +1 E symmetry manifold. Two sets of five\r\nb-type rotation-tunneling bands one set shifted from the other by an approximately\r\nconstant 113 MHz, were observed in the far-infrared. The splitting into two sets arises\r\nfrom water tunneling, while the overall band structure is due to internal rotation of the\r\nammonia top. Non-linear least-squares fits to an internal rotor Hamiltonian provided\r\nrotational constants, and an estimation of V_3 = 10.5 \u00b15.0 cm^(-1) for the barrier height\r\nto internal rotation for the NH3 monomer. A non-linear equilibrium hydrogen bond is\r\nmost consistent with the vibrationally averaged rotational constants; with the angle\r\ncos^(-1) [\u3008\u03bb_z\u3009] determined from \u3008\u03bb_z\u3009, the projection of the ammonia's angular momentum\r\nonto the framework. The water tunneling splitting and observed selection rules place\r\nconstraints on the barrier height for proton exchange of the water as well as the most\r\nfeasible water tunneling path along the intermolecular potential energy surface. An\r\nestimated barrier of 700 cm^(-1) was derived for the water tunneling motion about its\r\nc axis.
\r\n\r\nFinally, microwave spectra of CH_3OH\u2022\u2022\u2022H-2O and CH_3OD\u2022\u2022\u2022D_2O were recorded\r\nbetween 20 and 60 GHz, along with data from our collaborators at the National Institute\r\nfor Science and Technology for CH_3OH\u2022\u2022\u2022H_2O, ^(13)CH_3OH\u2022\u2022\u2022H_2O, CH_3OH\u2022\u2022\u2022DOH,\r\nCD_3OH\u2022\u2022\u2022H_2O, and CH_3OD\u2022\u2022\u2022D_2O between 7 and 24 GHz. Because CH_3OH and\r\nH_2O are both capable of accepting and donating hydrogen bonds, there existed some\r\nquestion as to which donor-acceptor pairing of the molecules was the lowest energy\r\nform. This question is further emphasized by the ambiguity and variety present in\r\nprevious experimental and computational results. Transitions from the methyl torsional\r\nA state were assigned for the various isotopomers. The fit of the structure to\r\nthe rotational constants gave unambiguous confirmation that the only conformation\r\nobserved in the supersonically cooled molecular beams corresponded to a water-donor,\r\nmethanol-acceptor complex.
", "date": "1996", "date_type": "degree", "id_number": "CaltechTHESIS:11122012-111319894", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:11122012-111319894", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2012-11-13 16:53:58", "doi": "10.7907/PYV0-B286", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Zewail-A-H", "name": { "family": "Zewail", "given": "Ahmed H." }, "role": "chair" }, { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "id": "Gray-H-B", "name": { "family": "Gray", "given": "Harry B." }, "orcid": "0000-0002-7937-7876", "role": "member" }, { "id": "Okumura-M", "name": { "family": "Okumura", "given": "Mitchio" }, "orcid": "0000-0001-6874-1137", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1995-09-28", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1996", "author_list": "Stockman, Paul Alan" }, { "id": "/id/eprint/3770", "eprint_id": 3770, "rev_number": 10, "documents": [ { "id": "/id/document/6408", "doc_id": 6408, "rev_number": 3, "files": [ { "id": "/id/file/38434", "fileid": 38434, "datasetid": "document", "objectid": 6408, "filename": "Putney_a_1996.pdf", "mime_type": "application/pdf", "filesize": 29149505, "mtime": "2012-12-26 03:02:52", "url": "/3770/1/Putney_a_1996.pdf" } ], "eprint_id": 3770, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Putney_a_1996.pdf", "language": "en", "security": "public", "license": "other", "main": "Putney_a_1996.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22940" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22940" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22940" } ] } }, { "id": "/id/document/22940", "doc_id": 22940, "rev_number": 3, "files": [ { "id": "/id/file/38432", "fileid": 38432, "datasetid": "document", "objectid": 22940, "filename": "preview.png", "mime_type": "image/png", "hash": "45bad708366588603039787bae582fac", "hash_type": "MD5", "filesize": 8571, "mtime": "2012-12-26 03:02:52", "url": "/3770/2/preview.png" } ], "eprint_id": 3770, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6408" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6408" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6408" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/70", "datestamp": "2008-09-29", "lastmod": "2021-04-19 22:27:10", "status_changed": "2009-09-25 03:05:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Putney-A", "name": { "family": "Putney", "given": "Angela" }, "show_email": "NO" } ] }, "title": "Magnetic white dwarf stars", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\n\r\nThree aspects of magnetic white dwarf stars are studied to aid in the understanding of stellar evolution.\r\n\r\nA survey of ~ 50 DC white dwarf stars was conducted in circular spectropolarimetry to search for magnetic fields [...] 30 kG. Four DC stars were discovered with magnetic fields above 30 kG: G 111-49 with B[subscript e] ~ \u2014220 MG, G 183-35 with B[subscript e] = +6.8 \u00b1 0.5 MG, G 256-7 with B[subscript e] = +4.9 \u00b1 0.5 MG, and G 234-4 with B[subscript e] = +39.6 \u00b1 11.6 kG. A new magnetic DB white dwarf was also discovered, LB 8827 with B[subscript e] = 1.0 \u00b1 0.5 MG. A total of 15% of the white dwarfs in the survey have a magnetic field > 30 kG. This value is far larger than the 2% of DA stars, but more than half of the DC stars were originally misclassified. Only 5% of the re-classified DC stars have magnetic fields above 30 kG.\r\n\r\nThree magnetic stars from the DC white dwarf survey were re-observed to investigate the possibility of rotation. Two are definitely rotating: LHS 1734 with 16 min [...] P < 1 yr and G 158-45 (=LHS 1044) with a probable period P ~ 11 hr but a definite period P [...] 1 d or P ~ a few days. G 183-35 might be rotating with 50 min [...] P < a few yr. From all the white dwarf rotations known, it is clear that angular momentum is lost before a star becomes a white dwarf, but not clear that the loss is greatly enhanced by magnetic fields.\r\n\r\nThe isolated magnetic white dwarfs G 99-47, KUV 813-14 (KUV 23162-1220), and G 227-35 were observed in linear and circular spectropolarimetry and then compared to calculated theoretical spectra to find a model for the magnetic field strength and structure. The comparisons were to Stokes' V/I (circular polarization) spectra in addition to total flux F[...], and these add many constraints to the possible solutions. An off-centered dipole or a dipole+quadrupole configuration best fits the observations.\r\n\r\nThe results of the survey and the modeling are consistent with the theory that the magnetic Ap stars are the predecessors of magnetic white dwarfs.\r\n", "date": "1996", "date_type": "degree", "id_number": "CaltechETD:etd-09252008-135215", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09252008-135215", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-29", "doi": "10.7907/mq60-yx71", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-25", "thesis_defense_date": "1995-10-30", "thesis_approved_date": "2008-09-29", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1996", "author_list": "Putney, Angela" }, { "id": "/id/eprint/3313", "eprint_id": 3313, "rev_number": 21, "documents": [ { "id": "/id/document/5833", "doc_id": 5833, "rev_number": 4, "files": [ { "id": "/id/file/34596", "fileid": 34596, "datasetid": "document", "objectid": 5833, "filename": "Chakrabarty_d_1996.pdf", "mime_type": "application/pdf", "filesize": 10383310, "mtime": "2012-12-26 02:59:01", "url": "/3313/1/Chakrabarty_d_1996.pdf" } ], "eprint_id": 3313, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original scanned version Chakrabarty_d_1996.pdf", "language": "en", "security": "internal", "license": "other", "main": "Chakrabarty_d_1996.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/90918" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/90918" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/90918" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/13", "datestamp": "2008-09-10", "lastmod": "2020-03-10 23:09:59", "status_changed": "2009-09-25 02:56:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "deepto@mit.edu", "id": "Chakrabarty-Deepto", "name": { "family": "Chakrabarty", "given": "Deepto" }, "orcid": "0000-0001-8804-8946", "show_email": "YES" } ] }, "title": "Hard X-Ray Detection and Timing of Accretion-Powered Pulsars with BATSE", "ispublished": "unpub", "full_text_status": "public", "keywords": "Neutron Stars, Pulsars", "abstract": "The BATSE all-sky monitor on the Compton Gamma Ray Observatory is a superb tool for the study of accretion-powered pulsars. In the first part of this thesis, I describe its capabilities for hard X-ray observations above 20 keV, present techniques for timing analysis of the BATSE data, and discuss general statistical issues for the detection of pulsed periodic signals in both the time and frequency domains. BATSE's 1-day pulsed sensitivity in the 20-60 keV range is \u2248 15 mCrab for pulse periods 2 s \u2272 Ppulse \u2272 400 s, covering most of the known accreting pulsars. Its sensitivity degrades substantially outside of this range.
\r\n\r\nIn the second part of this thesis, I present the results of several science investigations applying these techniques. Half the 42 known accreting pulsars have been detected with BATSE and are monitored whenever they are active. Except for a few which lie outside of BATSE's sensitivity range, the rest are all transient sources which may eventually be detected in outburst. The detected systems include four new transients discovered by BATSE, one of which is discussed in detail. A new technique used to localize this source, GRO J1948+32, is described.
\r\n\r\nObservations of the 38-s pulsar OAO 1657-415 discovered that it is in a 10.4-d eccentric orbit and undergoes regular X-ray eclipses by its massive companion, making it only the seventh known eclipsing X-ray pulsar. Constraints placed by the pulsar mass function and the eclipse duration indicate that the undetected binary companion must be an OB supergiant. If the companion can be identified and its orbital velocity measured, the neutron star mass can be determined.
\r\n\r\nThe 7.7-s pulsar 4U 1626-67 was found to be in an extended spin-down state, ending over a decade of rapid, steady spin-up. It is only the second steady-state disk accreter known to have undergone a torque reversal. The other, the 2-min pulsar GX 1+4, underwent two torque reversals during our observations and is detected up to 160 keV. During spin-down, we find that pulsed flux and torque in GX 1+4 are anticorrelated, the opposite of what is predicted by the usual theories of magnetic accretion torques.
\r\n", "date": "1996", "date_type": "degree", "id_number": "CaltechETD:etd-09022008-132322", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09022008-132322", "related_url": { "items": [ { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1086/186715" }, { "description": "Article adapted for Chapter 5 and Appendix G.", "type": "doi", "url": "https://doi.org/10.1086/175839" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Graduate Student Research Program Fellowship", "grant_number": "NGT-51184" }, { "agency": "NSF" }, { "agency": "NASA Compton Observatory Guest Observer Program", "grant_number": "NAG 5-1458" }, { "agency": "NASA Long-Term Space Astrophysics Program", "grant_number": "NAGW-4517" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/6K2P-2A91", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-02", "thesis_defense_date": "1995-12-21", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1996", "author_list": "Chakrabarty, Deepto" }, { "id": "/id/eprint/3445", "eprint_id": 3445, "rev_number": 10, "documents": [ { "id": "/id/document/5980", "doc_id": 5980, "rev_number": 3, "files": [ { "id": "/id/file/35636", "fileid": 35636, "datasetid": "document", "objectid": 5980, "filename": "Yan_l_1996.pdf", "mime_type": "application/pdf", "filesize": 9014916, "mtime": "2012-12-26 02:59:57", "url": "/3445/1/Yan_l_1996.pdf" } ], "eprint_id": 3445, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Yan_l_1996.pdf", "language": "en", "security": "public", "license": "other", "main": "Yan_l_1996.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22520" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22520" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22520" } ] } }, { "id": "/id/document/22520", "doc_id": 22520, "rev_number": 3, "files": [ { "id": "/id/file/35634", "fileid": 35634, "datasetid": "document", "objectid": 22520, "filename": "preview.png", "mime_type": "image/png", "hash": "29307244df532ae5e4f07b64204c87e8", "hash_type": "MD5", "filesize": 7621, "mtime": "2012-12-26 02:59:57", "url": "/3445/2/preview.png" } ], "eprint_id": 3445, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5980" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5980" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5980" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/45", "datestamp": "2008-10-31", "lastmod": "2021-04-16 22:55:32", "status_changed": "2009-09-25 02:58:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yan-Lin", "name": { "family": "Yan", "given": "Lin" }, "orcid": "0000-0003-1710-9339", "show_email": "NO" } ] }, "title": "Binary stars in globular clusters", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThis thesis consists of several surveys to search for binary stars and to estimate the frequencies of binary populations in globular clusters. The motivations for these searches are that 1) binary populations (even with a fraction as small as 3%) dominate the dynamical evolution of a globular cluster by producing a tremendous amount of energy through stellar encounters; 2) binary stars provide important information for understanding several apparently different phenomena such as blue stragglers, millisecond pulsars and X-ray sources.\r\n\r\nTwo different techniques were employed in our surveys. The first survey is based on radial velocities obtained using the Norris Multi-fiber Spectrograph on the Palomar 200 inch telescope. We discovered 5 spectroscopic binary candidates among a total of 65 stars in the globular cluster NGC 5053. A total of 223 velocities were obtained for these 65 stars over a timespan of 3 years with a typical velocity error per measurement of 3 kms[...]. With detailed computer simulations we calculated the fraction of binaries which might have been missed in our detection sample due to unfavourable binary orbital configurations. Thus, we derived a binary frequency of 19-26% depending on the adopted period distribution function and orbital eccentricities.\r\n\r\nThe second part of this thesis utilized a different technique -- the analysis of time series photometry. This method is efficient in searching for eclipsing binaries with periods of a few days, as demonstrated in our surveys in the two globular clusters M 71 and M 5. We discovered a total of 11 eclipsing binaries in the clusters, with periods of 0.3-0.7 days. All variables are main-sequence stars except one in M 5, which is a possible blue straggler. Their light curves indicate that one variable in M 71 and one in M 5 are detached or semi-detached eclipsing binaries; the rest of the 11 systems are W UMa type contact binaries. Based on a simple model of the evolution of contact binaries from initially detached short-period binaries, we estimated a lower limit of 1.3% on the frequency of primordial binaries in M 71 with initial orbital periods of 2.5-5 days. This implies that the primordial binary frequency is 22% assuming a flat logarithmic period distribution. This frequency is for binaries with initial periods shorter than 800 years since any longer-period binaries would have been disrupted over the lifetime of the cluster. A similar calculation was done in M 5. Adopting a flat logarithmic period distribution and a contact binary lifetime of 3 Gyr, we estimated an overall primordial binary frequency of [...]% for systems with periods of 2.5 days to 550 yrs. The discovery of 11 short-period main-sequence eclipsing binaries for the first time provides strong physical evidence which supports the scenario that some blue stragglers are formed by mass transfer and mergers in short-period main-sequence binary systems.\r\n", "date": "1996", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-140218", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-140218", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-31", "doi": "10.7907/n04t-dp55", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1995-11-02", "thesis_approved_date": "2008-10-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1996", "author_list": "Yan, Lin" }, { "id": "/id/eprint/3595", "eprint_id": 3595, "rev_number": 9, "documents": [ { "id": "/id/document/6167", "doc_id": 6167, "rev_number": 3, "files": [ { "id": "/id/file/36890", "fileid": 36890, "datasetid": "document", "objectid": 6167, "filename": "Vasisht_g_1996.pdf", "mime_type": "application/pdf", "filesize": 13682252, "mtime": "2012-12-26 03:01:12", "url": "/3595/1/Vasisht_g_1996.pdf" } ], "eprint_id": 3595, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Vasisht_g_1996.pdf", "language": "en", "security": "public", "license": "other", "main": "Vasisht_g_1996.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22705" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22705" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22705" } ] } }, { "id": "/id/document/22705", "doc_id": 22705, "rev_number": 3, "files": [ { "id": "/id/file/36888", "fileid": 36888, "datasetid": "document", "objectid": 22705, "filename": "preview.png", "mime_type": "image/png", "hash": "92c38846ccc3afdff786e48034871a75", "hash_type": "MD5", "filesize": 8651, "mtime": "2012-12-26 03:01:12", "url": "/3595/2/preview.png" } ], "eprint_id": 3595, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6167" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6167" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6167" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/95", "datestamp": "2008-11-03", "lastmod": "2021-04-16 22:18:05", "status_changed": "2009-09-25 03:01:22", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vasisht-G", "name": { "family": "Vasisht", "given": "Gautam" }, "show_email": "NO" } ] }, "title": "Many faces of young neutron stars", "ispublished": "unpub", "full_text_status": "public", "abstract": "The hardware aspect of this thesis consists in the design, fabrication and assembly of twin analog Flexible Filter Banks at Caltech. These are user-friendly, workhorse, radio-pulsar search and timing instruments. Novel features include the flexibility in configuring channel center-frequencies and widths, the rapid sampling down to 25 \u03bcs and a total instrument bandwidth ranging from a narrow 0.2 MHz to a mammoth 100 MHz. Frequency synthesis is used to downconvert, detect and sample the telescope receiver bandpass as 32 separate time-series in each polarization. The collected data are later subjected to standard pulsar search and timing algorithms in software.\n\nThe vital scientific issue addressed here is the nature of young neutron stars. In the standard picture, young neutron stars are rapidly spinning radio-luminous pulsars, which may also display pulsed emission at high X-ray and \u03b3-ray energies. However there is no evidence that all neutron stars are born according to this standard picture. We present radio or X-ray investigations of steady nebular emission produced by three clearly non-standard and ill-understood objects. In all likelihood, these are young neutron stars, a notion upheld by their association with young Galactic supernova remnants.\n\nBased on its display of high energy transients, the soft \u03b3-ray repeater SGR 1806-20 is posited to be a seismically active \"magnetar\", i.e., a neutron star with a super-strong magnetic field (10[superscript 15] G) nearly three orders of magnitude greater than pulsar dipolar fields. Our VLA observations of fleeting small-scale structure around SGR 1806-20 provide intriguing, although preliminary, support for the magnetar model. In time, similar observations could unravel the riddle of soft \u03b3-ray repeaters and possibly establish the reality of magnetars.\n\nX-ray observations of the remnant of the historical supernova of 386 A.D., SNR G 11.2-0.3 are presented. The nature of an embedded underlumnious plerion discovered in these observations argues for a central neutron star very different from the prototypical Crab pulsar. The urgency to undertake a large scale study of young and hollow Galactic shells in broadband X-rays with fine spatial resolution is elucidated.\n\nX-ray spectroscopy of the object 1E 1207.4-5209 at the core of the large remnant PKS 1209-51/52 has revealed a non-thermal source with a very steep spectrum. After considering various scenarios for lE 1207.4-5209, we conclude that its spectral signature, its lack of optical emission and its position at the center of a supernova remnant make it a source similar to the mysterious anomalous X-ray pulsars.\n\nA large and sensitive search for radio pulsar companions of massive stars was undertaken. Primary motivation stems from the recent discovery of binary radio pulsar B 1259-63 as the first member of such a population and a \"missing link\" in the current models of evolution. Prevalent expectations, based on binary evolution scenarios, suggested that many more such systems should exist and would be uncovered in sensitive targeted searches. Together with other smaller searches, this survey uncovered no pulsars orbiting early-type stars. We conclude that such binary systems must be rare.\n", "date": "1996", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-100913", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-100913", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-03", "doi": "10.7907/m11k-ex13", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "1996-04-08", "thesis_approved_date": "2008-11-03", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1996", "author_list": "Vasisht, Gautam" }, { "id": "/id/eprint/3443", "eprint_id": 3443, "rev_number": 10, "documents": [ { "id": "/id/document/5978", "doc_id": 5978, "rev_number": 2, "files": [ { "id": "/id/file/35622", "fileid": 35622, "datasetid": "document", "objectid": 5978, "filename": "Hansen_bms_1996.pdf", "mime_type": "application/pdf", "filesize": 9845757, "mtime": "2012-12-26 02:59:57", "url": "/3443/1/Hansen_bms_1996.pdf" } ], "eprint_id": 3443, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Hansen_bms_1996.pdf", "language": "en", "security": "public", "license": "other", "main": "Hansen_bms_1996.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22518" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22518" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22518" } ] } }, { "id": "/id/document/22518", "doc_id": 22518, "rev_number": 2, "files": [ { "id": "/id/file/35620", "fileid": 35620, "datasetid": "document", "objectid": 22518, "filename": "preview.png", "mime_type": "image/png", "hash": "434daa50fac7211050437c1057a0ca54", "hash_type": "MD5", "filesize": 7768, "mtime": "2012-12-26 02:59:57", "url": "/3443/2/preview.png" } ], "eprint_id": 3443, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5978" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5978" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5978" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/43", "datestamp": "2008-10-31", "lastmod": "2019-12-21 02:17:12", "status_changed": "2009-09-25 02:58:29", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "hansen@astro.UCLA.EDU", "id": "Hansen-B-M-S", "name": { "family": "Hansen", "given": "Bradley Miles Stougaard" }, "show_email": "NO" } ] }, "title": "The ages, speeds and offspring of pulsars", "ispublished": "unpub", "full_text_status": "public", "abstract": "We investigate the cooling of low mass white dwarfs with helium cores. We construct a detailed numerical model using the most modern input physics, including our own calculations of low temperature hydrogen opacities. We use our models to constrain the ages of binary millisecond pulsars from the optical observations of their white dwarf companions. We use this to place limits on the initial spin periods, magnetic field decay times and accretion histories of the millisecond pulsars. Our models can also be used along with observations of spectroscopic gravities and radial velocities to place interesting constraints on the neutron star equation of state. We provide grids of temperature and luminosity as a function of age for various white dwarf masses and surface compositions to facilitate future analyses.\r\n\r\nWe have investigated the effect of the pulsar wind on the atmospheric composition of binary companions. The spallation of atmospheric helium to hydrogen increases the cooling age of the white dwarf. We find that all white dwarf companions in binaries with orbital period < 300 days should cool as DA (hydrogen surface layer) white dwarfs, irrespective of their original hydrogen content. We investigate the effect of various wind compositions and note that, if almost all the hydrogen on the surface of a pulsar companion is the result of spallation of an ionic wind, then the D/H ratio is large.\r\n\r\nWe investigate the processes by which planets might form around a millisecond pulsar such as PSR B1257+12. We study the evolution of accretion disks of different mass, angular momentum and composition, corresponding to various proposed formation scenarios. We find that most formation scenarios require a high efficiency of conversion of metal-rich material into planets if they are to produce the observed parameters of the 1257+12 planetary system.\r\n\r\nWe have studied the distribution of pulsar proper motions in the light of the recent analysis of Lyne & Lorimer (1994). Using a simulation of the selection effects of the various surveys, and treating the censored data using survival statistics, we arrive at an estimate of the characteristic pulsar birth velocity ~ 300 km.s[superscript -1], 2/3 that of Lyne & Lorimer. We also show that the older pulsar population shows the effects of the asymmetric drift, indicating that it must be dynamically old.\r\n", "date": "1996", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-134917", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-134917", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-31", "doi": "10.7907/69DE-D262", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1996-05-23", "thesis_approved_date": "2008-10-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1996", "author_list": "Hansen, Bradley Miles Stougaard" }, { "id": "/id/eprint/4171", "eprint_id": 4171, "rev_number": 10, "documents": [ { "id": "/id/document/6871", "doc_id": 6871, "rev_number": 3, "files": [ { "id": "/id/file/41711", "fileid": 41711, "datasetid": "document", "objectid": 6871, "filename": "Ray_ps_1995.pdf", "mime_type": "application/pdf", "filesize": 4701782, "mtime": "2012-12-26 03:06:03", "url": "/4171/1/Ray_ps_1995.pdf" } ], "eprint_id": 4171, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Ray_ps_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Ray_ps_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23402" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23402" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23402" } ] } }, { "id": "/id/document/23402", "doc_id": 23402, "rev_number": 3, "files": [ { "id": "/id/file/41709", "fileid": 41709, "datasetid": "document", "objectid": 23402, "filename": "preview.png", "mime_type": "image/png", "hash": "4a5cd7e478ac65245d802f50e8825343", "hash_type": "MD5", "filesize": 17972, "mtime": "2012-12-26 03:06:03", "url": "/4171/2/preview.png" } ], "eprint_id": 4171, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6871" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6871" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6871" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/41/71", "datestamp": "2007-11-02", "lastmod": "2021-04-16 22:27:01", "status_changed": "2009-09-25 03:12:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ray-Paul-Shelton", "name": { "family": "Ray", "given": "Paul Shelton" }, "show_email": "NO" } ] }, "title": "High-sensitivity searches for radio pulsars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Radio pulsars are rapidly spinning, highly magnetized neutron stars which emit beams of radio waves and are observed to pulse when the beam crosses the Earth. They represent the end-point in the evolution of massive stars, and are excellent laboratories for the study of the bulk properties of matter at nuclear densities and beyond. Millisecond pulsars are old pulsars reborn through accretion of matter from a companion star, spinning so fast that the surface velocities approach the speed of light.\r\n\r\nWe describe several high-sensitivity searches for radio pulsars, both for very recently born pulsars in supernova remnants and for ancient millisecond pulsars born early in the history of the Galaxy.\r\n\r\nWe have conducted a survey of 18 supernova remnants for young pulsars using the 305-m radio telescope in Arecibo, Puerto Rico at 430 MHz and 1400 MHz. No pulsars were discovered in this survey which was sensitive to pulsars as faint as 0.2 mJy. The selection effects making pulsars difficult to find in supernova remnants, including high background temperatures of the remnants and high birth velocities of pulsars, are discussed. We conclude that deeper and more extensive surveys are required to constrain the pulsar population in supernova remnants.\r\n\r\nWe have also performed several very large area surveys with excellent sensitivity to pulsars as fast as 1 millisecond, also employing the Arecibo 305-m dish. These surveys will help place limits on the population of low-luminosity pulsars in the Galaxy. A total of 12 non-recycled pulsars were discovered with periods ranging from 96 ms to 2.06 seconds.\r\n\r\nThe primary motivation for these surveys was the discovery of new millisecond pulsars. One 5.9 ms pulsar was discovered and initial timing observations show that it is in a binary system with orbital period 56.2 d and semi-major axis 20.1 lt-s. The implied companion mass is at least 0.2 solar masses. This pulsar, as well as a number of others discovered in recent surveys, are providing excellent laboratories for studies of the formation and evolution of millisecond pulsars, as well as measurements of general relativistic parameters, constraints on the cosmological background of gravitational waves, a pulsar based time standard and dynamical-optical frame ties.\r\n", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-10182007-151414", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10182007-151414", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-11-02", "doi": "10.7907/6m41-p432", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-10-18", "thesis_defense_date": "1995-01-11", "thesis_approved_date": "2007-11-02", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Ray, Paul Shelton" }, { "id": "/id/eprint/4216", "eprint_id": 4216, "rev_number": 7, "documents": [ { "id": "/id/document/6943", "doc_id": 6943, "rev_number": 3, "files": [ { "id": "/id/file/42163", "fileid": 42163, "datasetid": "document", "objectid": 6943, "filename": "Rauch_kp_1995.pdf", "mime_type": "application/pdf", "filesize": 20483410, "mtime": "2012-12-26 03:06:35", "url": "/4216/1/Rauch_kp_1995.pdf" } ], "eprint_id": 4216, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Rauch_kp_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Rauch_kp_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23474" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23474" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23474" } ] } }, { "id": "/id/document/23474", "doc_id": 23474, "rev_number": 3, "files": [ { "id": "/id/file/42161", "fileid": 42161, "datasetid": "document", "objectid": 23474, "filename": "preview.png", "mime_type": "image/png", "hash": "fb4707361597fbbc5812a703d30b713c", "hash_type": "MD5", "filesize": 10453, "mtime": "2012-12-26 03:06:35", "url": "/4216/2/preview.png" } ], "eprint_id": 4216, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6943" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6943" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6943" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/16", "datestamp": "2007-11-07", "lastmod": "2021-04-16 22:13:39", "status_changed": "2009-09-25 03:13:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rauch-K-P", "name": { "family": "Rauch", "given": "Kevin Patrick" }, "show_email": "NO" } ] }, "title": "Black holes and accretion disks in active galactic nuclei : microlensing, caustics, and collisional stellar dynamics", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nInteractions between and the structure of black holes, accretion disks, and dense star clusters are investigated. Observed rapid gravitational microlensing variability in the quasar Q2237+0305 is used in conjunction with numerical simulations of microlensed quasar accretion disks to determine whether the observations constrain theoretical accretion disk models. It is found that blackbody disks are at least three times too large to account for the observed variability, and on that basis it is argued that the optical emission is either nonthermal or optically thin.\r\n\r\nAccurate, efficient, and general-purpose routines to compute geodesic trajectories in the Kerr spacetime describing rotating black holes are implemented and applied to several problems. The optical caustic structure of the Kerr metric describing rotating black holes is determined and its possible relevance to rapid X-ray variability in active galactic nuclei is discussed. It is found that the (primary) caustic is a small tube with an asteroid cross section which extends behind the black hole asymptotically parallel to the optic axis but displaced from it by an amount proportional to the spin of the hole, and that the angular magnification is unexpectedly high everywhere inside the caustic. Sample point source light curves and the appearance of thick accretion disks around Kerr black holes are calculated and the influence of caustics on them is assessed.\r\n\r\nThe dynamical evolution of the core of a dense star cluster around a Kerr black hole and under the influence of star-disk interactions is examined. It is shown that there are astrophysically plausible regimes in which star-disk interactions can dominate all other dynamical processes. The effects of star-disk interactions on single orbits are illustrated. It is found that star-disk interactions steepen the initial density profile towards an equilibrium [...] profile and simultaneously increase the central density by up to two orders of magnitude. It is argued that this process could self limit when densities climb to such a level that collisions between stars become important.\r\n\r\nSimulations of the dynamical evolution of the density cusp of a star cluster around a massive black hole in a regime where stellar collisions dominate other dynamical processes are performed. The calculations are done using a discrete cluster of stars and a fully relativistic formalism. Versatile numerical methods are developed and applied to this problem. A modified form of Kepler's Equation asymptotically valid in the Kerr geometry is derived. It is found that collisions produce a constant density core which is mainly populated by stars on highly radial orbits, in contrast to previous Fokker-Planck analyses in which an [...] profile has been found. Collisional refilling of the loss cone is seen. Additional applications of the numerical algorithms are suggested.\r\n", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-10222007-142133", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10222007-142133", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-11-07", "doi": "10.7907/cpyq-cr33", "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_committee": { "items": [ { "email": "rdb@tapir.caltech.edu", "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "chair" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-10-22", "thesis_defense_date": "1994-08-31", "thesis_approved_date": "2007-11-07", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Rauch, Kevin Patrick" }, { "id": "/id/eprint/3472", "eprint_id": 3472, "rev_number": 7, "documents": [ { "id": "/id/document/6015", "doc_id": 6015, "rev_number": 3, "files": [ { "id": "/id/file/35863", "fileid": 35863, "datasetid": "document", "objectid": 6015, "filename": "Apostolatos_ta_1995.pdf", "mime_type": "application/pdf", "filesize": 8932474, "mtime": "2012-12-26 03:00:12", "url": "/3472/1/Apostolatos_ta_1995.pdf" } ], "eprint_id": 3472, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Apostolatos_ta_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Apostolatos_ta_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22555" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22555" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22555" } ] } }, { "id": "/id/document/22555", "doc_id": 22555, "rev_number": 3, "files": [ { "id": "/id/file/35861", "fileid": 35861, "datasetid": "document", "objectid": 22555, "filename": "preview.png", "mime_type": "image/png", "hash": "ae6e8db19b4017ade591a2c0bbacb891", "hash_type": "MD5", "filesize": 13277, "mtime": "2012-12-26 03:00:12", "url": "/3472/2/preview.png" } ], "eprint_id": 3472, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6015" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6015" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6015" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/72", "datestamp": "2007-09-18", "lastmod": "2021-04-16 23:10:50", "status_changed": "2009-09-25 02:58:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Apostolatos-T-A", "name": { "family": "Apostolatos", "given": "Theocaris A." }, "show_email": "NO" } ] }, "title": "Topics in general relativity : naked singularities, and theoretical aspects of gravitational waves from merging compact binaries", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nTwo topics in classical general relativity are discussed: a) The clothing of singularities by event horizons, and b) various issues in the evolution of coalescing compact binaries, as sources of gravitational waves to be detected by the LIGO/VIRGO/GEO ground-based detectors and/or the LISA space-based detector. More specifically:\r\n\r\nWe investigate a problem related to an important conjecture of classical relativity, namely the existence of a \"cosmic censorship\" that forbids the formation of naked singularities, and always clothes them with event horizons that causally hide them from the rest of the Universe. Under consideration is the role of rotation in an infinite cylindrical shell consisting of collisionless dust particles, half of which rotate clockwise and half counterclockwise. We show that, although such a shell without any rotation is known to collapse into a line singularity, the presence of an arbitrarily small amount of rotation is sufficient to halt the collapse. Such a shell, starting from a non equibrium configuration, will \"breath\" radially, emitting gravitational waves, and will finally settle down to an equilibrium radius at which gravity is balanced by centrifugal forces. This suggests the essential role that rotation might play in halting the gravitational collapse of an elongated distribution of mass and preventing the formation of a naked singularity. However, this is a highly idealized example, and it can, by no means, ensure the validity of the \"cosmic censorship\" hypothesis.\r\n\r\nOn a separate topic, we explore the details of how gravitational radiation reaction drives the evolution of a slightly eccentric orbit of a small body around nonrotating supermassive black holes. A combination of analytic and numerical results arise from the solution of the Teukolsky perturbation equation. It is shown that in the fully relativistic situation, as in the Newtonian quadrupole approximation, there is a tendency for circularization of the orbit down to an orbital radius [...], where M is the mass of the black hole, and G and c are Newton's gravitation constant and the speed of light. It is further shown that for radii smaller than [...] the eccentricity increases.\r\n\r\nFinally, an attempt is made to understand and construct analytic expressions that, based on the laws of general relativity, approximately describe the simultaneous precession in rapidly spinning black hole and/or neutron star and inspiral binaries with circular orbits. The precession is produced by general relativistic spin-orbit and spin-spin coupling; the inspiral, by gravitational radiation reaction. We derive the corresponding approximate waveforms to be received by the network of LIGO, VIRGO, and GEO earth-based gravitational-wave detectors. We then go on to investigate the adequateness of various \"families of templates,\" to detect these spin-modulated waveforms by the method of \"matching filters,\" We introduce a \"fitting factor\" FF as a measure of templates' adequateness, and show the complete inadequateness, for the task of detection, of the \"Newtonian template family\" (the set of the waveforms derived from the Newtonian, quadrupole approximation formalism). Another template family with an extra parameter is suggested that performs much better.", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-09112007-132644", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09112007-132644", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-09-18", "doi": "10.7907/2x5m-b994", "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_committee": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-09-11", "thesis_defense_date": "1994-11-01", "thesis_approved_date": "2007-09-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Apostolatos, Theocaris A." }, { "id": "/id/eprint/4221", "eprint_id": 4221, "rev_number": 13, "documents": [ { "id": "/id/document/6948", "doc_id": 6948, "rev_number": 3, "files": [ { "id": "/id/file/42206", "fileid": 42206, "datasetid": "document", "objectid": 6948, "filename": "Schoelkopf_rj_1995.pdf", "mime_type": "application/pdf", "filesize": 7226391, "mtime": "2012-12-26 03:06:38", "url": "/4221/1/Schoelkopf_rj_1995.pdf" } ], "eprint_id": 4221, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Schoelkopf_rj_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Schoelkopf_rj_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23479" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23479" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23479" } ] } }, { "id": "/id/document/23479", "doc_id": 23479, "rev_number": 3, "files": [ { "id": "/id/file/42204", "fileid": 42204, "datasetid": "document", "objectid": 23479, "filename": "preview.png", "mime_type": "image/png", "hash": "a73ad2e2a4b66e09835cb9d6873ad84e", "hash_type": "MD5", "filesize": 10550, "mtime": "2012-12-26 03:06:37", "url": "/4221/2/preview.png" } ], "eprint_id": 4221, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6948" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6948" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6948" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/21", "datestamp": "2007-11-07", "lastmod": "2021-04-19 22:26:47", "status_changed": "2009-09-25 03:13:53", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schoelkopf-Robert-J", "name": { "family": "Schoelkopf", "given": "Robert J." }, "show_email": "NO" } ] }, "title": "Studies of noise in Josephson-effect mixers and their potential for submillimeter heterodyne detection", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThis thesis describes both theoretical and experimental investigations into the dynamics and noise processes of Josephson junctions, with the intent of evaluating their potential as mixers in heterodyne instruments for submillimeter-wave (i.e., the frequency range from 300 GHz to 3THz) detection. Superconducting tunnel junctions utilizing the nonlinearity due to photon-assisted tunneling of quasiparticles (SIS mixers) have become the state-of-the-art technology for sensitive heterodyne detection up to frequencies of about 700 [...]. Recent progress in the fabrication of high [...], superconductors has led to Josephson-effect devices with [...] products of up to ten millivolts, which might be suitable for mixing at frequencies of many terahertz. The key question for weighing the prospects for high-frequency Josephson mixers is that of the sensitivity which can be attained.\r\n\r\n\tPrevious experimental work on Josephson mixing suggests the existence of an \"excess\" noise, which degrades the sensitivity. Theoretical modeling of mixer performance, based on the resistivelyshunted junction (RSJ) model for the dynamics of the device, also indicates the presence of larger noise than expected. The origin of this noise was not clearly understood, however, nor was its exact magnitude or expected scaling with frequency or junction characteristics known. In addition, previous experiments utilized crude devices of the point-contact type, which were unstable and thus undesirable for real applications.\r\n\r\n\tIn the first part of this thesis research, extensive numerical simulations were performed with the RSJ model, including calculations of mixer noise and conversion efficiency. These calculations have revealed that the source of excess noise is the AC Josephson oscillations of the device, which can be completely incoherent, with a linewidth comparable to their frequency. Thus they appear as a broadband noise source. While this noise is intrinsic and unavoidable, an optimized mixer is still shown to be capable of interesting sensitivity levels, and the excess noise is expected to become relatively less important as the operating frequency is increased.\r\n\r\n\tSecondly, a process has been developed for the fabrication of stable, well-characterized, and reproducible Josephson devices based on resistively-shunted Nb and NbN tunnel junctions. The devices utilize submicron-area, high current-density tunnel junctions and a AuGe shunt resistor to yield completely non-hysteretic I-V curves, normal-state resistances of about [...] products of about half a millivolt. These devices should be nearly optimal for mixing at [...].\r\n\r\n\tHeterodyne measurements using these junctions have been performed in a waveguide mixer mount. Receiver temperatures as low as 190 K (DSB), with -6 dB conversion efficiency, have been obtained at 100 [...], but these results are still a factor of about four higher than those predicted by the RSJ simulations. Accurate measurements of the available noise power of the junctions at the intermediate frequency of 1.5 [...] were made, and confirmed that the receivers were limited by elevated junction output noise. The deviations of the noise from theoretical predictions are shown to be caused by the nonlinear interaction of the junction with the embedding circuit. While this work points out some of the complexity introduced by the strong nonlinearity of Josephson devices, it is still expected that Josephson-effect mixers may be useful for heterodyne detection at very high frequencies.\r\n", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-10232007-104241", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10232007-104241", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-11-07", "doi": "10.7907/xezv-q641", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-10-23", "thesis_defense_date": "1994-11-01", "thesis_approved_date": "2007-11-07", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Schoelkopf, Robert J." }, { "id": "/id/eprint/4239", "eprint_id": 4239, "rev_number": 8, "documents": [ { "id": "/id/document/6973", "doc_id": 6973, "rev_number": 3, "files": [ { "id": "/id/file/42361", "fileid": 42361, "datasetid": "document", "objectid": 6973, "filename": "Thompson_dj_1995.pdf", "mime_type": "application/pdf", "filesize": 5506078, "mtime": "2012-12-26 03:06:48", "url": "/4239/1/Thompson_dj_1995.pdf" } ], "eprint_id": 4239, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Thompson_dj_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Thompson_dj_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23504" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23504" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23504" } ] } }, { "id": "/id/document/23504", "doc_id": 23504, "rev_number": 3, "files": [ { "id": "/id/file/42359", "fileid": 42359, "datasetid": "document", "objectid": 23504, "filename": "preview.png", "mime_type": "image/png", "hash": "8d31a6f278f29e9d216aff7948860490", "hash_type": "MD5", "filesize": 7717, "mtime": "2012-12-26 03:06:48", "url": "/4239/2/preview.png" } ], "eprint_id": 4239, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6973" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6973" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6973" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/39", "datestamp": "2007-11-07", "lastmod": "2021-04-16 22:18:24", "status_changed": "2009-09-25 03:14:34", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Thompson-D", "name": { "family": "Thompson", "given": "David" }, "show_email": "NO" } ] }, "title": "Surveys for primeval galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nWe present the results from two complementary surveys for young and forming ellipticals or spheroids at high redshift, one based on a narrowband imaging technique using a Fabry-Perot interferometer, and the other a serendipitous long-slit spectroscopic survey.\n\nThe Fabry-Perot survey is sensitive to Lya emission in four discrete redshift ranges: z = 2.80 - 2.98, 3.27 - 3.45, 4.42 - 460, and 4.75 - 4.89. The total area of the survey was 0.63 [...], surveyed to a 1[...] limiting line flux of [...] 8.5 x [...] erg [...]. An area of 0.05 [...] was surveyed to a fainter flux limit of [...] 1.5 x [...] erg [...]. A total comoving volume of 110,000 [...] was surveyed to a [...] limiting restframe emission line luminosity of [...] 2.0 x [...] erg [...] (a Friedman cosmology with [...] = 75 km [...] Mpc[...] and [...] = 0.2 is assumed throughout this thesis).\n\nThe long-slit survey is sensitive to [...] in the range of 3.1 [...] 5.2, with lesser areas surveyed across the entire optical passband. A total of 421 independent spectroscopic frames were searched, covering an area of 0.0042 [...] (14.97 arcmin[...]). 65 emission-line candidates were identified, including 30 galaxies with [...] and 2 quasars. An additional 20 objects were assigned tentative redshifts, all \nwith [...], and have properties consistent with the galaxies seen in the deep field redshift surveys. The remaining objects are candidate [...] galaxies at high red-shift, with isolated, unidentified emission lines and little or no continuum. They require further spectroscopy to check on their nature. A total comoving volume of 102,600 [...] was surveyed to a [...] limiting restframe emission line luminosity of [...] erg [...].\n\nIn neither case was an obvious population of primeval galaxies revealed, despite the combined surveys covering a volume of space sufficient to include [...] 200 galaxies with [...] (using the local space density of massive galaxies, and assuming no density evolution). These galaxies could have been detected if they were unobscured by dust and were actively forming stars at a rate of 100 [...]. A \nnumber of candidates remain to be followed up with spectroscopic observations, and may yet prove to be the elusive PGs. The lack of detection of a population of [...]-luminous objects could be due to dust quenching of the [...] line, a higher redshift of formation than surveyed, short lifetime in the [...]-bright phase, or even masking of the star-formation emission-line signature by an active nucleus. \n\nA study on the feasibility of conducting primeval galaxy surveys in the near infrared, based on emission-lines of [0 II], [0 III], and the Balmer lines, and the results of a preliminary survey based on these techniques, are also presented. It is shown that the new large-format infrared arrays will reach the necessary sensitivities over large enough areas to make such surveys practical.", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-10242007-142316", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10242007-142316", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-11-07", "doi": "10.7907/b644-y527", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-10-24", "thesis_defense_date": "1994-10-24", "thesis_approved_date": "2007-11-07", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Thompson, David" }, { "id": "/id/eprint/4256", "eprint_id": 4256, "rev_number": 9, "documents": [ { "id": "/id/document/6996", "doc_id": 6996, "rev_number": 3, "files": [ { "id": "/id/file/42506", "fileid": 42506, "datasetid": "document", "objectid": 6996, "filename": "Weir_n_1995.pdf", "mime_type": "application/pdf", "filesize": 30942618, "mtime": "2012-12-26 03:06:58", "url": "/4256/1/Weir_n_1995.pdf" } ], "eprint_id": 4256, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Weir_n_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Weir_n_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23526" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23526" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23526" } ] } }, { "id": "/id/document/23526", "doc_id": 23526, "rev_number": 3, "files": [ { "id": "/id/file/42504", "fileid": 42504, "datasetid": "document", "objectid": 23526, "filename": "preview.png", "mime_type": "image/png", "hash": "484a99f45ee11eb51fc7dcc30ae74de0", "hash_type": "MD5", "filesize": 13575, "mtime": "2012-12-26 03:06:58", "url": "/4256/2/preview.png" } ], "eprint_id": 4256, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6996" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6996" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6996" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/56", "datestamp": "2007-10-25", "lastmod": "2021-04-16 23:14:13", "status_changed": "2009-09-25 03:14:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Weir-W-N", "name": { "family": "Weir", "given": "William Nicholas" }, "show_email": "NO" } ] }, "title": "Automated analysis of the Digitized Second Palomar Sky Survey : system design, implementation, and initial results", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nWe describe the design, implementation, and initial scientific results of a system for analyzing the Digitized Second Palomar Observatory Sky Survey (DPOSS). The system (SKICAT) facilitates and largely automates the pipeline processing of DPOSS from raw pixel data into calibrated, classified object catalog form.\r\n\r\nA fundamental constraint limiting the scientific usefulness of optical imaging surveys is the level at which objects may be reliably distinguished as stars, galaxies, or artifacts. We therefore expended great effort to explore techniques that would make most efficient use of the data for classification purposes. The classifier implemented within SKICAT was created using a new machine learning technology, whereby an algorithm determines a near-optimal set of classification rules based upon training examples. Using this approach, we were able to construct a classifier which distinguishes objects to the same level of accuracy as in previous surveys using comparable plate material, but nearly one magnitude fainter (or an equivalent [...]). \r\n\r\nOur first analysis of DPOSS using SICAT is of an overlapping set of four survey fields near the North Galactic Pole, in both the J and F passbands. Through detailed simulations of a subset of these data, we were able to analyze systematic aspects of our detection and measurement procedures, as well as optimize them. We discuss how we calibrate the plate magnitudes to the Gunn-Thuan g and r photometric system using CCD sequences obtained in a program devoted expressly to calibrating DPOSS. Our technique results in an estimated plate-to-plate zero point standard error of under [...] in g and below [...] in r, for J and F plates, respectively.\r\n\r\nUsing the catalogs derived from these fields, we compare our differential galaxy counts in g and r with those from recent Schmidt plate surveys as well as predictions from evolutionary and non-evolutionary (NE) galaxy models. While we find some significant differences between our measurements and others, particularly at the bright end, we find generally good agreement between our counts and recent NE and mild evolutionary models calibrated to consistently fit bright and faint galaxy counts, colors, and redshift distributions. The consistency of our results with these predictions provides additional support to the view that very recent (z < 0.1) or exotic galaxy evolution, or some non-standard forms of cosmology, may not be necessary to reconcile these diverse observations with theory.\r\n", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-10252007-081840", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10252007-081840", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-10-25", "doi": "10.7907/wdng-9x48", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-10-25", "thesis_defense_date": "1994-01-21", "thesis_approved_date": "2007-10-25", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Weir, William Nicholas" }, { "id": "/id/eprint/4272", "eprint_id": 4272, "rev_number": 13, "documents": [ { "id": "/id/document/7012", "doc_id": 7012, "rev_number": 3, "files": [ { "id": "/id/file/42628", "fileid": 42628, "datasetid": "document", "objectid": 7012, "filename": "Xu_w_1995.pdf", "mime_type": "application/pdf", "filesize": 12298460, "mtime": "2012-12-26 03:07:05", "url": "/4272/1/Xu_w_1995.pdf" } ], "eprint_id": 4272, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Xu_w_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Xu_w_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23542" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23542" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23542" } ] } }, { "id": "/id/document/23542", "doc_id": 23542, "rev_number": 3, "files": [ { "id": "/id/file/42626", "fileid": 42626, "datasetid": "document", "objectid": 23542, "filename": "preview.png", "mime_type": "image/png", "hash": "2abb9b85903656e343ebf00e9d8bd59c", "hash_type": "MD5", "filesize": 8012, "mtime": "2012-12-26 03:07:05", "url": "/4272/2/preview.png" } ], "eprint_id": 4272, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7012" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7012" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7012" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/72", "datestamp": "2007-11-13", "lastmod": "2021-11-05 22:40:50", "status_changed": "2009-09-25 03:15:14", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Xu-Wenge", "name": { "family": "Xu", "given": "Wenge" }, "show_email": "NO" } ] }, "title": "The first Caltech-Jodrell Bank VLBI survey", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThis thesis presents the author's major contributions to the first Caltech-Jodrell Bank VLBI survey (CJ1). It demonstrates convincingly that the VLBI snapshot technique is a reliable and highly efficient method of making images of large samples of objects.\r\n\r\nThe CJ1 sample consists of 135 objects with 1.3 Jy > [...] GHz [...] 0.7 Jy, [...](1950) [...] 35\u00b0 and [...] > 10\u00b0. The combination of the CJ1 sample with the Pearson-Readhead sample provides a complete, flux density limited sample of 200 objects with [...] GHZ [...] 0.7 Jy, [...](1950) [...] 35\u00b0 and [...] > 10\u00b0 for which all of the objects accessible to Mark II VLBI have been mapped at both 5 GHz and 1.6 GHz. In this thesis we present the 5 GHz VLBI observations from the CJ1 survey and follow-up observations of 8 compact symmetric objects (CSO) or CSO candidates at 8.4 GHz. In addition, we present 5 GHz MERLIN observations of 20 objects and 1.4 GHz VLA observations of 92 objects in the CJ1+PR sample. The VLA maps, together with L band (1.3-1.7 GHz) maps available in the literature, provide a complete set of VLA maps for the CJ1+PR sample. Furthermore, we present new redshifts, optical counterparts and optical polarimetry measurements of the objects in the CJ1 sample.\r\n\r\nBased on morphological attributes on scales < 5 kpc and [...] 5 kpc, we identify six physically distinct classes in the CJ1+PR sample, one of which is the CSO class. Identification of CSO's may have a profound impact on our understanding of AGN. Detailed study of one archetypal CSO, 2352+495, has demonstrated that the CSO's are likely a class of short-lived powerful galaxies.\r\n\r\nWe have confirmed the bimodal distribution of the misalignment angle and identified that the peak near 90\u00b0 is contributed by a group of objects with high optical polarization, high fractional core flux, high radio variability and flat radio spectrum. All of these are symptoms of relativistic beaming.\r\n\r\nThe mean angular sizes of the CJ1+PR objects show only slight dependence on redshift, contrary to the finding by Kellermann. However, our results show that the angular size distributions of objects with z < 0.1 and those with z > 0.1 are significantly different. This may indicate an evolutionary effect.\r\n", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-10262007-132906", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10262007-132906", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-11-13", "doi": "10.7907/k8f8-gn20", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-10-26", "thesis_defense_date": "1994-12-01", "thesis_approved_date": "2007-11-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Xu, Wenge" }, { "id": "/id/eprint/1911", "eprint_id": 1911, "rev_number": 9, "documents": [ { "id": "/id/document/3277", "doc_id": 3277, "rev_number": 3, "files": [ { "id": "/id/file/19546", "fileid": 19546, "datasetid": "document", "objectid": 3277, "filename": "Peri_ml_1995.pdf", "mime_type": "application/pdf", "filesize": 7047983, "mtime": "2012-12-26 02:44:03", "url": "/1911/1/Peri_ml_1995.pdf" } ], "eprint_id": 1911, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Peri_ml_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Peri_ml_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19969" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19969" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19969" } ] } }, { "id": "/id/document/13341", "doc_id": 13341, "rev_number": 3, "files": [ { "id": "/id/file/202085", "fileid": 202085, "datasetid": "document", "objectid": 13341, "filename": "Peri_ml_1995.txt", "mime_type": "text/plain", "filesize": 1945, "mtime": "2016-08-22 21:15:19", "url": "/1911/2/Peri_ml_1995.txt" } ], "eprint_id": 1911, "pos": 2, "format": "text/plain", "format_desc": "Author OK 2011", "language": "en", "security": "internal", "license": "other", "main": "Peri_ml_1995.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/19969", "doc_id": 19969, "rev_number": 2, "files": [ { "id": "/id/file/19544", "fileid": 19544, "datasetid": "document", "objectid": 19969, "filename": "preview.png", "mime_type": "image/png", "hash": "bf69cd4b6b55b5a2e21d8528ede96e5b", "hash_type": "MD5", "filesize": 13260, "mtime": "2012-12-26 02:44:02", "url": "/1911/3/preview.png" } ], "eprint_id": 1911, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3277" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3277" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3277" } ] } }, { "id": "/id/document/121576", "doc_id": 121576, "rev_number": 1, "files": [ { "id": "/id/file/366968", "fileid": 366968, "datasetid": "document", "objectid": 121576, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "4cc8c0f61bdf4e544245418996620ed0", "hash_type": "MD5", "filesize": 902, "mtime": "2021-06-23 21:30:16", "url": "/1911/4/indexcodes.txt" } ], "eprint_id": 1911, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/13341" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13341" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13341" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/19/11", "datestamp": "2004-05-21", "lastmod": "2019-12-21 01:56:53", "status_changed": "2009-09-25 02:19:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "michal@alumni.caltech.edu", "id": "Peri-M-L", "name": { "family": "Peri", "given": "Michal Leah" }, "show_email": "NO" } ] }, "title": "Asteroseismological observations of eta Cassiopeiae A with the Palomar east arm echelle spectrograph", "ispublished": "unpub", "full_text_status": "public", "keywords": "asteroseismology, stellar oscillations, doppler spectroscopy\r\nechelle spectrograph, Palomar observatory, Palomar 200\", telescope, fiber optic feed, eta Cassiopeiae A", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nAsteroseismology is the study of acoustic oscillations in stars. Such oscillations probe the stellar interior, and thus carry information on the physical conditions in regions of the star that are not accessible through ordinary observational techniques. Oscillations have not yet been measured for any star other than the Sun, however, because they are quite small. The solar p-modes generate Doppler shifts of [...], as well as variations [...] in surface intensity. Theory predicts that the corresponding variations will be at most a few times larger in other solar-type stars. The goal of this thesis is to extend the methods of asteroseismology to the levels where one can reasonably expect to detect oscillations on solar-type stars.\r\n\r\nDoppler spectroscopy is the preferred method for asteroseismological observations. The fundamental limitations on sensitivity imposed by photon noise can be alleviated by looking at bright stars with large telescopes and by observing a large number of spectral lines simultaneously. The observations require high resolution over a broad wavelength regime with excellent stability on the short timescales [...] associated with p-mode periodicities.\r\n\r\nTo obtain such observations, this project began with the design and construction of a new high-resolution spectrometer for Palomar 200\" Hale Telescope. The East Arm Echelle Spectrograph, which is coupled by optical fiber to prime focus, produces a resolution of [...] over most of the visible spectrum. The design was optimized for making high-precision radial velocity measurements, incorporating fiber-optic double scrambling for enhanced stability and a molecular iodine absorption cell for Doppler calibration. To enhance utility to other astronomical applications, the instrument also offers a low-resolution mode with R=20000.\r\n\r\nSpecialized data reduction software was developed to compensate for the echelle order curvature and spectral line tilt. The analysis code extracts spectral Doppler shift, carefully isolating the stellar signal from atmospheric perturbation and instrumental instabilities. The algorithms were designed to be robust and automated for processing large numbers of frames required for asteroseismological timeseries.\r\n\r\nInstrumental performance was assessed from timeseries of solar radial velocity measurements. The spectrograph readily measures motion associated with the Earth's rotation. Configured for asteroseismology observations, the instrument demonstrated an rms sensitivity of 1.14 m/s per frame over [...] 1/2 hour timescales. This precision is within a factor of [...] 2 of the photon noise limit attainable for single measurements, indicating the instrument provides excellent stability over timescales associated with stellar acoustic oscillations.\r\n\r\nIn August 1993 we obtained a six-night timeseries of observations on the solar twin [eta] Cas. The measurements carried an rms radial velocity scatter of [...] 3 m/s per 60 second exposure. The power spectrum derived from this data showed a mean power spectral density corresponding to a Doppler amplitude of 10.8 cm/s over the frequency range 450-4450 [...]. Unfortunately, we found no clear evidence of p-mode oscillations. Interpretation of the data is complicated by the lack of specific predictions for the star's seismicity. Nevertheless, we set a very conservative threshold for the absence of oscillations at a Doppler amplitude of 30-35 cm/s.\r\n\r\nThis limit represents a very substantial gain over previous asteroseismological observations. The [eta] Cas results push the state of the art by factor of two, on a much fainter star than had been previously observed. This accomplishment increases the number of stars that can be reasonably targeted for study by an order of magnitude. Our conservative threshold lies well within the range of acoustic behavior predicted for main-sequence dwarf stars and is the first to approach the level of precision required to observe pulsations of solar amplitude. Although we did not see p-modes in [eta] Cas, we believe that the methodology developed in this thesis is capable of detecting asteroseismological phenomena on other solar-type candidate stars.", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-05212004-105738", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05212004-105738", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-21", "doi": "10.7907/VKRJ-A345", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-21", "thesis_defense_date": "1994-06-21", "thesis_approved_date": "2004-05-21", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Peri, Michal Leah" }, { "id": "/id/eprint/4346", "eprint_id": 4346, "rev_number": 19, "documents": [ { "id": "/id/document/7104", "doc_id": 7104, "rev_number": 3, "files": [ { "id": "/id/file/43274", "fileid": 43274, "datasetid": "document", "objectid": 7104, "filename": "McMuldroch_s_1995.pdf", "mime_type": "application/pdf", "filesize": 6352429, "mtime": "2012-12-26 03:07:44", "url": "/4346/1/McMuldroch_s_1995.pdf" } ], "eprint_id": 4346, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "McMuldroch_s_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "McMuldroch_s_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/46531" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/46531" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/43/46", "datestamp": "2007-11-13", "lastmod": "2023-11-08 00:16:43", "status_changed": "2009-09-25 03:16:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "McMuldroch-Stuart", "name": { "family": "McMuldroch", "given": "Stuart" }, "show_email": "NO" } ] }, "title": "The Circumstellar Environments of FU Orionis Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science", "abstract": "Extensive observations were made of six FU Orionis objects (RNO 1B/1C, V1057 Cygni, Elias 1-12, V1515 Cygni and FU Orionis) and one pre-outburst candidate (V1331 Cygni) using the Owens Valley millimeter-wave array and the Caltech Submillimeter Observatory (CSO). Aperture synthesis maps of CO (1\u21920), \u00b9\u00b3CO (1\u21920), \u00b9\u00b3CO (2\u21921), \u00b9\u2078CO (1\u21920), and \u00b3CO (2\u21921) molecular lines and associated dust continuum emission trace the masses, kinematics and morphology of FU Orionis disks, envelopes, and outflows. Maps from the CSO delineate outflowing gas at larger spatial scales while line strengths, when input into radiative transfer models, yield column densities and fractional chemical abundances.
\r\n\r\nUnresolved 1.3 mm continuum emission from Vl331 Cygni and V1057 Cygni reveal massive circumstellar disks of 0.5 and 0.09 M\u2609, respectively. Maps of the 2.6 and 3.1 mm continuum emission reveal that RNO 1C is surrounded by a flattened dusty envelope, 5000 AU in size, with mass \u2a7e 1.1 M\u2609. No evidence is seen for multiple systems with orbital periods \u2273 4 x 10\u2074 years years.\r\n\r\nAll sources, with the exception of RNO 1B/1C are surrounded by large molecular gas envelopes between 2000-7500 AU in size, with masses ranging from 2 x 10\u207b\u00b3 to 0.36 M\u2609. Aperture synthesis maps suggest the envelopes are asymmetrically distributed. Gas kinematics around V1057 Cygni and Elias 1-12 suggest, but do not demand, that this material is rotating and possibly infalling.
\r\n\r\nOf the seven sources observed, all but FU Orionis show signs of outflowing molecular gas. No high velocity clumps or \"bullets\" are seen towards any of the sources. V1331 Cygni, V1057 Cygni, and V1515 Cygni possess arc or ring-like outflow morphologies, while emission from RNO 1B/1C and Elias 1-12 delineates filled outflow shells. All emission patterns are consistent with outflow shells being viewed at different angles. Although based on the statistics of small numbers, observations suggest shells are seen more frequently around FUors than T Tauri stars. Shell formation may therefore be caused by time-dependent events in the outflow. Cross-cutting arcs within the shell structure, seen towards RNO 1B/1C and Elias 1-12, are probably ridges of gas swept-up by the most recent outbursts, confirming the repetitive nature of FUor outbursts. Estimates of the dynamical ages of the arcs suggest that the interval between outbursts is ~5 x 10\u00b3 and 1.3 x 10\u2074 years for RNO 1B/1C and Elias 1-12 respectively, consistent with previous estimates of FUor cycling times.
\r\n\r\nComparable envelopes and shell-like outflow structure are seen towards embedded sources while envelopes surrounding T Tauri stars are smaller and less massive. This suggests FU Orionis objects are transition sources between deeply embedded and optically visible stars. The strength of the molecular outflow emission is correlated with the mass of the extended envelope; the outflow has evacuated molecular gas leaving less to be swept-up by subsequent outbursts, while envelope masses are smaller since less material is available for accretion.
\r\n\r\nChemically, fractional abundances of SiO and methanol are enhanced towards RNO 1B/1C by over an order of magnitude. Methanol is enhanced relative to HCN and H2CO towards Elias 1-12. Such large changes in fractional abundances must be caused by chemical processing. The SiO enrichments may be produced by sputtering or evaporation of dust grains in regions of directly shocked material or by chemical reactions of SiH4 after sublimation from grain surfaces. Methanol enrichments are difficult to produce in strong shocks, and may be caused by low velocity grain-grain collisions. For RNO 1B/1C, evaporation of the entire methanol rich grain mantles seems to be required; while for Elias 1-12 mantle phase changes from an amorphous ice to a clathrate hydrate can be invoked, expelling the methanol, with smaller molecules remaining trapped in the clathrate. Such low velocity collisions probably occur in the turbulent shear zones surrounding the outflowing gas.
", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-10312007-094538", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10312007-094538", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-11-13", "doi": "10.7907/14NE-ZW09", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "advisor" }, { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "id": "Westphal-J-A", "name": { "family": "Westphal", "given": "James A." }, "role": "chair" }, { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "co-chair" }, { "id": "Burnett-D-S", "name": { "family": "Burnett", "given": "Donald S." }, "role": "member" }, { "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "member" }, { "id": "Muhleman-D-O", "name": { "family": "Muhleman", "given": "Duane Owen" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-10-31", "thesis_defense_date": "1994-10-28", "thesis_approved_date": "2007-11-13", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "McMuldroch, Stuart" }, { "id": "/id/eprint/4347", "eprint_id": 4347, "rev_number": 11, "documents": [ { "id": "/id/document/7105", "doc_id": 7105, "rev_number": 3, "files": [ { "id": "/id/file/43281", "fileid": 43281, "datasetid": "document", "objectid": 7105, "filename": "Koerner_dw_1995.pdf", "mime_type": "application/pdf", "filesize": 4981212, "mtime": "2012-12-26 03:07:45", "url": "/4347/1/Koerner_dw_1995.pdf" } ], "eprint_id": 4347, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Koerner_dw_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Koerner_dw_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23634" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23634" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23634" } ] } }, { "id": "/id/document/23634", "doc_id": 23634, "rev_number": 3, "files": [ { "id": "/id/file/43279", "fileid": 43279, "datasetid": "document", "objectid": 23634, "filename": "preview.png", "mime_type": "image/png", "hash": "35701615b41ff9ad6d72ba8ed8b74459", "hash_type": "MD5", "filesize": 8039, "mtime": "2012-12-26 03:07:45", "url": "/4347/2/preview.png" } ], "eprint_id": 4347, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7105" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7105" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7105" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/43/47", "datestamp": "2007-11-13", "lastmod": "2021-04-19 22:38:16", "status_changed": "2009-09-25 03:16:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Koerner-David", "name": { "family": "Koerner", "given": "David" }, "show_email": "NO" } ] }, "title": "The kinematics of circumstellar disks around T Tauri stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Astronomy", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nAperture synthesis images of molecular gas around the T Tauri stars, GM Aurigae, RY Tauri, DL Tauri, DO Tauri, and AS 209 are interpreted with the aid of a kinematic model of a circumstellar disk. The velocity structure and morphology of the gas strongly suggest that circumstellar disks with radii of a few hundred AU are present around all five stars. Explicit identification of kinematic patterns in the spectral line maps is achieved for the two largest disks, GM Aur and DO Tau.\r\n\r\nMaps of the relatively old T Tauri star, GM Aur, in the [...] line at 4\" resolution reveal compact gas associated with the stellar position and at the core of a larger rotating gaseous disk, 950 x 530 AU in extent. The mean velocity gradient across the disk, which is oriented along [...], is consistent with rotation about an axis at [...]. The structure observed in [...] aperture synthesis maps agrees well with synthetic maps of the gas emission generated from a model. For a disk that is inclined [...] from face on, in Keplerian rotation, a 0.80 [...] central mass (star + disk), a systemic velocity, [...], of 15.38 km [...] and a mass, 0.1 [...] is derived.\r\n\r\nA survey of T Tauri stars for circumstellar molecular gas also yields evidence for rotating disks. RY Tau, DL Tau, DO Tau, and AS 209 are detected in CO[...] emission elongated along [...], respectively, with deconvolved half-maximum radii of 110, 250, 350, and 290 AU in aperture synthesis images at [...] resolution. Three of these, RY Tau, DL Tau, and AS 209, exhibit velocity gradients parallel to this direction in first moment velocity maps, suggesting rotation of the circumstellar gas. Spectra of RY Tau and AS 209 exhibit a characteristic double-peaked shape, but that of DO Tau is dominated by the presence of high-velocity blue-shifted gas. DL Tau's spectrum has a linewidth that is too narrow [...] to be resolved into double peaks. Position-Velocity Diagrams (PVDs) constructed parallel and perpendicular to the axis of elongation imply rotation and infall or outflow, respectively. Those for RY Tau, DL Tau, and AS 209 show predominantly rotation, but some evidence of an orthogonal gradient (infall or outflow) is seen for RY Tau and AS 209. In contrast, the PVDs for DO tau suggest that its molecular emission originates predominantly from outflow or infall.\r\n\r\nRecent evidence of infall in circumstellar gas around T Tauri stars has motivated construction of a kinematic model of molecular emission from a disk of rotating and infalling gas. The velocity structure of the model disk assumes that infalling gas obeys angular momentum conservation on ballistic trajectories until it reaches the radial value, [...], where the magnitude of the rotational velocity component reaches the Keplerian value. For [...], gas is assumed to be in circular Keplerian orbits. Synthetic spectral line maps are generated by the model and cross-correlated with aperture synthesis maps for a range of the free parameters, including [...]. The best-fit value of [...] for RY Tau, DL Tau, and AS 209, approximately matches that of the outer radius of their emission, indicating these disks are predominantly in Keplerian rotation. However, emission from these stars is marginally resolved and uncertainties in the best-fit parameters are correspondingly high. In contrast, kinematic patterns are well-resolved in emission from DO Tau found in maps within a narrow, near-systemic velocity range. These are best matched by simulations from a model disk with [...] = 350 AU and an outer radius of 500 AU. This result strongly suggests that, in this case, infall from the molecular cloud onto a rotating disk is still in progress.\r\n", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-10312007-162008", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10312007-162008", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-11-13", "doi": "10.7907/css3-2v20", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "role": "chair" }, { "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "id": "Beckwith-S-V-W", "name": { "family": "Beckwith", "given": "Steve V. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-10-31", "thesis_defense_date": "1994-09-13", "thesis_approved_date": "2007-11-13", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Koerner, David" }, { "id": "/id/eprint/1059", "eprint_id": 1059, "rev_number": 13, "documents": [ { "id": "/id/document/1624", "doc_id": 1624, "rev_number": 3, "files": [ { "id": "/id/file/10121", "fileid": 10121, "datasetid": "document", "objectid": 1624, "filename": "Groesbeck_td_1995.pdf", "mime_type": "application/pdf", "filesize": 12358555, "mtime": "2012-12-26 02:34:58", "url": "/1059/1/Groesbeck_td_1995.pdf" } ], "eprint_id": 1059, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Groesbeck_td_1995.pdf", "language": "en", "security": "public", "license": "other", "main": "Groesbeck_td_1995.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18404" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18404" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18404" } ] } }, { "id": "/id/document/18404", "doc_id": 18404, "rev_number": 3, "files": [ { "id": "/id/file/10119", "fileid": 10119, "datasetid": "document", "objectid": 18404, "filename": "preview.png", "mime_type": "image/png", "hash": "5da5602bae8476c246896122b0778d4b", "hash_type": "MD5", "filesize": 11595, "mtime": "2012-12-26 02:34:58", "url": "/1059/2/preview.png" } ], "eprint_id": 1059, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1624" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/1624" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1624" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/10/59", "datestamp": "2006-03-22", "lastmod": "2021-10-27 22:23:45", "status_changed": "2009-09-25 01:54:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Groesbeck-Todd Dickson", "name": { "family": "Groesbeck", "given": "Todd Dickson" }, "show_email": "NO" } ] }, "title": "The Contribution of Molecular Line Emission to Broadband Flux Measurements at Millimeter and Submillimeter Wavelengths", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "We present measurements of the ratio of flux carried by molecular emission lines to the total flux observed from six astronomical sources in the 330-360 GHz frequency range, demonstrating that the integrated line emission can represent a significant fraction, and in some cases even the majority, of the total flux observed. Given the narrow widths of these emission lines for most sources in the interstellar medium, it has generally been assumed that the contribution of the integrated lines would be negligible when compared to the continuum flux measured by a very broadband instrument. We extend the previous work by Sutton et al. (1984), which demonstrated that line emission was responsible for a large part of the total flux observed from Orion-KL, by presenting observations at higher frequencies of Orion-KL and several additional sources. These observations provide the most comprehensive determination of the ratio of line flux to continuum flux yet made at submillimeter wavelengths.
\r\n\r\nWe have performed spectral line surveys of the star-forming regions Orion-KL, Orion-S, and IRAS 16293-2422, and the evolved stars IRC +10216, VY Canis Majoris, and OH 231.8+4.2. Observations for Orion-KL and IRC +10216 give continuous frequency coverage over approximately the 330-360 GHz band; for the other sources the coverage ranges between 30 and 60% of the same frequency band. Comparisons of the line survey data with total flux measurements demonstrates that the contribution of the integrated line emission to the total flux at these frequencies ranges from as low as ~10% for Orion-S and IRAS 16293-2422 to at least ~60% for Orion-KL and IRC +10216. We also estimate the amount of flux carried in weak lines below our sensitivity limits \r\nbased on the observed distributions of line intensities.
\r\n\r\nAn improved deconvolution method has been used to obtain a single sideband spectrum from the double sideband observations. We have also developed computer versions of line catalogs which allow immediate line identification and analysis, assuming conditions of local thermodynamic equilibrium (LTE) prevail. The same catalog programs also permit simulation of emission line spectra for arbitrary molecular abundances and excitation temperatures, again assuming LIE. For each of the observed sources, we present simulations of the spectrum from 0 to 1000 GHz, using molecular parameters derived from our data and additional published observations. In all cases, the simulations indicate that the relative importance of the line emission decreases at higher frequencies (~ > 700 GHz). We discuss the significance of these findings regarding the determination of dust parameters from broadband flux measurements, concluding that such measurements must be corrected for possible line flux contributions before they can be reliably used.
", "date": "1995", "date_type": "degree", "id_number": "CaltechETD:etd-03222006-103422", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03222006-103422", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-03-22", "doi": "10.7907/rbaq-gb42", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "orcid": "0000-0003-0787-1610", "role": "member" }, { "id": "Carlstrom-J-E", "name": { "family": "Carlstrom", "given": "John E." }, "role": "member" }, { "id": "Kavanagh-R-W", "name": { "family": "Kavanagh", "given": "Ralph William" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-03-22", "thesis_defense_date": "1994-09-09", "thesis_approved_date": "2006-03-22", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1995", "author_list": "Groesbeck, Todd Dickson" }, { "id": "/id/eprint/3437", "eprint_id": 3437, "rev_number": 9, "documents": [ { "id": "/id/document/5972", "doc_id": 5972, "rev_number": 3, "files": [ { "id": "/id/file/35575", "fileid": 35575, "datasetid": "document", "objectid": 5972, "filename": "Lee_j_1994.pdf", "mime_type": "application/pdf", "filesize": 5956598, "mtime": "2012-12-26 02:59:54", "url": "/3437/1/Lee_j_1994.pdf" } ], "eprint_id": 3437, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Lee_j_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Lee_j_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22512" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22512" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22512" } ] } }, { "id": "/id/document/22512", "doc_id": 22512, "rev_number": 3, "files": [ { "id": "/id/file/35573", "fileid": 35573, "datasetid": "document", "objectid": 22512, "filename": "preview.png", "mime_type": "image/png", "hash": "8a5c00fffd1e102af7a2937f406457df", "hash_type": "MD5", "filesize": 9571, "mtime": "2012-12-26 02:59:54", "url": "/3437/2/preview.png" } ], "eprint_id": 3437, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5972" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5972" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5972" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/37", "datestamp": "2008-09-18", "lastmod": "2021-04-16 22:21:01", "status_changed": "2009-09-25 02:58:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lee-Jeo", "name": { "family": "Lee", "given": "Jeongwoo" }, "show_email": "NO" } ] }, "title": "Study of solar microwave radiation using multifrequency data", "ispublished": "unpub", "full_text_status": "public", "abstract": "I have carried out analysis of multifrequency data of solar microwave radiation gathered by the frequency-agile telescope at Owens Valley Radio Observatory to address several long-standing problems in the study of active region structure and solar flare particles.\r\n\r\nIn the study of active region structure, I use the microwave data and the magnetograms of NOAA 4741 obtained during 1986 August 2 - 9 to discover: (i) change of dominant radiation mechanism with the coronal height, (ii) angle-dependent properties of the gyroresonance opacity, (iii) distribution of the coronal magnetic fields and its implication for the force balance in the upper atmosphere of the active region. The merit of this study lies in the fact that most results are empirical and thus provide an observational basis to test theoretical sunspot models and the gyromagnetic radiation theory.\r\n\r\nIn the flare study, I deal with impulsive bursts and extended bursts, aiming at two issues: (i) the physical link between microwaves and hard X-rays in impulsive bursts and (ii) influence of ambient plasma on the evolution of extended microwave activity. The first issue has been addressed by a kinetic approach made to deduce the distribution of microwave-emitting electrons and hard X-ray electrons in momentum space, referring to the 1989 March 18 flare in NOAA 5395. For the second issue, I analyse data of extended microwave bursts on 1990 May 24 (NOAA 6063), 1991 March 7 and 8 (NOAA 6538), and 1991 March 22 (NOAA 6555) in terms of a nonuniform coronal trap model to deduce source conditions responsible for the observed anomalies of extended bursts. These data sets and results of analysis underline the influence of the source condition on the spectral and temporal evolution of microwave radiation during solar flares.\r\n", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-092806", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-092806", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-18", "doi": "10.7907/1vr9-wh15", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1993-10-21", "thesis_approved_date": "2008-09-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Lee, Jeongwoo" }, { "id": "/id/eprint/7688", "eprint_id": 7688, "rev_number": 17, "documents": [ { "id": "/id/document/38107", "doc_id": 38107, "rev_number": 3, "files": [ { "id": "/id/file/118250", "fileid": 118250, "datasetid": "document", "objectid": 38107, "filename": "Markovic 1994.zip", "mime_type": "application/x-zip", "hash": "00a16114c694c42573e7f40eba759d20", "hash_type": "MD5", "filesize": 79347143, "mtime": "2013-05-09 15:49:59", "url": "/7688/1/Markovic 1994.zip" } ], "eprint_id": 7688, "pos": 1, "placement": 1, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Markovic 1994.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"datestamp": "2013-05-09 16:04:31", "lastmod": "2022-11-09 19:20:00", "status_changed": "2013-05-09 16:04:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Markovi\u0107-D", "name": { "family": "Markovi\u0107", "given": "Dragoljub" }, "show_email": "NO" } ] }, "title": "Black holes in the early universe, in compact binaries, and as energy sources inside solar-type stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis consists of three separate studies of roles that black holes might\r\nplay in our universe.
\r\n\r\nIn the first part we formulate a statistical method for inferring the cosmological\r\nparameters of our universe from LIGO/VIRGO measurements of the gravitational\r\nwaves produced by coalescing black-hole/neutron-star binaries. This method is\r\nbased on the cosmological distance-redshift relation, with \"luminosity distances\"\r\ndetermined directly, and redshifts indirectly, from the gravitational waveforms.\r\nUsing the current estimates of binary coalescence rates and projected \"advanced\"\r\nLIGO noise spectra, we conclude that by our method the Hubble constant should\r\nbe measurable to within an error of a few percent. The errors for the mean density\r\nof the universe and the cosmological constant will depend strongly on the size of\r\nthe universe, varying from about 10% for a \"small\" universe up to and beyond\r\n100% for a \"large\" universe. We further study the effects of random gravitational\r\nlensing and find that it may strongly impair the determination of the cosmological\r\nconstant.
\r\n\r\nIn the second part of this thesis we disprove a conjecture that black holes cannot\r\nform in an early, inflationary era of our universe, because of a quantum-field-theory induced\r\ninstability of the black-hole horizon. This instability was supposed to arise\r\nfrom the difference in temperatures of any black-hole horizon and the inflationary\r\ncosmological horizon; it was thought that this temperature difference would make\r\nevery quantum state that is regular at the cosmological horizon be singular at\r\nthe black-hole horizon. We disprove this conjecture by explicitly constructing a\r\nquantum vacuum state that is everywhere regular for a massless scalar field. We\r\nfurther show that this quantum state has all the nice thermal properties that one\r\nhas come to expect of \"good\" vacuum states, both at the black-hole horizon and\r\nat the cosmological horizon.
\r\n\r\nIn the third part of the thesis we study the evolution and implications of a hypothetical\r\nprimordial black hole that might have found its way into the center of the\r\nSun or any other solar-type star. As a foundation for our analysis, we generalize\r\nthe mixing-length theory of convection to an optically thick, spherically symmetric\r\naccretion flow (and find in passing that the radial stretching of the inflowing fluid\r\nelements leads to a modification of the standard Schwarzschild criterion for convection).\r\nWhen the accretion is that of solar matter onto the primordial hole, the\r\nrotation of the Sun causes centrifugal hangup of the inflow near the hole, resulting\r\nin an \"accretion torus\" which produces an enhanced outflow of heat. We find, however, that the turbulent viscosity, which accompanies the convective transport\r\nof this heat, extracts angular momentum from the inflowing gas, thereby buffering\r\nthe torus into a lower luminosity than one might have expected. As a result, the\r\nsolar surface will not be influenced noticeably by the torus's luminosity until at\r\nmost three days before the Sun is finally devoured by the black hole. As a simple\r\nconsequence, accretion onto a black hole inside the Sun cannot be an answer to\r\nthe solar neutrino puzzle.
\r\n", "date": "1994", "date_type": "degree", "id_number": "CaltechTHESIS:05092013-084229368", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05092013-084229368", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_on": "2013-05-09 16:04:31", "doi": "10.7907/ms5q-kt36", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1994-02-28", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Markovi\u0107, Dragoljub" }, { "id": "/id/eprint/836", "eprint_id": 836, "rev_number": 12, "documents": [ { "id": "/id/document/1255", "doc_id": 1255, "rev_number": 3, "files": [ { "id": "/id/file/7891", "fileid": 7891, "datasetid": "document", "objectid": 1255, "filename": "Banfield_dj_1994.pdf", "mime_type": "application/pdf", "filesize": 11402692, "mtime": "2012-12-26 02:32:50", "url": "/836/1/Banfield_dj_1994.pdf" } ], "eprint_id": 836, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Banfield_dj_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Banfield_dj_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18057" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18057" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18057" } ] } }, { "id": "/id/document/18057", "doc_id": 18057, "rev_number": 3, "files": [ { "id": "/id/file/7889", "fileid": 7889, "datasetid": "document", "objectid": 18057, "filename": "preview.png", "mime_type": "image/png", "hash": "e9474f6fdde68aa5977edfa010e4d836", "hash_type": "MD5", "filesize": 23007, "mtime": "2012-12-26 02:32:50", "url": "/836/2/preview.png" } ], "eprint_id": 836, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1255" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/1255" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1255" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/08/36", "datestamp": "2006-03-03", "lastmod": "2021-04-16 22:13:35", "status_changed": "2009-09-25 01:47:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Banfield-Donald-J", "name": { "family": "Banfield", "given": "Donald J." }, "show_email": "NO" } ] }, "title": "A dynamical history of the inner Neptunian satellites and Martian weather : Viking observations and M.O. data assimilation techniques", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Applied Physics", "abstract": "We examine a scenario involving the capture origin of Triton, and infer the dynamical history of the Neptune satellite system. Triton's post-capture orbit forced chaotic perturbations on the original inner satellites of Neptune, leading to their mutual collisions and self-destruction. Neptune's current inner satellite system re-formed equatorially after Triton's orbital circularization. The 4.7\u00b0 inclination of 1989N6 is probably due to a temporary inclination resonance. The 2:1 secondary resonance of the 1989N6-1989N3 12:10 resonance would eject 1989N6 at 4.7\u00b0, matching the observations. We have established limits for Neptune's Q: 12,000 < QN < 330,000.\r\n\r\nWe examine a steady-state scheme for data assimilation in the context of a single, sun-synchronous, polar-orbiting satellite. The optimal (Wiener) gains are steady in time, and equivalent to those of a Kalman filter. The gains are computed by iteration using prior estimates to assimilate simulated observations of one model run ('Truth') into another run. The resulting prediction errors then form the next estimate of the gains. In model tests, the scheme works well even if only the mass field is observed. Although the scheme was developed for Mars Observer, it should be applicable to data retrieved from Earth atmosphere satellites, e.g., UARS.\r\n\r\nSpring and fall Viking IRTM T15 observations are used to estimate the Martian weather correlation length scale in the range 0.5-1 mbar. The results are important in providing a benchmark for validating Martian GCMs, determining the optimal placement of a network of landers, and guiding data assimilation efforts. Atmospheric temperature observations are used to compute an atmospheric mean state, which is subtracted from the observations to yield weather temperature residuals. These residuals are correlated with each other to determine the weather temperature correlation length scale (~ 1500km) and the weather temperature variance (~ 4-11K2). This work suggests that ~110 landers are needed to globally observe Mars' weather.", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-03022006-132818", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03022006-132818", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-03-03", "doi": "10.7907/07dr-qq38", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-03-02", "thesis_defense_date": "1993-12-10", "thesis_approved_date": "2006-03-03", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "appliedphys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Banfield, Donald J." }, { "id": "/id/eprint/3435", "eprint_id": 3435, "rev_number": 9, "documents": [ { "id": "/id/document/5970", "doc_id": 5970, "rev_number": 3, "files": [ { "id": "/id/file/35561", "fileid": 35561, "datasetid": "document", "objectid": 5970, "filename": "Navarro_j_1994.pdf", "mime_type": "application/pdf", "filesize": 7706691, "mtime": "2012-12-26 02:59:54", "url": "/3435/1/Navarro_j_1994.pdf" } ], "eprint_id": 3435, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Navarro_j_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Navarro_j_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22510" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22510" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22510" } ] } }, { "id": "/id/document/22510", "doc_id": 22510, "rev_number": 3, "files": [ { "id": "/id/file/35559", "fileid": 35559, "datasetid": "document", "objectid": 22510, "filename": "preview.png", "mime_type": "image/png", "hash": "ef4138926bb09121ee47f34260414930", "hash_type": "MD5", "filesize": 7344, "mtime": "2012-12-26 02:59:53", "url": "/3435/2/preview.png" } ], "eprint_id": 3435, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5970" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5970" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5970" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/35", "datestamp": "2008-09-18", "lastmod": "2021-04-16 22:25:59", "status_changed": "2009-09-25 02:58:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Navarro-J", "name": { "family": "Navarro", "given": "Jose" }, "show_email": "NO" } ] }, "title": "A wide bandwidth pulsar timing machine", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nPulsar timing has turned millisecond pulsars into powerful tools for the study of neutron star physics, time-keeping, astrometry, the interstellar medium and binary systems. It uses millisecond pulsars as probes of the gravitational fields of their companions, of globular clusters and of the Galaxy, and provides information on the dynamics of the solar system. It has also confirmed predictions of general relativity, for which Joe Taylor and Russell Hulse received the 1993 Nobel Prize in Physics. Vasts amounts of information are expected as the current searches continue to discover new millisecond pulsars.\n\nThis thesis describes the design and construction of the Caltech Fast Pulsar Timing Machine and some preliminary results at the Parkes Observatory. The FPTM is a wide band timing machine built around a digital correlator for long-term timing stability and has a large observing bandwidth to time millisecond pulsars at high radio frequencies, where propagation effects are minimized.\n\nIt is the combination of the 128 MHz bandwidth. the 512 lag digital correlator and the 1024 period phase bins with a minimum size of 2.7 [...] that gives the FPTM its power. The large bandwidth makes new observations of faint pulsars possible above 1 GHz, where current receivers easily provide radio signals with more than 100 MHz of bandwidth. The large number of channels reduces the dispersion smearing of distant millisecond pulsars, which often defines the timing floor in timing systems, and the 1024 phase bins of 2.7 [...] or more ensure that the pulsar profile is adequately sampled.\n\nThe FPTM is currently at Parkes Observatory, in Australia, where we are undertaking a long-term precision timing program for millisecond pulsars. We frequently observe the bright binary millisecond pulsar J0437-4715 with sub-microsecond times-of-arrival, and have already found interesting features in the pulse profile that could not be resolved with previous timing systems. Nevertheless, we still find drifts in the timing residuals of as much as a few [...] over several hours which we do not yet understand (even though they are also seen by the other timing system at Parkes!). We are confident that we will solve these residuals and consistently time PSR J0437-4715 at the level of 100 ns or better.\n\nWe also present the discovery of J0218+4232, a very luminous binary field millisecond pulsar. Its 2.3 ms pulsations were only detected after an exhaustive search that involved building new hardware.\n", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-091511", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-091511", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-18", "doi": "10.7907/x08x-cm32", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1994-05-27", "thesis_approved_date": "2008-09-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Navarro, Jose" }, { "id": "/id/eprint/3440", "eprint_id": 3440, "rev_number": 16, "documents": [ { "id": "/id/document/5975", "doc_id": 5975, "rev_number": 3, "files": [ { "id": "/id/file/35599", "fileid": 35599, "datasetid": "document", "objectid": 5975, "filename": "Roth_j_1994.pdf", "mime_type": "application/pdf", "filesize": 9915525, "mtime": "2012-12-26 02:59:56", "url": "/3440/1/Roth_j_1994.pdf" } ], "eprint_id": 3440, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Roth_j_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Roth_j_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22515" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22515" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22515" } ] } }, { "id": "/id/document/22515", "doc_id": 22515, "rev_number": 3, "files": [ { "id": "/id/file/35597", "fileid": 35597, "datasetid": "document", "objectid": 22515, "filename": "preview.png", "mime_type": "image/png", "hash": "dd147edb876f6be8742e45b1ac51b886", "hash_type": "MD5", "filesize": 9001, "mtime": "2012-12-26 02:59:55", "url": "/3440/2/preview.png" } ], "eprint_id": 3440, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5975" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5975" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5975" } ] } }, { "id": "/id/document/51872", "doc_id": 51872, "rev_number": 3, "files": [ { "id": "/id/file/150350", "fileid": 150350, "datasetid": "document", "objectid": 51872, "filename": "JoshuaRoth_1994_Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "ac23f381800fd21f220acc2b99705a8e", "hash_type": "MD5", "filesize": 1028, "mtime": "2014-09-08 21:43:26", "url": "/3440/3/JoshuaRoth_1994_Thesis Permission Form.txt" } ], "eprint_id": 3440, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "author ok 9/8/2014", "language": "en", "security": "internal", "license": "other", "main": "JoshuaRoth_1994_Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/40", "datestamp": "2008-09-18", "lastmod": "2019-12-21 02:06:25", "status_changed": "2009-09-25 02:58:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "joshrothastro@gmail.com", "id": "Roth-J", "name": { "family": "Roth", "given": "Joshua" }, "show_email": "NO" } ] }, "title": "Constraints upon the cosmological density parameter from Tully-Fisher observations of IRAS galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "cosmology peculiar velocities omega IRAS spiral galaxies", "abstract": "Mapping galaxy peculiar velocities, or departures from the uniform expansion of the universe, on megaparsec scales promises to indicate whether number density fluctuations in galaxy counts trace density fluctuations in the underlying matter (to within some factor b), and, if so, to constrain the cosmological density parameter \u03a9, which dictates whether space will expand forever or one day collapse. To sample the peculiar velocity field to distances approaching that of the Hydra-Centaurus complex (but in all directions) we have extracted an all sky, quasi volume limited sample to 4000 km sec-1 from the 1.9 Jy 60 micron IRAS redshift survey of Michael Strauss and collaborators. These objects enjoy distance predictions as functions of \u03b2 \u2261 \u03a90.6/b derived from iterative correction of their redshifts for mutual peculiar gravity, which scales with \u03b2. Our volume limited sample most efficiently probes the cosmic flowfield and enjoys objective and uniform selection criteria whose effects upon inferred quantities can be probed with simulations.
\r\n\r\nWe have sought to measure relative distances to the 251 objects in this sample judged a priori suitable for use in the Tully-Fisher (luminosity - linewidth) relation. The requisite neutral hydrogen radio spectra and near infrared CCD photometry have been obtained for about one half of these objects. Methods of reducing the radio and CCD data are explained in detail. Isophotal I band magnitudes are reproduced by independent observations to ~ 0.05 magnitudes precision. Errors and biases in neutral hydrogen linewidths at low signal to noise ratio are quantified.
\r\n\r\nThe I band magnitude and 21 cm. linewidth data imply a Tully-Fisher (TF) relation at each value of \u03b2 from 0.05 to 2.00 used by Strauss et al. to iterate the IRAS redshift catalog. The \u03b2 value producing minimum apparent TF scatter is investigated as a diagnostic with extensive Monte Carlo simulations. Such simulations suggest that, if the \u03b2 knob setting producing minimum apparent TF scatter were found to equal unity, ~ 100 galaxy distance moduli to ~ 0.5 magnitudes precision would constrain the actual value of \u03b2 to lie within the range 0.7 \u2272 \u03b2 \u2272 1.3 at a ~ 95% confidence level.
\r\n\r\n'\u03b2 response profiles' (apparent TF scatter versus \u03b2) observed in various subsets of our provisional database are presented. Our provisional database yields minimum apparent TF scatter at a \u03b2 value of ~ 0.9. Excising the apparently problematic Virgo cluster region yields a response profile favoring \u03b2 values of ~ 0.6 \u00b1 0.2, or \u03a9 ~ 0.4 \u00b1 0.3. Excising data points disfavored by statistical estimates of leverage upon \u03b2 likewise favors low values of \u03b2 ~ 0.5. Limitations to our current data analysis which preclude our asserting strong constraints upon the density parameter at present are discussed in detail.
\r\n", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-105723", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-105723", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-18", "doi": "10.7907/G8Y2-6V10", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "chair" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1993-06-16", "thesis_approved_date": "2008-09-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Roth, Joshua" }, { "id": "/id/eprint/3442", "eprint_id": 3442, "rev_number": 10, "documents": [ { "id": "/id/document/5977", "doc_id": 5977, "rev_number": 3, "files": [ { "id": "/id/file/35613", "fileid": 35613, "datasetid": "document", "objectid": 5977, "filename": "Horowitz_ik_1994.pdf", "mime_type": "application/pdf", "filesize": 11230840, "mtime": "2012-12-26 02:59:56", "url": "/3442/1/Horowitz_ik_1994.pdf" } ], "eprint_id": 3442, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Horowitz_ik_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Horowitz_ik_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22517" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22517" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22517" } ] } }, { "id": "/id/document/22517", "doc_id": 22517, "rev_number": 3, "files": [ { "id": "/id/file/35611", "fileid": 35611, "datasetid": "document", "objectid": 22517, "filename": "preview.png", "mime_type": "image/png", "hash": "2ab71c2fee0899462d38316e4715bfc0", "hash_type": "MD5", "filesize": 8021, "mtime": "2012-12-26 02:59:56", "url": "/3442/2/preview.png" } ], "eprint_id": 3442, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5977" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5977" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5977" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/42", "datestamp": "2008-10-30", "lastmod": "2021-04-16 23:06:11", "status_changed": "2009-09-25 02:58:28", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Horowitz-Irwin-Kenneth", "name": { "family": "Horowitz", "given": "Irwin Kenneth" }, "show_email": "NO" } ] }, "title": "Evolution of emission line galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThis thesis compares two samples of emission line galaxies, selected on the basis of the strength of their [0111]\u03bb\u03bb4959, 5007 and/or H\u03b2 \u03bb4861 emission lines. The distant sample is drawn from the 4-Shooter transit survey undertaken by Schmidt, Schneider and Gunn (1994 and references therein), and consists of 370 galaxies with emission line equivalent widths in excess of 50[...] and fluxes above well-defined wavelength-dependent limits. This survey consists of 6 narrow strips of the sky covering ~ 62 square degrees. Each of these galaxies is classified by using line ratio diagnostics from the moderate resolution spectra taken to identify the emission line.\r\n\r\nThe nearby sample is taken from the first CfA Northern Sky Redshift Survey, and consists of 81 galaxies from Burg (1987) with [OIII]\u03bb\u03bb4959,5007 EW\u226523.75[...] and an additional 26 Seyfert galaxies from Edelson (1987). This sample is observed on the 1.5m Oscar Meyer telescope using the Echelle Spectrograph in a low-resolution, long slit mode (McCarthy, 1988). Each of the 107 galaxies is observed twice, along perpendicular axes over a wavelength range from 4350[...] to 7200[...], which covers the emission lines of interest such as H\u03b2 \u03bb4861, [OIII]\u03bb\u03bb4959,5007 and H\u03b1 \u03bb6563. These data are used both to classify the 107 galaxies from their line ratio diagnostics as well as to model the spatial and spectral light distribution on the plane of the sky for a comparison of how each would appear in the distant survey as a function of redshift.\r\n\r\nMaximum redshifts in both the nearby and the distant survey are determined for each CfA galaxy, and predicted number counts, based on both a no-evolution model as well as a model incorporating density evolution, are made from the corresponding ratio of accessible volumes in the two surveys. Corrections are made to the predicted counts to account for sample incompletenesses and the overdensity of the CfA survey relative to the average density of galaxies in the \"local\" universe. These predicted counts are compared to the observed counts from the distant survey for each object class. The results from this comparison are consistent with the no-evolution model for emission line galaxies out to z~0.5, and do not support the conjecture (Broadhurst et al. 1988; Colless et al. 1990) that there is an evolving population of dwarf star-forming emission line galaxies.\r\n", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-134503", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-134503", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-30", "doi": "10.7907/c8r3-gs98", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1994-04-25", "thesis_approved_date": "2008-10-30", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Horowitz, Irwin Kenneth" }, { "id": "/id/eprint/3446", "eprint_id": 3446, "rev_number": 10, "documents": [ { "id": "/id/document/5981", "doc_id": 5981, "rev_number": 3, "files": [ { "id": "/id/file/35643", "fileid": 35643, "datasetid": "document", "objectid": 5981, "filename": "Herbig_th_1994.pdf", "mime_type": "application/pdf", "filesize": 6849441, "mtime": "2012-12-26 02:59:58", "url": "/3446/1/Herbig_th_1994.pdf" } ], "eprint_id": 3446, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Herbig_th_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Herbig_th_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22521" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22521" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22521" } ] } }, { "id": "/id/document/22521", "doc_id": 22521, "rev_number": 3, "files": [ { "id": "/id/file/35641", "fileid": 35641, "datasetid": "document", "objectid": 22521, "filename": "preview.png", "mime_type": "image/png", "hash": "408365bbd35daa8d47f000531afdc840", "hash_type": "MD5", "filesize": 9933, "mtime": "2012-12-26 02:59:58", "url": "/3446/2/preview.png" } ], "eprint_id": 3446, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5981" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5981" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5981" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/46", "datestamp": "2008-09-16", "lastmod": "2021-11-05 22:41:07", "status_changed": "2009-09-25 02:58:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Herbig-Thomas", "name": { "family": "Herbig", "given": "Thomas" }, "show_email": "NO" } ] }, "title": "A measurement of the Sunyaev-Zeldovich effect in the coma cluster of galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "This thesis presents a measurement of the Sunyaev-Zeldovich effect in the Coma cluster of galaxies. The observed effect is \u0394T[subscript 0,obs] = -302.1\u00b148\u03bcK, and was measured at a frequency of 32GHz with the 5.5m telescope at the Owens Valley Radio Observatory. Interpreted in the context of existing X-ray models, I derive a peak central SZ effect of \u0394T[subscript 0,peak] = -495.3\u00b178.7\u00b5K. With this interpretation, I also calculate a value of H[subscript 0] = 74.2\u00b127.9kms[superscript -1]Mpc[superscript -1] for the Hubble constant. This is the first successful measurement of the SZ effect in a nearby cluster, an important advance because of the much better potential for its astronomical and cosmological interpretation.", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-151722", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-151722", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-16", "doi": "10.7907/3wd8-xa84", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1993-09-20", "thesis_approved_date": "2008-09-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Herbig, Thomas" }, { "id": "/id/eprint/4534", "eprint_id": 4534, "rev_number": 9, "documents": [ { "id": "/id/document/7353", "doc_id": 7353, "rev_number": 2, "files": [ { "id": "/id/file/44886", "fileid": 44886, "datasetid": "document", "objectid": 7353, "filename": "Flanagan_ee_1994.pdf", "mime_type": "application/pdf", "filesize": 42149155, "mtime": "2012-12-26 03:09:32", "url": "/4534/1/Flanagan_ee_1994.pdf" } ], "eprint_id": 4534, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Flanagan_ee_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Flanagan_ee_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23878" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23878" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23878" } ] } }, { "id": "/id/document/15960", "doc_id": 15960, "rev_number": 3, "files": [ { "id": "/id/file/204383", "fileid": 204383, "datasetid": "document", "objectid": 15960, "filename": "Flanagan_Eanna_E_1994.txt", "mime_type": "text/plain", "filesize": 1562, "mtime": "2016-08-22 21:17:26", "url": "/4534/2/Flanagan_Eanna_E_1994.txt" } ], "eprint_id": 4534, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Flanagan_Eanna_E_1994.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/23878", "doc_id": 23878, "rev_number": 2, "files": [ { "id": "/id/file/44884", "fileid": 44884, "datasetid": "document", "objectid": 23878, "filename": "preview.png", "mime_type": "image/png", "hash": "bbb2fd876a3e84d7c76795e42a2e68bf", "hash_type": "MD5", "filesize": 14679, "mtime": "2012-12-26 03:09:32", "url": "/4534/3/preview.png" } ], "eprint_id": 4534, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7353" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7353" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7353" } ] } }, { "id": "/id/document/124367", "doc_id": 124367, "rev_number": 1, "files": [ { "id": "/id/file/369797", "fileid": 369797, "datasetid": "document", "objectid": 124367, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "10d58916660e6271677374af4587af8d", "hash_type": "MD5", "filesize": 807, "mtime": "2021-06-23 23:30:13", "url": "/4534/4/indexcodes.txt" } ], "eprint_id": 4534, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15960" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15960" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15960" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/45/34", "datestamp": "2006-11-13", "lastmod": "2020-03-10 23:39:07", "status_changed": "2009-09-25 03:20:17", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "eef3@cornell.edu", "id": "Flanagan-E-E", "name": { "family": "Flanagan", "given": "Eanna E." }, "show_email": "YES" } ] }, "title": "Topics in general relativity : the hoop conjecture and theoretical aspects of gravitational wave detection", "ispublished": "unpub", "full_text_status": "public", "abstract": "The body of this thesis consists of four chapters (2 through 5), each of which is a paper that has been published in or submitted for publication to Physical Review D. I am the sole author of chapters 2, 3, and 4; Curt Cutler coauthored chapter 5 with me.\r\n\r\nThese four chapters deal with two topics in general relativity: the formation of horizons in nonspherical gravitational collapse (chapters 2 and 3), and some theoretical aspects of the effort to detect gravitational waves from cosmic sources (chapters 4 and 5). These four chapters were written largely for experts in the topics they cover. As an aid to general readers, I shall give in this introductory chapter some background information about chapters 2 through 5 and a nontechnical overview of their contents.", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-11132006-095610", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-11132006-095610", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-11-13", "doi": "10.7907/7SW7-8076", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-11-13", "thesis_defense_date": "1993-09-23", "thesis_approved_date": "2006-11-13", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Flanagan, Eanna E." }, { "id": "/id/eprint/4843", "eprint_id": 4843, "rev_number": 10, "documents": [ { "id": "/id/document/7732", "doc_id": 7732, "rev_number": 3, "files": [ { "id": "/id/file/47474", "fileid": 47474, "datasetid": "document", "objectid": 7732, "filename": "Willette_gt_1994.pdf", "mime_type": "application/pdf", "filesize": 4011220, "mtime": "2012-12-26 03:12:18", "url": "/4843/1/Willette_gt_1994.pdf" } ], "eprint_id": 4843, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Willette_gt_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Willette_gt_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/24251" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/24251" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/24251" } ] } }, { "id": "/id/document/24251", "doc_id": 24251, "rev_number": 3, "files": [ { "id": "/id/file/47472", "fileid": 47472, "datasetid": "document", "objectid": 24251, "filename": "preview.png", "mime_type": "image/png", "hash": "34ba195c46b1a2ccd1541b03d1240618", "hash_type": "MD5", "filesize": 10045, "mtime": "2012-12-26 03:12:18", "url": "/4843/2/preview.png" } ], "eprint_id": 4843, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7732" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7732" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7732" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/48/43", "datestamp": "2007-12-13", "lastmod": "2021-04-16 22:29:41", "status_changed": "2009-09-25 03:27:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Willette-G-T", "name": { "family": "Willette", "given": "Gregory Thomas" }, "show_email": "NO" } ] }, "title": "Stochastic excitation of the solar oscillations by turbulent convection", "ispublished": "unpub", "full_text_status": "public", "keywords": "Applied Physics", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\n\r\nThe thesis topic is the stochastic excitation of the solar p-modes by turbulent convection, and the work consists of four parts: three theoretical sections and one observational. In the first section of the thesis, an explicit calculation of the acoustic radiation of a buoyant oscillating bubble is presented as a model for the excitation of the solar p-modes. The central scientific issue addressed in this work is the cancellation of monopole and dipole radiation fields in an anisotropic medium, first pointed out by Goldreich and Kumar (1990). When the bubble oscillation frequency is small compared to the acoustic cutoff, the monopole and dipole disturbances cancel to the quadrupole order in the far field. The second section deals with the role of convective structures in a wide number of problems, including the creation of acoustic disturbances, the transport of heat and magnetic fields, and the penetration of flows into stable layers of the atmosphere (overshoot). A model of plume convection is developed to discuss these issues. It is argued that the scaleheight-sized flows (the only energetically significant ones) are properly characterized as coherent, entropy-preserving plumes, in contradistinction to the picture of amorphous parcels of fluid suggested by the Mixing Length Theory, and in spite of the large Reynolds numbers typical in astrophysical convection. The third section of the thesis is an analysis of high-resolution surface velocity data taken with a magneto-optical filter on the 10 inch telescope at Big Bear Solar Observatory. Estimates are obtained for the frequencies and amplitudes of the solar oscillations of high spherical harmonic degree ([...] 2000). The observed mode energies follow a Boltzmann distribution [...], as is predicted in the stochastic excitation model. In the final section of the thesis, a derivation of the variational principle for an incompressible fluid is presented. The Lagrange and Hamiltonian densities are calculated to third order in the displacement field, and these results suitable to study the non-linear interactions among incompressible modes.\r\n", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-12072007-081017", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-12072007-081017", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-12-13", "doi": "10.7907/7nmq-8a04", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-12-07", "thesis_defense_date": "1994-05-23", "thesis_approved_date": "2007-12-13", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Willette, Gregory Thomas" }, { "id": "/id/eprint/2644", "eprint_id": 2644, "rev_number": 12, "documents": [ { "id": "/id/document/4939", "doc_id": 4939, "rev_number": 3, "files": [ { "id": "/id/file/28653", "fileid": 28653, "datasetid": "document", "objectid": 4939, "filename": "Leroy_ss_1994.pdf", "mime_type": "application/pdf", "filesize": 8359682, "mtime": "2012-12-26 02:53:18", "url": "/2644/1/Leroy_ss_1994.pdf" } ], "eprint_id": 2644, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Leroy_ss_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Leroy_ss_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21489" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21489" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21489" } ] } }, { "id": "/id/document/21489", "doc_id": 21489, "rev_number": 3, "files": [ { "id": "/id/file/28651", "fileid": 28651, "datasetid": "document", "objectid": 21489, "filename": "preview.png", "mime_type": "image/png", "hash": "d63245cb5bf74cea6389fd12fedb35cc", "hash_type": "MD5", "filesize": 9737, "mtime": "2012-12-26 02:53:18", "url": "/2644/2/preview.png" } ], "eprint_id": 2644, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4939" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4939" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4939" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/26/44", "datestamp": "2008-06-18", "lastmod": "2021-04-19 22:26:51", "status_changed": "2009-09-25 02:42:13", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Leroy-Stephen-Sylvain", "name": { "family": "Leroy", "given": "Stephen Sylvain" }, "show_email": "NO" } ] }, "title": "Convectively generated internal gravity waves in Venus's middle atmosphere : momentum transport and radio scintillations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Physics", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThis work is divided into two papers. Firstly, we theoretically calculate how gravity waves are emitted from the neutrally buoyant dry convection in Venus's middle atmosphere and investigate whether such waves play a significant role in supporting the superrotation of Venus's atmosphere. Secondly, we attempt to explain the radio scintillations seen in the occultations of many spacecraft, particularly Pioneer Venus, as caused by convectively generated gravity waves. Below are the abstracts of the two papers presented in this thesis.\r\n\r\nPaper I:\r\n\r\nWe calculate the emission of internal gravity waves from neutrally buoyant dry convection embedded within a stable atmosphere with static stability and zonal winds varying in height. We apply this theory to Venus's middle atmosphere to investigate whether these waves can help support the superrotation of Venus's atmosphere. Furthermore, we model the radio scintillation data obtained for Venus as caused by such internal gravity waves. The emission mechanism is similar to that suggested for driving the gravity modes of the Sun. We assume a background atmosphere on which we have superimposed linear wave propagation. Waves are damped by reabsorption by the convection, wavebreaking in the stable atmosphere, critical layer absorption, and by wave radiation to space. Wavebreaking is imposed wherever the waves become convectively unstable. Inertial effects are neglected and plane parallel geometry is assumed. Propagation of the waves is handled using a second order WKBJ approximation. A complete three dimensional ensemble of waves is retained.\r\n\r\nWe show that both westward and eastward propagating waves exert strong accelerations on the mean flow. The westward propagating carry enough momentum to support the westward superrotation between the convection and the cloud-tops; however, the bulk of the wave momentum flux is critically absorbed and deposited within a kilometer of the convection because most of the waves propagate slowly in the horizontal. The eastward propagating waves are found to exert large decelerations above the zonal wind maximum. The decelerations are larger than 20 m [...] day [...], similar to wave drag in the Earth's mesosphere.\r\n\r\nIn the course of evaluating our model, we have found that dry convection must have \"penetrative\" mixed layers above and below it. This arises from wavebreaking of gravity waves immediately after their generation. The effect of the penetrative layer is to filter wave emission and to create a discontinuity in the background temperature lapse rate dT/dz. The latter may be observable in atmospheres.\r\n\r\nPaper II:\r\n\r\nWe simulate radio scintillations as they would appear in Pioneer Venus radio occultation data assuming that the index of refraction fluctuations in Venus's atmosphere responsible for the scintillations are directly caused by gravity wave fluctuations. We assume that the gravity waves are created by a global convection layer between 50 and 55 km altitude in Venus's atmosphere and propagate vertically. Associated with the gravity waves are density fluctuations which create the index of refraction variations. We compare the simulated scintillations with data and argue that this theory for the radio scintillations is preferable to the theory that the scintillations are caused by clear air turbulence in Venus's atmosphere.\r\n\r\nWe show that these gravity waves can explain the shape and amplitude of the radio scintillation variance spectra in frequency. The shape of the simulated radio scintillation variance spectra in frequency is nearly a direct result of a saturated spectrum of breaking gravity waves. This saturated spectrum is the spectrum of breaking gravity waves in the vertical wavenumber. On the other hand, the overall amplitude is subject to parameters such as the intensity of the convection, the angle between the zonal winds and the beam path, and the zonal wind profile at polar latitudes. Limits can be placed, though, on the intensity of the convection which generates the waves and on the angle between the radio beam path and the winds in Venus's atmosphere. We find that the convection in Venus's middle atmosphere, even in polar regions, must transport 1 W/[...] to create gravity waves strong enough to break. This result is dependent on the amplitude of the zonal winds at polar latitudes.\r\n", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-06182008-135507", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06182008-135507", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-06-18", "doi": "10.7907/msgs-7b48", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "chair" }, { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-06-18", "thesis_defense_date": "1994-05-23", "thesis_approved_date": "2008-06-18", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Leroy, Stephen Sylvain" }, { "id": "/id/eprint/3591", "eprint_id": 3591, "rev_number": 8, "documents": [ { "id": "/id/document/6163", "doc_id": 6163, "rev_number": 3, "files": [ { "id": "/id/file/36860", "fileid": 36860, "datasetid": "document", "objectid": 6163, "filename": "Young_kh_1994.pdf", "mime_type": "application/pdf", "filesize": 7459866, "mtime": "2012-12-26 03:01:10", "url": "/3591/1/Young_kh_1994.pdf" } ], "eprint_id": 3591, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Young_kh_1994.pdf", "language": "en", "security": "public", "license": "other", "main": "Young_kh_1994.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22701" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22701" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22701" } ] } }, { "id": "/id/document/22701", "doc_id": 22701, "rev_number": 3, "files": [ { "id": "/id/file/36858", "fileid": 36858, "datasetid": "document", "objectid": 22701, "filename": "preview.png", "mime_type": "image/png", "hash": "f352950996f968253203ab5f46efa54e", "hash_type": "MD5", "filesize": 8603, "mtime": "2012-12-26 03:01:10", "url": "/3591/2/preview.png" } ], "eprint_id": 3591, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6163" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6163" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6163" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/91", "datestamp": "2008-11-06", "lastmod": "2021-04-16 22:17:59", "status_changed": "2009-09-25 03:01:19", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Young-K-H", "name": { "family": "Young", "given": "Kenneth Harbour" }, "show_email": "NO" } ] }, "title": "Submillimeter and infrared studies of mass lost by asymptotic giant branch stars", "ispublished": "unpub", "full_text_status": "public", "abstract": "This thesis consists of four separate studies of the material ejected from highly evolved red giant stars, preceded by a brief introductory chapter.\n\nChapter 2 presents the results of an attempt to identify all the post main sequence stars in the sky with circumstellar shells large enough to have been resolved by the IRAS satellite. Both the 60\u03bcm and 100\u03bc survey mode data were used. A total of 512 stars were examined, including all evolved stars with envelopes which had been detected in surveys of mm or submm CO emission. A total of 76 stars were found to have shells with radii exceeding 2' in the 60\u03bc data. Most of these resolved shells surround semiregular variable stars. Although only 40% of the resolved objects are carbon stars, the fraction of carbon stars with resolved envelopes is higher than that of oxygen\u2014rich stars. The linear sizes of these shells were calculated; the average shell size is 0.76 pc. If a measurement of the expansion velocity was available from CO observations, the age of the shell was estimated using a simple model of the shell's interaction with the ISM. Some of the shells appear to be detached, and in most cases shells with inner radii greater than ~ 0.3 pc have no detectable CO. The duration of mass loss for Mira variables and carbon stars is estimated to be 10[superscript 5] and 2 x 10[superscript 5] years, respectively. The procedure by which the data were analysed is explained in the appendix to chapter 2, which also contains the results of several tests performed to verify the results statistically.\n\nA survey of CO(3-2) emission from Mira variables comprises chapter 3. The survey examined nearby oxygen\u2014rich Miras, without regard to their infrared properties. Several new detections were made, including some circumstellar shells with expansion velocities lower than any previously reported. Mass loss rates for the detected stars were calculated. While the mass loss rate shows significant correlation with all 4 IRAS fluxes (when normalized by distance), it appears completely uncorrelated with any color derived from these fluxes. A star's spectral type at maximum light was found to be a good predictor of which stars would be detectable; no star earlier than M5.5 was detected even though some such stars had large IRAS fluxes. A power\u2014law relationship was found between the envelope expansion velocity and the star's mass loss rate. Extrapolation of this result implies that envelopes with expansion velocities above ~ 18 km s[superscript -1] must be optically thick.\n\nThe peculiar submm emission line profiles of CRL 2688, a protoplanetary nebula, are examined in chapter 4. The molecular envelope was found to have three kinematic components, including a previously undetected ~ 100 km s[superscript -1] wind. The mechanical momentum in this high velocity wind appears to be much too large to have been supplied by radiation pressure. A strong self-absorption feature seen in the CO emission lines was examined at very high spectral resolution, and was found to have an extremely sharp blue edge. The sharpness of this feature shows that the velocity field in the extended envelope is very well ordered.\n\nThe final chapter examines atomic carbon emission in the envelope of the young planetary nebula NGC 7027. Neutral carbon, traced by the 609\u03bcm hyperfine line, is extended over a region 30-40\" in diameter, and appears to be coextensive with CO throughout most of the neutral envelope. A 158\u03bcm spectrum of C II was used to calculate a lower limit to the C II mass. There appears to be roughly equal amounts of CO, C I and C II in the inner neutral envelope. Most of the atomic carbon must have been liberated by photodissociation of CO. Estimates of the mass loss rate for this object derived from CO observations may be too low by a factor of ~ 3.\n", "date": "1994", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-085430", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-085430", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-06", "doi": "10.7907/pkm9-jk53", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "1993-08-01", "thesis_approved_date": "2008-11-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1994", "author_list": "Young, Kenneth Harbour" }, { "id": "/id/eprint/7299", "eprint_id": 7299, "rev_number": 33, "documents": [ { "id": "/id/document/16578", "doc_id": 16578, "rev_number": 5, "files": [ { "id": "/id/file/101641", "fileid": 101641, "datasetid": "document", "objectid": 16578, "filename": "Buttgenbach_th_1993.pdf", "mime_type": "application/pdf", "filesize": 41494583, "mtime": "2012-12-26 04:46:10", "url": "/7299/1/Buttgenbach_th_1993.pdf" } ], "eprint_id": 7299, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Buttgenbach_th_1993.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28255" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28255" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28255" } ] } }, { "id": "/id/document/16579", "doc_id": 16579, "rev_number": 3, "files": [ { "id": "/id/file/208069", "fileid": 208069, "datasetid": "document", "objectid": 16579, "filename": "Buttgenbach_th_1993.zip", "mime_type": "application/zip", "filesize": 73309901, "mtime": "2016-08-22 21:24:24", "url": "/7299/2/Buttgenbach_th_1993.zip" } ], "eprint_id": 7299, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Buttgenbach_th_1993.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/28255", "doc_id": 28255, "rev_number": 3, "files": [ { "id": "/id/file/101639", "fileid": 101639, "datasetid": "document", "objectid": 28255, "filename": "preview.png", "mime_type": "image/png", "hash": "c33b9c279def0e38aae7d0feec0e485e", "hash_type": "MD5", "filesize": 27141, "mtime": "2012-12-26 04:46:10", "url": "/7299/3/preview.png" } ], "eprint_id": 7299, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16578" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/16578" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16578" } ] } }, { "id": "/id/document/127754", "doc_id": 127754, "rev_number": 1, "files": [ { "id": "/id/file/373190", "fileid": 373190, "datasetid": "document", "objectid": 127754, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "24b4b10f36535caacb64c11ba87349bd", "hash_type": "MD5", "filesize": 32020, "mtime": "2021-06-24 02:03:08", "url": "/7299/4/indexcodes.txt" } ], "eprint_id": 7299, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16578" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16578" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16578" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/00/72/99", "datestamp": "2012-11-30 21:40:59", "lastmod": "2022-11-09 19:20:01", "status_changed": "2012-11-30 21:40:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "B\u00fcttgenbach-T-H", "name": { "family": "B\u00fcttgenbach", "given": "Thomas H." }, "show_email": "NO" } ] }, "title": "Quasi-optical sis receivers and astrophysical observations at submillimeter wavelengths", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis describes the development of a new generation of submillimeter wave receivers aimed\r\nat future integrated array receivers and presents astronomical observations taken with a single\r\nelement of such a new receiver in the submillimeter wavelength band.
\r\n\r\nThe technological development presented in this thesis was driven by the need to develop\r\nheterodyne receivers based on superconductor- insulator-superconductor (SIS) detectors, which\r\nhave proven to be the most sensitive detectors in the millimeter and low submillimeter band, and\r\nthat are suitable for the construction of array receivers. A quasi--optical approach was chosen in\r\norder to take advantage of the planar photolithography used in SIS diode manufacturing. This\r\nallows straightforward integration with planar antennas. The introductory chapter describes an\r\ninitial receiver design, based on a planar logarithmic spiral antenna, that was an improvement\r\nover existing quasi-optical designs using planar antennas.
\r\n\r\nThis receiver was the first submillimeter SIS receiver ever to be used for astronomical\r\nobservations. However, it also showed that two major problems still had to be overcome to\r\ndevelop this technology to the mature state where array receivers can be designed. The beam of\r\nan individual element, launched by the planar antenna, has to be of high quality - comparable\r\nto that of a waveguide hom antenna - to provide good coupling to a telescope. Second, the\r\nimpedance of the SIS detector, dominated by its capacitance, has to be matched to the antenna's\r\nimpedance over the operating range of the receiver.
\r\n\r\nThe optics problem was solved by introducing a novel antenna design called the hybrid\r\nantenna. The hybrid antenna is defined as a dielectric lens-antenna as a special case of an\r\nextended hemispherical dielectric lens that is operated in the diffraction limited regime. It is a\r\nmodified version of the planar antenna on a lens scheme developed by Rutledge. The dielectric\r\nlens- antenna is fed by a planar-structure feed antenna and the combination of the two is termed\r\na hybrid antenna. Beam pattern and aperture efficiency measurements were made at millimeter\r\nand submillimeter wavelengths as a function of extension of the hemispherical lens and different\r\nlens sizes. An optimum extension distance is found experimentally and theoretically for which\r\nexcellent beam patterns and simultaneously high aperture efficiencies can be achieved. At 115\r\nGHz the aperture efficiency was measured to be (76 \u00b1 5 )% for a diffraction limited beam with\r\nsidelobes below -17 dB. The hybrid antenna is diffraction limited, space efficient in an array\r\ndue to its high aperture efficiency, and is easily mass produced, thus being well suited for focal\r\nplane heterodyne receiver arrays. A single element hybrid antenna receiver yielded coupling\r\nefficiencies between the receiver and the Caltech Submillimeter Telescope of values approaching\r\nthose achieved by the best waveguide horn based receiver systems.
\r\n\r\nThe problem of tuning the SIS junction's capacitance was solved by using a novel superconducting\r\ntransmission line circuit, called the end-loaded-stub, together with a real impedance\r\ntransformer. This Nb based circuit is integrated with the planar feed antenna of the hybrid antenna\r\nand a Nb/AlO_x/Nb SIS detector. A goal for the matching circuit design was to achieve an octave\r\nof bandwidth and computer modeling of the device correctly predicted the measured bandwidth\r\nand characteristic frequencies to within 8%. The bandwidth measurements were carried out by\r\nusing the SIS diode in direct detection mode with a fuurier Transform Spectrometer. A good\r\nmatch was obtained from 200 GHz to 475 GHz between the antenna and a relatively large area (1\r\n\u00b5m^2) tunnel junction with wR_nC \u2248 2-4. Noise measurements were made in heterodyne mode\r\nat 318 GHz, 395 GHz, 426 GHz and 492 GHz, yielding uncorrected double sideband receiver\r\nnoise temperatures of 200 K, 230 K, 220 K and 500 K, respectively. These results are comparable\r\nto state of the art waveguide receivers.
\r\n\r\nThe combination of a hybrid antenna with the integrated tuning circuit thus lays the foundation\r\nfor the development of integrated SIS focal plane receiver arrays.
\r\n\r\nThe final chapter describes observations of the neutral carbon C I(^3P_1 \u2192 ^3P_0) line at 492\r\nGHz with a single element quasi-optical SIS receiver. The goal was to investigate the large- and\r\nsmall-scale distribution of C I in the interstellar medium (ISM). Observations of neutral atomic\r\ncarbon in the galaxy IC 342, made at the Caltech Sub\r\nmillimeter Observatory, are presented, which\r\nrepresent the first extragalactic submillimeter detection of C I. The C I emission from IC 342 was\r\nfound to have a main beam temperature of about 1 K, which is a factor of two greater than that\r\nfor ^(13)CO \u2192 1) in the same size beam. The integrated line intensity for the central 15\" of\r\nIC 342 was found to be (6.2 \u00b1 1.2) x 10^(-6) erg s^(-1) cm^(-2) sr^(-1). A 45\" cut from the center to the\r\nsouth showed that the intensity ratio of C I to CO(2 \u2192 1) is constant at about 1.4. The C I to\r\nCO abundance ratio is about 15% and the total C I abundance relative to hydrogen is 7 x 10^(-6),\r\nyielding about \u2265 10% of all carbon in the gas phase to be in form of neutral atomic carbon.
\r\n\r\nComparing the IC 342 data with COBE observations of the Milky Way it is found that the\r\nintensity ratio of C I to CO(2 \u2192 1) is approximately the same for IC 342 as it is for the Milky\r\nWay, despite the fact that the IC 342 measurements are from the center a moderate star burst\r\ngalaxy, while the COBE data are an average over the entire Milky Way. From the comparison\r\nbetween the Milky Way and IC 342 and the cut through IC 342 it can thus be concluded that\r\nthere is a strong correlation of CO with C I emission on large scales.
\r\n\r\nThe small-scale structure of neutral carbon in the ISM is studied with a 3' by 4' (\u0394\u03b1 \u0394\u03b4)\r\nmap, sampled at 20\" intervals with a 15\" beam, in the Orion Molecular Cloud (OMC). The map\r\ncovers the embedded infrared source IRc2, the southern source (OMC-1 south, FIR 3,4) and the\r\nionizing stars of the Trapezium. C I is found to be widespread with a typical intensity of about\r\n6 x 10^(-6) ergs^(-1)cm^(-2) sr^(-1)and some enhancement at the interface between the ionized and neutral\r\nmolecular medium with a peak intensity of 9.6 x 10^(-6) erg s^(-1) cm^(-2) sr^(-1). A typical gas phase\r\nabundance of neutral carbon relative to hydrogen of \u2248 3 x 10^(-6) is found, decreasing two orders\r\nof magnitude in the cores of the condensations.
\r\n\r\nTheoretical model calculations of ion chemistry of molecular clouds with external UV illumination\r\nwere performed for this thesis, based on a code by Le Bourlot, which allow for an\r\nexplanation of the observed relation of neutral carbon to CO and hydrogen on both, large and\r\nsmall, scales. It is suggested, based on the observational data presented and the good agreement\r\nof the observations with the ion chemistry model, that the C I (1 \u2192 0) emission emanates from\r\nthe bulk of gas in molecular clouds, i.e., from regions similar to those emitting in the low J ^(13)CO\r\nlines. This requires the bulk of the observed medium to be in the chemically low-density regime\r\nwhere charge transfer reactions of atomic species dominate over protonation reactions (started by\r\nH^+_3) of oxygen bearing molecules. The fine structure emission lines from neutral carbon are thus\r\na more important coolant for the ISM than the rotational transitions of CO for low to moderate\r\nhydrogen densities. This is in contrast to previous PDR models that only had significant neutral\r\ncarbon abundances in a thin PDR transition layer on the surface of molecular clouds irradiated\r\nby FUV.
\r\n\r\n\r\n\r\n", "date": "1993", "date_type": "degree", "id_number": "CaltechTHESIS:11302012-115924624", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:11302012-115924624", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2012-11-30 21:40:59", "doi": "10.7907/1dkj-1503", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1993-04-01", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1993", "author_list": "B\u00fcttgenbach, Thomas H." }, { "id": "/id/eprint/7302", "eprint_id": 7302, "rev_number": 20, "documents": [ { "id": "/id/document/16675", "doc_id": 16675, "rev_number": 5, "files": [ { "id": "/id/file/101746", "fileid": 101746, "datasetid": "document", "objectid": 16675, "filename": "Biehle_g_1993.pdf", "mime_type": "application/pdf", "filesize": 38858344, "mtime": "2012-12-26 04:46:15", "url": "/7302/1/Biehle_g_1993.pdf" } ], "eprint_id": 7302, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Biehle_g_1993.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28264" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28264" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28264" } ] } }, { "id": "/id/document/16676", "doc_id": 16676, "rev_number": 3, "files": [ { "id": "/id/file/208071", "fileid": 208071, "datasetid": "document", "objectid": 16676, "filename": "Biehle_gt_1993.zip", "mime_type": "application/zip", "filesize": 138062201, "mtime": "2016-08-22 21:24:25", "url": "/7302/2/Biehle_gt_1993.zip" } ], "eprint_id": 7302, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Biehle_gt_1993.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/28264", "doc_id": 28264, "rev_number": 3, "files": [ { "id": "/id/file/101744", "fileid": 101744, "datasetid": "document", "objectid": 28264, "filename": "preview.png", "mime_type": "image/png", "hash": "be9d9e3bad929e96c142a2c921e06e3d", "hash_type": "MD5", "filesize": 44421, "mtime": "2012-12-26 04:46:15", "url": "/7302/3/preview.png" } ], "eprint_id": 7302, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16675" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/16675" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16675" } ] } }, { "id": "/id/document/127763", "doc_id": 127763, "rev_number": 1, "files": [ { "id": "/id/file/373199", "fileid": 373199, "datasetid": "document", "objectid": 127763, "filename": "indexcodes.txt", "mime_type": "text/x-c", "hash": "57a1519c21f6bf0c18a5bf6e2761c226", "hash_type": "MD5", "filesize": 30980, "mtime": "2021-06-24 02:03:23", "url": "/7302/4/indexcodes.txt" } ], "eprint_id": 7302, "pos": 4, "placement": 4, "mime_type": "text/x-c", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16675" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16675" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16675" } ] } } ], "eprint_status": "archive", "userid": 104, "dir": "disk0/00/00/73/02", "datestamp": "2012-12-04 18:04:08", "lastmod": "2022-11-09 19:20:01", "status_changed": "2012-12-04 18:04:08", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Biehle-G-T", "name": { "family": "Biehle", "given": "Garrett T." }, "show_email": "NO" } ] }, "title": "Studies of stars with neutron cores and of x-ray binaries displaying quasi-periodic oscillations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis contains the results of two investigations: one into the nature of stars with degenerate neutron cores and the other into the interpretation of the phenomenology of luminous low-mass X-ray binaries (LMXBs) displaying slow\r\nquasi-periodic oscillations (QPOs) in their X-ray flux.
\r\n\r\nA star with a degenerate neutron core would be a red giant or supergiant. In this thesis we investigate the structure of such a supergiant, particularly examining\r\nthe energy production and seeking an identifying observational signature. This star is convective from near the photosphere down to the base of the envelope just\r\noutside the degenerate core (radius 10 km). The star's luminosity comes from the rp-process in a convective burning region within 100 km of the base of the envelope. The convection brings fuel for the rp-process into the burning region from throughout the envelope and deposits the products of rp-burning back into the envelope, including the photosphere. After about 10^5 years, the abundances of Br, Rb, Y, and Nb at the surface of the star will be about 200 times greater than their solar abundances, and that of Mo, over 1000 times solar. A suitable observational signature would be the strong enhancement of absorption lines for these elements in the star's spectrum. As many as 10 of the nearest 100 red\r\nsupergiants (those within 5 kpc) could have neutron cores.
\r\n\r\nThe other investigation concerns a model of rapid accretion onto an unmagnetized neutron star with radius somewhat less than 6GM/c^2. This model is applied to the phenomenology of a class of LMXBs displaying slow (\u223c 6 Hz)\r\nQPOs in X-ray flux. These sources are highly luminous (approximately Eddington) and display what appears to be three modes (\"branches\") of accretion. In this model, at low accretion rates, the neutron star lies within the inner edge of the accretion disk, and matter is dripped onto the neutron star from the inner edge. As the accretion rate increases, the transition from the \"horizontal branch\"\r\nto the \"normal branch\" occurs when the disk thickens and its inner edge touches the star and forms a boundary layer. The formation of a boundary layer changes the structure of the inner disk and the spectral character of the escaping X-rays. The transition from the normal branch to the \"flaring branch\" occurs when the boundary layer covers the whole surface of the neutron star and radiation escapes\r\nprimarily through convective instabilities. This thesis presents an exploration of this model, with an emphasis on establishing the plausibility that a neutron star could indeed lie inside an accretion disk accreting at the observed rate and that a change of mass accretion rate could push the inner radius onto the surface of the\r\nstar.
\r\n", "date": "1993", "date_type": "degree", "id_number": "CaltechTHESIS:12042012-092833556", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:12042012-092833556", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Dan Anguka", "deposited_on": "2012-12-04 18:04:08", "doi": "10.7907/sx31-ra11", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "id": "Vogel-P", "name": { "family": "Vogel", "given": "Petr" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1992-10-22", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1993", "author_list": "Biehle, Garrett T." }, { "id": "/id/eprint/7384", "eprint_id": 7384, "rev_number": 36, "documents": [ { "id": "/id/document/34492", "doc_id": 34492, "rev_number": 3, "files": [ { "id": "/id/file/109435", "fileid": 109435, "datasetid": "document", "objectid": 34492, "filename": "Santee_m_1993.pdf", "mime_type": "application/pdf", "hash": "7a88573d9f4585519e72a16b35db6994", "hash_type": "MD5", "filesize": 26472443, "mtime": "2013-01-09 18:27:06", "url": "/7384/1/Santee_m_1993.pdf" } ], "eprint_id": 7384, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Santee_m_1993.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 87, "dir": "disk0/00/00/73/84", "datestamp": "2013-01-09 21:19:02", "lastmod": "2021-04-16 22:56:34", "status_changed": "2013-01-09 21:19:02", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Santee-Michelle", "name": { "family": "Santee", "given": "Michelle" }, "show_email": "NO" } ] }, "title": "The thermal structure, dust loading, and meridional transport in the Martian atmosphere during late southern summer", "ispublished": "unpub", "full_text_status": "public", "keywords": "Geology", "abstract": "This thesis consists of two papers, both of which investigate the state of the Martian\r\natmosphere during a relatively clear period in late southern summer. The first paper\r\ndescribes a new technique for the simultaneous retrieval of atmospheric temperatures\r\nand dust abundances from thermal emission spectra. The second paper describes a\r\ndiagnostic stream function model which is used with the temperature and dust results\r\nof the first paper to solve for the meridional and vertical components of the diabatic\r\ncirculation simultaneously. The abstracts for the two papers are reproduced below.
\r\n\r\nPAPER I:
\r\n\r\nThe temperature structure and dust loading of the Martian atmosphere are investigated\r\nusing thermal emission spectra recorded by the Mariner 9 infrared interferometer\r\nspectrometer (IRIS). The analysis is restricted to a subset of the IRIS data\r\nconsisting of approximately 2400 spectra in a 12-day period extending from L_s = 343\u00b0\r\nto L_s = 348\u00b0, corresponding to late southern summer on Mars. Simultaneous retrieval\r\nof the vertical distribution of both atmospheric temperature and dust optical depth\r\nis accomplished through an iterative procedure which is performed on each spectrum.\r\nThe inclusion of dust opacity in the retrieval algorithm causes the retrieved\r\ntemperatures to change by more than 20 K in some atmospheric layers. The largest\r\ncolumn-integrated 9 \u00b5m dust optical depths (~ 0.4) occur over the equatorial regions.\r\nThe highest atmospheric temperatures (> 260 K) are found at low altitudes\r\nnear the sub-solar latitude (~ 6\u00b0 s), while the coldest temperatures (\u02c2 150 K) are\r\nfound at levels near 1.0 mbar over the winter pole. A comparison of temperature\r\nmaps for 2 PM and 2 AM indicates diurnal temperature variations as large as 80 K\r\nat low altitudes near the sub- solar latitude, whereas diurnal temperature changes at\r\npressures less than 1.0 mbar are typically about 10 K. Both dayside and nightside\r\ntemperatures above about 0.1 mbar (~ 40 km) are warmer over the winter (north)\r\npolar region than over the equator or the summer (south) polar region. This thermal\r\nstructure suggests the existence of a net zonally-averaged meridional circulation with\r\nrising motion at low latitudes, poleward flow at altitudes above 40 km, and subsidence\r\nover the poles. Because a meridional circulation transports atmospheric constituents\r\nas well as heat, it has significant implications for the net flux of dust and water into\r\nthe polar regions.
\r\n\r\nPAPER II:
\r\n\r\nThe circulation of the Martian atmosphere during late southern summer is calculated\r\ndiagnostically from the observed atmospheric temperature distribution. We use global\r\nmaps of temperature and dust optical depth (~ 0-60 km) retrieved from a subset of\r\nthe Mariner 9 IRIS thermal emission spectra spanning L_s = 343\u00b0- 348\u00b0 [Santee and\r\nCrisp, 1992]. This thermal structure is characterized by a reversed meridional temperature\r\ngradient (temperatures increasing poleward) at altitudes above about 40 km.\r\nZonal- mean zonal winds are derived from the zonally-averaged temperatures assuming\r\ngradient wind balance and zero surface zonal wind. Both hemispheres have intense\r\nmid- latitude westerly jets (with velocities of 80- 90 m/s near 50 km); in the southern\r\ntropics the winds are strongly easterly (with velocities of 100 m/s near 50 km).\r\nThe north-south atmospheric transport includes contributions from the zonal- mean\r\nmeridional circulation and large-scale waves. Their net effect can be approximated\r\nby the diabatic circulation, which is that circulation needed to maintain the observed\r\ntemperature distribution (warm winter pole, cool tropics) in the presence of the radiative\r\nforcing. A radiative transfer model [Crisp, 1990] which accounts for absorption,\r\nemission and multiple scattering by particles and non- grey gases is used to compute\r\nthe solar heating and thermal cooling rates from diurnal averages of the retrieved\r\nIRlS temperature and dust distributions. At pressures below 4 mbar, there are large\r\nnet heating rates (up to 8 K/ day) in the equatorial region and large net cooling rates\r\n(up to 20 K/ day) in the polar regions. These net heating rates are used in a diagnostic\r\nstream function model which solves for the meridional and vertical components of\r\nthe diabatic circulation simultaneously. We find a two-cell circulation, with upwelling\r\nover the equator(~ 1.5 cm/s), poleward motion in both hemispheres(~ 2 m/s), and\r\nsubsidence over the poles (1-2 cm/ s). This circulation is sufficiently vigorous that the\r\nmeridional transport time scale is ~ 13 days. Vertical transport is primarily advective\r\nin nature, except in the high-altitude winter polar regions, where diffusive processes\r\ndominate. Water vapor desorbed from the low-latitude regolith during late northern\r\nwinter/ early northern spring may be transported upward by the ascending branch of\r\nthis circulation, where it would be transported poleward by the high-altitude meridional\r\nwinds. This process could provide a high-altitude source of water vapor for the\r\npolar hood.
\r\n\r\n\r\n\r\n\r\n", "date": "1993", "date_type": "degree", "id_number": "CaltechTHESIS:01092013-102520560", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01092013-102520560", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2013-01-09 21:19:02", "doi": "10.7907/5qzc-4127", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "advisor" }, { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1992-06-19", "review_status": "approved", "option_major": { "items": [ "geol" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1993", "author_list": "Santee, Michelle" }, { "id": "/id/eprint/3971", "eprint_id": 3971, "rev_number": 19, "documents": [ { "id": "/id/document/6625", "doc_id": 6625, "rev_number": 4, "files": [ { "id": "/id/file/40025", "fileid": 40025, "datasetid": "document", "objectid": 6625, "filename": "Ghez_a_1993.pdf", "mime_type": "application/pdf", "filesize": 10007894, "mtime": "2012-12-26 03:04:22", "url": "/3971/1/Ghez_a_1993.pdf" } ], "eprint_id": 3971, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Scanned (no OCR) Ghez_a_1993", "language": "en", "security": "internal", "license": "other", "main": "Ghez_a_1993.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"hash_type": "MD5", "filesize": 20110, "mtime": "2021-06-23 23:07:35", "url": "/3971/10/indexcodes.txt" } ], "eprint_id": 3971, "pos": 10, "placement": 10, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/104005" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/104005" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/104005" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/39/71", "datestamp": "2004-10-08", "lastmod": "2021-07-27 00:12:26", "status_changed": "2009-09-25 03:08:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ghez@astro.ucla.edu", "id": "Ghez-Andrea-Mia", "name": { "family": "Ghez", "given": "Andrea Mia" }, "orcid": "0000-0003-3230-5055", "show_email": "YES" } ] }, "title": "The Multiplicity of T Tauri Stars in the Star Forming Regions Taurus-Auriga and Ophiucus-Scorpius: A 2.2 \u00b5m Speckle Imaging Survey", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy; binary stars; high angular resolution imaging; T Tauri stars; young stars", "note": "The Nobel Prize in Physics 2020 was divided, one half awarded to Roger Penrose \"for the discovery that black hole formation is a robust prediction of the general theory of relativity\", the other half jointly to Reinhard Genzel and Andrea Ghez \"for the discovery of a supermassive compact object at the centre of our galaxy.\"", "abstract": "We present the results of a magnitude limited (K \u2264 8.5 mag) multiplicity survey of T Tauri stars (TTS) in two nearby star forming regions (SFR), Taurus-Auriga and Ophiuchus-Scorpius. Each of the 69 stars in the sample was observed at K(2.2 \u00b5m) with an infrared array camera on the Hale 5-m Telescope at Palomar Observatory and imaged using two-dimensional speckle interferometric techniques.
\r\n\r\nThirty three companion stars were found, of which 15 were new detections. A subset of 64 observations was sensitive to all companion stars in the projected linear range 14 to 225 AU and the magnitude difference range 0.0 to 2.0 mag. We used this subset and region to study the multiplicity of TTS; the frequency of companion stars within this region is 34 \u00b1 9%, independent of SFR. We discovered a distinction between the classical TTS (CTTS) and the weak-lined TTS (WTTS) based on the binary star frequency as a function of separation; the WITS dominate the binary star distribution at the closer separations and the CTTS populate the wider separations. The cross over occurred near 100 AU, the size typically quoted for a circumstellar disk. We suggest that all TTS begin as CTTS and become WTTS when accretion has ceased, and that the nearby companion stars act to shorten the accretion timescale in multiple star systems.
\r\n\r\nIntegrated over all magnitude differences the binary star frequency in the projected linear separation range 14 to 225 AU for TTS (59 \u00b1 16%) is a factor of 3.5 greater than that of the solar-type main sequence stars (17 \u00b1 3%). Given the limited angular separation range that we are sensitive to, i.e., both the spectroscopic and wide binaries are missed, the rate at which binaries are detected suggests that most, if not all, TTS stars have companions. We propose that the observed overabundance of companions to TTS with respect to their older counterparts on the main sequence is an evolutionary effect; in this scheme triple and higher order TTS, which are observed at higher frequencies than for the solar-type main sequence stars, are disrupted by close encounters with another star or system of stars.
", "date": "1993", "date_type": "degree", "id_number": "CaltechETD:etd-10072004-143305", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10072004-143305", "related_url": { "items": [ { "description": "Nobel Prize announcement (Physics, 2020)", "type": "org", "url": "https://www.nobelprize.org/prizes/physics/2020/summary/" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Pacific Telesis Foundation" }, { "agency": "Amelia Earhart Fellowship" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Nobel Prize", "Astronomy Department", "Caltech Distinguished Alumni Award" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-10-08", "doi": "10.7907/AD5X-DA38", "alt_title": { "items": [ "The Multiplicity of T Tauri Stars in the Star Forming Regions Taurus-Auriga and Ophiucus-Scorpius: A 2.2 Micrometer Speckle Imaging Survey" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "chair" }, { "email": "scf@theory.caltech.edu", "id": "Frautschi-S-C", "name": { "family": "Frautschi", "given": "Steven C." }, "role": "member" }, { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "member" }, { "email": "afs@astro.caltech.edu", "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "role": "member" }, { "email": "bts@irastro.caltech.edu", "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-10-07", "thesis_defense_date": "1992-09-29", "thesis_approved_date": "2004-10-08", "thesis_awards": "The Nobel Prize in Physics, 2020.\r\nCaltech Distinguished Alumni Award, 2012", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1993", "author_list": "Ghez, Andrea Mia" }, { "id": "/id/eprint/3743", "eprint_id": 3743, "rev_number": 9, "documents": [ { "id": "/id/document/6360", "doc_id": 6360, "rev_number": 3, "files": [ { "id": "/id/file/38181", "fileid": 38181, "datasetid": "document", "objectid": 6360, "filename": "Tinney_cg_1993.pdf", "mime_type": "application/pdf", "filesize": 10663227, "mtime": "2012-12-26 03:02:35", "url": "/3743/1/Tinney_cg_1993.pdf" } ], "eprint_id": 3743, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Tinney_cg_1993.pdf", "language": "en", "security": "public", "license": "other", "main": "Tinney_cg_1993.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22898" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22898" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22898" } ] } }, { "id": "/id/document/22898", "doc_id": 22898, "rev_number": 3, "files": [ { "id": "/id/file/38179", "fileid": 38179, "datasetid": "document", "objectid": 22898, "filename": "preview.png", "mime_type": "image/png", "hash": "1bff26d81766b9e841008c562cfc777d", "hash_type": "MD5", "filesize": 7012, "mtime": "2012-12-26 03:02:35", "url": "/3743/2/preview.png" } ], "eprint_id": 3743, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6360" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6360" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6360" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/43", "datestamp": "2008-10-24", "lastmod": "2021-04-16 22:24:34", "status_changed": "2009-09-25 03:04:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tinney-C-G", "name": { "family": "Tinney", "given": "Christopher G." }, "show_email": "NO" } ] }, "title": "The faintest stars", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nWe construct a 270 square degree photometric catalogue from plate material of the UKSRC and POSSII surveys. The procedures used and quality checks applied are described in detail, and should be considered as illustrative for those planning scientific programmes with the forthcoming scans of these surveys.\n\nInfrared JHKLL' photometry and low resolution infrared spectra (\u03bb \u2248 1.0-2.5\u03bcm) for a selection of the latest stars known are presented. The combined photometric and spectral data are used to evaluate bolometric corrections and bolometric magnitudes for late type M-dwarfs almost 2-magnitudes fainter than the faintest previously measured objects. We examine some of the current problems associated with the effective temperature scale for very low mass stars.\n\nFirst results are presented from a CCD trigonometric parallax programme at the Palomar 60\" telescope. We double the number of extremely late M-dwarfs (M[subscript bol] > 13) with directly measured distances. Structure in the main sequences so constructed suggest that the faintest known stars may not be stably supported by nuclear burning. We show that \u03c3(\u03c0) \u2264 0.004\" can be obtained in a few years using standard CCDs on a common-user telescope.\n\nWe present infrared K-band photometry of complete samples of VLM candidates selected by our photographic catalogues, and construct a bolometric luminosity function which extends to M[subscript Bol] = 13.75. We find significant evidence for a luminosity function decreasing towards these luminosities. We also find that our data are consistent with the results of studies based on the Nearby Star sample. We convert our observed LF into the form of a mass function which extends with reasonable statistics to 0.08M[...] \u2014 the H-burning minimum mass. The mass function 'turns over' at \u2248 0.25M[...], goes through a local minimum at \u2248 0.15M[...], and seems to increase again below 0.1M[...] \u2014 none of these features are predicted by any of the current theories of star formation. Lastly, the mass density we observe just above the H-burning minimum mass makes it difficult to envisage brown dwarfs contributing significant quantities of missing mass without invoking either a mass function in this region significantly steeper than that seen for main sequence stars, or an extremely low cut-off mass to the mass function.\n", "date": "1993", "date_type": "degree", "id_number": "CaltechETD:etd-09242008-091045", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09242008-091045", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-24", "doi": "10.7907/0wrn-f607", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "advisor" }, { "id": "Reid-N", "name": { "family": "Reid", "given": "Neill" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "chair" }, { "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "role": "member" }, { "id": "Reid-N", "name": { "family": "Reid", "given": "Neill" }, "role": "member" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-24", "thesis_defense_date": "1992-10-29", "thesis_approved_date": "2008-10-24", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1993", "author_list": "Tinney, Christopher G." }, { "id": "/id/eprint/3261", "eprint_id": 3261, "rev_number": 10, "documents": [ { "id": "/id/document/5764", "doc_id": 5764, "rev_number": 3, "files": [ { "id": "/id/file/34149", "fileid": 34149, "datasetid": "document", "objectid": 5764, "filename": "Anderson_sb_1993.pdf", "mime_type": "application/pdf", "filesize": 3983715, "mtime": "2012-12-26 02:58:34", "url": "/3261/1/Anderson_sb_1993.pdf" } ], "eprint_id": 3261, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Anderson_sb_1993.pdf", "language": "en", "security": "public", "license": "other", "main": "Anderson_sb_1993.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22305" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22305" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22305" } ] } }, { "id": "/id/document/22305", "doc_id": 22305, "rev_number": 3, "files": [ { "id": "/id/file/34147", "fileid": 34147, "datasetid": "document", "objectid": 22305, "filename": "preview.png", "mime_type": "image/png", "hash": "6745b73a6458da4a9d151a6e64e9a580", "hash_type": "MD5", "filesize": 19172, "mtime": "2012-12-26 02:58:34", "url": "/3261/2/preview.png" } ], "eprint_id": 3261, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5764" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5764" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5764" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/61", "datestamp": "2008-08-28", "lastmod": "2021-04-16 23:13:46", "status_changed": "2009-09-25 02:55:28", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Anderson-Stuart-Bruce", "name": { "family": "Anderson", "given": "Stuart Bruce" }, "show_email": "NO" } ] }, "title": "A study of recycled pulsars in globular clusters", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nWe have performed a search for radio pulsars in 11 globular clusters visible from the 305 m Arecibo radio telescope. We have found 11 pulsars in the four clusters: M53, M13, NGC6760, and M15; each containing one binary pulsar: 1310+18A, 1639+36B, 1908+00A, and 2127+11C, respectively; as well as a total of seven isolated pulsars: 1639+36A, 2127+11B, 2127+11D, 2127+11E, 2127+11F[superscript 1], 2127+11G, 2127+11H[superscript 1].\r\n\r\nIn this thesis we present the various search strategies employed and discuss the results of pulse time of arrival analysis for the seven isolated pulsars and the binary pulsar 2127+11C, as well as initial Doppler orbits for the binary pulsars 1310+18A and 1639+36B. The remaining pulsar 1908+00A is the subject of current research.\r\n\r\nThe binary pulsar 2127+11C has been found to be in an 8 hour orbit about another degenerate star. The detection of a relativistic precession of the orbit and time dilation effects constrain the pulsar and companion star masses to be [massive pulsar] = 1.34 \u00b1 .23 [...] and [mass of companion] = 1.37 \u00b1 .23 [...].\r\n\r\nStudy of the radial positions and anomalous spin period derivatives of the seven isolated pulsars in M15 has revealed otherwise unobtainable information on the structure of this post core collapsed globular cluster. From the observed spatial pulsar distribution of [...] it is inferred that the mass of isolated pulsars in M15 is approximately 1.4[...]. From the negative period derivative of PSR 2127+11A,D, it is inferred that the central mass-to-light ratio is > 1.9 [...] /[...] and the central mass density is > 2.7 x 10[superscript 6] [...]pc[superscript -3].\r\n\r\nFrom the observed isolated pulsar luminosity function in M15, [...] and an assumed minimum luminosity of 1.0 mJy kpc[superscript 2] it is inferred that the current population of observable isolated pulsars in M15 is [...](100).\r\n\r\nThe observed dispersion measures towards the eight pulsars in M15 and their relative spatial positions indicate that the spectrum of inhomogeneities in the interstellar medium observed at smaller length scales, extends up to 10[superscript 17] cm.\r\n", "date": "1993", "date_type": "degree", "id_number": "CaltechETD:etd-08282008-094151", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08282008-094151", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-08-28", "doi": "10.7907/mb1s-an45", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-28", "thesis_defense_date": "1992-09-23", "thesis_approved_date": "2008-08-28", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1993", "author_list": "Anderson, Stuart Bruce" }, { "id": "/id/eprint/7382", "eprint_id": 7382, "rev_number": 20, "documents": [ { "id": "/id/document/34478", "doc_id": 34478, "rev_number": 3, "files": [ { "id": "/id/file/109398", "fileid": 109398, "datasetid": "document", "objectid": 34478, "filename": "Reisenegger_ta_1993.pdf", "mime_type": "application/pdf", "hash": "7c6881c42e4bc9299f41d6ecc9bf5593", "hash_type": "MD5", "filesize": 18339616, "mtime": "2013-01-08 23:29:40", "url": "/7382/1/Reisenegger_ta_1993.pdf" } ], "eprint_id": 7382, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Reisenegger_ta_1993.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"/id/document/45820", "doc_id": 45820, "rev_number": 3, "files": [ { "id": "/id/file/134324", "fileid": 134324, "datasetid": "document", "objectid": 45820, "filename": "Reisenegger Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "31fa181c715c46fd97157f971632f802", "hash_type": "MD5", "filesize": 624, "mtime": "2014-02-10 22:19:56", "url": "/7382/8/Reisenegger Thesis Permission Form.txt" } ], "eprint_id": 7382, "pos": 8, "placement": 8, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "author ok feb 2014", "language": "en", "security": "internal", "license": "other", "main": "Reisenegger Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/127842", "doc_id": 127842, "rev_number": 1, "files": [ { "id": "/id/file/373278", "fileid": 373278, "datasetid": "document", "objectid": 127842, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "5a409046d8a7c8afc72baf6f6e61d3ee", "hash_type": "MD5", "filesize": 23735, "mtime": "2021-06-24 02:09:55", "url": "/7382/9/indexcodes.txt" } ], "eprint_id": 7382, "pos": 9, "placement": 9, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/34478" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/34478" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/34478" } ] } } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/73/82", "datestamp": "2013-01-08 23:46:05", "lastmod": "2020-03-10 19:14:36", "status_changed": "2013-01-08 23:46:05", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "areisene@astro.puc.cl", "id": "Reisenegger-T-A", "name": { "family": "Reisenegger", "given": "Tassilo Andreas" }, "show_email": "YES" } ] }, "title": "Hydrodynamics of neutron star interiors and laboratory superfluids", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics ; hydrodynamics ; neutron stars ; superfluids", "abstract": "This thesis contains the following papers:
\r\n\r\n1) A new class of g-modes in neutron stars (Astrophys. J., 395, 240 (1992)):\r\nIn the fluid core of a neutron star, the ratio of the number densities of charged\r\nparticles (protons and electrons) to neutrons is an increasing function of the mass\r\ndensity. This composition gradient stably stratifies the matter, giving rise to g-modes\r\nwith periods ranging upward from a few milliseconds. Some of these modes\r\nare computed and their damping mechanisms are discussed.
\r\n\r\n2) Magnetic field decay in isolated neutron stars (Astrophys. J., 395, 250\r\n(1992)): We investigate mechanisms that promote the loss of magnetic flux from\r\nan isolated neutron star. Ambipolar diffusion involves a drift of the magnetic field\r\nand charged particles relative to the neutrons, opposed by frictional drag. Variants\r\nof it include both the buoyant rise and the dragging by superfluid neutron vortices\r\nof magnetic flux tubes. The charged particle flux decomposes into a solenoidal\r\nand an irrotational component. The irrotational component perturbs the chemical\r\nequilibrium, generating pressure gradients that effectively choke it. The solenoidal\r\ncomponent can transport magnetic flux from the outer core to the crust on a short\r\ntimescale. Flux that threads the inner core is permanently trapped unless particle\r\ninteractions can rapidly smooth departures from chemical equilibrium. We speculate\r\nthat Hall drift may lead to a turbulent cascade of the magnetic field in the\r\nsolid crust, terminated by ohmic dissipation at small scales.
\r\n\r\n3) The spin-up problem in helium II (To appear, J. Low Temp. Phys., 92 (1/2)\r\n(July 1993)): The laminar spin-up of helium II is studied by solving the linearized\r\ntwo-fluid equations in a simple case. No direct interactions between vortex lines\r\nand container walls are included. Two mechanisms are identified for the transfer\r\nof angular momentum from the container to the interior fluid. Both involve a\r\npoloidal secondary flow. An analytic expression for the spin-up time is found.
\r\n", "date": "1993", "date_type": "degree", "id_number": "CaltechTHESIS:01082013-145722103", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01082013-145722103", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_on": "2013-01-08 23:46:05", "doi": "10.7907/1FTJ-0J14", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1993-04-30", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1993", "author_list": "Reisenegger, Tassilo Andreas" }, { "id": "/id/eprint/6638", "eprint_id": 6638, "rev_number": 18, "documents": [ { "id": "/id/document/13549", "doc_id": 13549, "rev_number": 4, "files": [ { "id": "/id/file/87896", "fileid": 87896, "datasetid": "document", "objectid": 13549, "filename": "Sigurdsson_s_1992.pdf", "mime_type": "application/pdf", "filesize": 44932033, "mtime": "2012-12-26 04:38:38", "url": "/6638/1/Sigurdsson_s_1992.pdf" } ], "eprint_id": 6638, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Sigurdsson_s_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/13550", "doc_id": 13550, "rev_number": 3, "files": [ { "id": "/id/file/207479", "fileid": 207479, "datasetid": "document", "objectid": 13550, "filename": "Sigurdsson_s_1992.zip", "mime_type": "application/zip", "filesize": 126166024, "mtime": "2016-08-22 21:23:10", "url": "/6638/2/Sigurdsson_s_1992.zip" } ], "eprint_id": 6638, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Sigurdsson_s_1992.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/127004", "doc_id": 127004, "rev_number": 1, "files": [ { "id": "/id/file/372438", "fileid": 372438, "datasetid": "document", "objectid": 127004, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "1fdc927287a43dfd765e97a502172292", "hash_type": "MD5", "filesize": 33644, "mtime": "2021-06-24 01:18:48", "url": "/6638/3/indexcodes.txt" } ], "eprint_id": 6638, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/13549" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13549" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13549" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/00/66/38", "datestamp": "2011-08-31 16:28:08", "lastmod": "2022-11-09 19:20:04", "status_changed": "2011-08-31 16:28:08", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sigurdsson-Steinn", "name": { "family": "Sigurdsson", "given": "Steinn" }, "show_email": "NO" } ] }, "title": "Dynamics of neutron stars and binaries in globular clusters or, M\u00e9nages \u00e0 trois: revitalizing burnt out degenerates through partner swapping", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Interaction cross-sections and collision cross-sections for a set of hard multi-mass binary-single star interactions are calculated in order to estimate three-body collision cross-sections in galactic globular clusters. The cross-sections are calculated by direct integration of binary-single star encounters, using Monte Carlo sampling to average over the three-body phase space. A number of mass-ratios physically relevant to the globular cluster environment are used. Differential energy transfer rates due to three-body interactions are calculated. Parametric\r\napproximations for the various cross-sections calculated are found.\r\n\r\nThe results of the cross-sections are used to evaluate various formation scenarios for the pulsars PSR2127+11C (M15C) and PSR1744-24A (TER5A). In addition the contribution of the globular cluster system to the galactic birthrate of PSR1913+16 type systems is estimated.\r\n\r\nThe dynamics and interactions of a test binary population in a number of globular cluster models are calculated in a static background. The cluster method used are isotropic multi-mass King models of varying concentration and density.\r\nThe model developed is generalisable to an arbitrary cluster distribution function, including one evolving in time. Relative probabilities of different encounters are\r\nfound for binaries on arbitrary trajectories in the various cluster models. The actual interaction rates of the test population are calculated by direct integration, using Monte Carlo sampling to average over the initial binary parameters. The number of neutron stars expected to be recycled in different concentration clusters is estimated with a particular view to understanding the pulsar population observed in clusters 47Tuc and M15.\r\n\r\nEstimates are also made of the binary density profile of the different concentration class clusters, and the final distribution in binary parameters. The production rate of \"blue stragglers\" and the interaction rate of (sub)giants and white dwarfs in the various clusters are also estimated.", "date": "1992", "date_type": "degree", "id_number": "CaltechTHESIS:08312011-085802800", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08312011-085802800", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2011-08-31 16:28:08", "doi": "10.7907/gcf0-px44", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1991-08-01", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1992", "author_list": "Sigurdsson, Steinn" }, { "id": "/id/eprint/6633", "eprint_id": 6633, "rev_number": 17, "documents": [ { "id": "/id/document/13540", "doc_id": 13540, "rev_number": 4, "files": [ { "id": "/id/file/87794", "fileid": 87794, "datasetid": "document", "objectid": 13540, "filename": "Klinkhammer_g_1992.pdf", "mime_type": "application/pdf", "filesize": 33400680, "mtime": "2012-12-26 04:38:36", "url": "/6633/1/Klinkhammer_g_1992.pdf" } ], "eprint_id": 6633, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Klinkhammer_g_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/13541", "doc_id": 13541, "rev_number": 4, "files": [ { "id": "/id/file/207468", "fileid": 207468, "datasetid": "document", "objectid": 13541, "filename": "Klinkhammer_g_1992.zip", "mime_type": "application/zip", "filesize": 55700058, "mtime": "2016-08-22 21:23:10", "url": "/6633/2/Klinkhammer_g_1992.zip" } ], "eprint_id": 6633, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Klinkhammer_g_1992.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/126999", "doc_id": 126999, "rev_number": 1, "files": [ { "id": "/id/file/372433", "fileid": 372433, "datasetid": "document", "objectid": 126999, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "93d2a598b220a443f10f9981b4f6c94d", "hash_type": "MD5", "filesize": 25628, "mtime": "2021-06-24 01:18:22", "url": "/6633/3/indexcodes.txt" } ], "eprint_id": 6633, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/13540" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13540" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13540" } ] } } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/66/33", "datestamp": "2011-08-30 20:16:00", "lastmod": "2022-11-09 19:20:03", "status_changed": "2011-08-30 20:16:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Klinkhammer-G-U", "name": { "family": "Klinkhammer", "given": "Gunnar Ulrich" }, "show_email": "NO" } ] }, "title": "Multiply connected spacetimes and closed timelike curves in semiclassical gravity", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "In this thesis, we present three studies motivated by the recent interest in spacetimes with closed timelike curves (\"CTC's\").\r\n\r\nFirst, it has been shown that certain energy conditions must be violated if spacetime is to develop CTC's. We initiate a study of whether quantum field theory permits such violations by proving that, in Minkowski spacetime, a free scalar field will satisfy the weak and strong energy conditions averaged along any complete null or timelike geodesic. We remark that in fiat, but topologically nontrivial spacetimes, the averaged weak energy condition can be violated.\r\n\r\nSecond, it has been argued that the most likely way by which Nature might prevent the creation of CTC's is a divergent vacuum polarization at the chronology\r\nhorizon where such CTC's first arise. We derive the form of the vacuum polarization of a conformal scalar field and of a spin-1/2 field near a closed null geodesic from which the null generators of a generic compactly generated chronology horizon spring forth. We show that the tensorial structure of the polarization and its degree of divergence are the same for scalar and for spin-1/2 fields and are independent\r\nof the details of the spacetime geometry. We also show that in generic cases, there will be no cancellation of this divergence for a combination of scalar and spin-1/2 fields that has equal numbers of Fermi and Bose degrees of freedom.\r\n\r\nThird, in anticipation of the possibility that Nature might permit CTC's, we demonstrate that for a classical body with a hard-sphere potential and no internal degrees of freedom (a \"billiard ball\") traveling nonrelativistically in a wormhole spacetime with CTC's, the Cauchy problem is ill-posed in a peculiar way. For certain (\"dangerous\") initial data, there would appear to be no self-consistent\r\nsolution to the equations of motion because the ball collides with its younger self after having traversed the wormhole. However, we show that for a wide range of dangerous and non-dangerous initial data, there is an infinity of self-consistent solutions, each involving one self-collision. No initial data are found for which\r\nthere is no self-consistent solution.\r\n", "date": "1992", "date_type": "degree", "id_number": "CaltechTHESIS:08302011-113709010", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08302011-113709010", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_on": "2011-08-30 20:16:00", "doi": "10.7907/694e-b162", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1992-05-15", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1992", "author_list": "Klinkhammer, Gunnar Ulrich" }, { "id": "/id/eprint/6645", "eprint_id": 6645, "rev_number": 20, "documents": [ { "id": "/id/document/13583", "doc_id": 13583, "rev_number": 3, "files": [ { "id": "/id/file/207487", "fileid": 207487, "datasetid": "document", "objectid": 13583, "filename": "Palmer_dm_1992.zip", "mime_type": "application/zip", "filesize": 12086806, "mtime": "2016-08-22 21:23:11", "url": "/6645/2/Palmer_dm_1992.zip" } ], "eprint_id": 6645, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Palmer_dm_1992.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/13584", "doc_id": 13584, "rev_number": 5, "files": [ { "id": "/id/file/88013", "fileid": 88013, "datasetid": "document", "objectid": 13584, "filename": "Palmer_dm_1992.pdf", "mime_type": "application/pdf", "filesize": 5791657, "mtime": "2012-12-26 04:38:40", "url": "/6645/3/Palmer_dm_1992.pdf" } ], "eprint_id": 6645, "pos": 3, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Palmer_dm_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/127013", "doc_id": 127013, "rev_number": 1, "files": [ { "id": "/id/file/372447", "fileid": 372447, "datasetid": "document", "objectid": 127013, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "4be949774165330107a1d9c1c90bc578", "hash_type": "MD5", "filesize": 29322, "mtime": "2021-06-24 01:19:31", "url": "/6645/4/indexcodes.txt" } ], "eprint_id": 6645, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/13584" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13584" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13584" } ] } } ], "eprint_status": "archive", "userid": 51, "dir": "disk0/00/00/66/45", "datestamp": "2011-09-07 18:28:06", "lastmod": "2021-04-16 23:26:00", "status_changed": "2011-09-07 18:28:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Palmer-David-M", "name": { "family": "Palmer", "given": "David M." }, "show_email": "NO" } ] }, "title": "Gamma-ray imaging observations of Supernova 1987A", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "The Caltech imaging \u03b3-ray telescope has made four balloon flights from Alice Springs, Australia, to observe the hard X-ray and \u03b3-ray emission from Supernova 1987 A as it evolved between 1987 May and 1989 April. We have detected \u03b3-rays with the time behavior and spectral signature expected from freshly-synthesized radioisotopes embedded in a cloud of ejecta. In particular, we detect the 847 and 1238 keY \u03b3-ray lines produced by the decay of ^(56)Co, and the continuum spectrum expected from Compton scattering of these \u03b3-trays. The results of these observations are compared with other measurements and with theoretical models of supernovae, and it is found that our results are consistent with core-collapse models for SN 1987A in which the centrally-produced radioisotopes have propagated outwards to mix with the ejecta.\r\n", "date": "1992", "date_type": "degree", "id_number": "CaltechTHESIS:09012011-153518265", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09012011-153518265", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Julie Guan", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_by": "Tony Diaz", "deposited_on": "2011-09-07 18:28:06", "doi": "10.7907/ctqh-qa26", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1992-02-28", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1992", "author_list": "Palmer, David M." }, { "id": "/id/eprint/6688", "eprint_id": 6688, "rev_number": 20, "documents": [ { "id": "/id/document/13643", "doc_id": 13643, "rev_number": 4, "files": [ { "id": "/id/file/88609", "fileid": 88609, "datasetid": "document", "objectid": 13643, "filename": "Achterberg_rk_1992.pdf", "mime_type": "application/pdf", "filesize": 31425622, "mtime": "2012-12-26 04:38:53", "url": "/6688/1/Achterberg_rk_1992.pdf" } ], "eprint_id": 6688, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Achterberg_rk_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/13644", "doc_id": 13644, "rev_number": 4, "files": [ { "id": "/id/file/207535", "fileid": 207535, "datasetid": "document", "objectid": 13644, "filename": "Achterberg_rk_1992.zip", "mime_type": "application/zip", "filesize": 84553366, "mtime": "2016-08-22 21:23:15", "url": "/6688/2/Achterberg_rk_1992.zip" } ], "eprint_id": 6688, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Achterberg_rk_1992.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/127056", "doc_id": 127056, "rev_number": 1, "files": [ { "id": "/id/file/372490", "fileid": 372490, "datasetid": "document", "objectid": 127056, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "7cb3d981a024571cd6c5ebb0a612b841", "hash_type": "MD5", "filesize": 20217, "mtime": "2021-06-24 01:23:25", "url": "/6688/3/indexcodes.txt" } ], "eprint_id": 6688, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/13643" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13643" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13643" } ] } } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/66/88", "datestamp": "2011-09-26 18:42:06", "lastmod": "2023-11-08 00:36:10", "status_changed": "2011-09-26 18:42:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Achterberg-Richard-Karl", "name": { "family": "Achterberg", "given": "Richard Karl" }, "show_email": "NO" } ] }, "title": "Numerical Simulation of Baroclinic Jovian Vortices", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science and Astronomy", "abstract": "This thesis consists of two papers on the dynamics of Jovian planet atmospheres. The first paper discusses the uses of a normal-mode expansion in the vertical for modeling\r\nthe dynamics of Jupiter's atmosphere. The second paper uses a non-linear numerical model based on the normal-mode expansion of the first paper to study the dynamics\r\nof baroclinic vortices. The abstracts for the two papers are reproduced below.
\r\n\r\nPaper 1:
\r\n\r\nWe propose a non-linear, quasi-geostrophic, baroclinic model of Jovian atmospheric dynamics, in which vertical variations of velocity are represented by a truncated sum over a complete set of orthogonal functions obtained by a separation of variables of the linearized quasi-geostrophic potential vorticity equation. A set of equations for the time variation of the mode amplitudes in the non-linear case is then derived. We show that for a planet with a neutrally stable, fluid interior instead of a solid lower boundary, the barotropic mode represents motions in the interior, and is not affected by the baroclinic modes. One consequence of this is that a normal mode model with one baroclinic mode is dynamically equivalent to a one layer model with solid lower topography. We also show that for motions in Jupiter's cloudy lower troposphere, the stratosphere behaves nearly as a rigid lid, so that the normal-mode model is applicable to Jupiter. We test the accuracy of the normal-mode model for Jupiter using two simple problems: forced, vertically propagating Rossby waves, using two and three baroclinic modes, and baroclinic instability, using two baroclinic modes. We find that the normal-mode model provides qualitatively correct results,\r\neven with only a very limited number of vertical degrees of freedom.
\r\n\r\nPaper 2:
\r\n\r\nWe examine the evolution of baroclinic vortices in a time dependent, nonlinear numerical model of a Jovian atmosphere. The model uses a normal-mode expansion in the vertical, using the barotropic and first two baroclinic modes (Achterberg and Ingersoll 1989). Our results for the stability of baroclinic vortices on an \u0192-plane in the absence of a mean zonal flow are consistent with previous results in the literature, although the presence of the deep fluid interior on the Jovian planets appears to shift the stability boundaries to smaller length scales. The presence of a mean zonal shear flow acts to stabilize vortices against instability, significantly modifies\r\nthe finite amplitude form of baroclinic instabilities, and combined with internal barotropic instability (Gent and McWilliams 1986) produces periodic oscillations in the\r\nlatitude and longitude of the vortex as observed at the level of the cloud tops. This instability may explain some, but not all, observations of longitudinal oscillations of\r\nvortices on the outer planets. Oscillations in aspect ratio and orientation of stable elliptical vortices in a zonal shear flow are observed in this baroclinic model, as in\r\nsimpler two-dimensional models (Kida 1981). The meridional propagation and decay of vortices on a \u03b2-plane is inhibited by the presence of a mean zonal flow. The direction of propagation of a vortex relative to the mean zonal flow depends upon the sign of the meridional potential vorticity gradient; combined with observations of vortex drift rates, this may provide a constraint on model assumption for the flow in the deep interior of Jupiter.
\r\n", "date": "1992", "date_type": "degree", "id_number": "CaltechTHESIS:09262011-111706613", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09262011-111706613", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_on": "2011-09-26 18:42:06", "doi": "10.7907/0pjs-sb11", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" }, { "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1991-10-03", "review_status": "approved", "option_major": { "items": [ "plansci", "astronomy" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1992", "author_list": "Achterberg, Richard Karl" }, { "id": "/id/eprint/3139", "eprint_id": 3139, "rev_number": 12, "documents": [ { "id": "/id/document/5584", "doc_id": 5584, "rev_number": 3, "files": [ { "id": "/id/file/32981", "fileid": 32981, "datasetid": "document", "objectid": 5584, "filename": "vanPutten_mhpm_1992.pdf", "mime_type": "application/pdf", "filesize": 6302571, "mtime": "2012-12-26 02:57:24", "url": "/3139/1/vanPutten_mhpm_1992.pdf" } ], "eprint_id": 3139, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "vanPutten_mhpm_1992.pdf", "language": "en", "security": "public", "license": "other", "main": "vanPutten_mhpm_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22127" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22127" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22127" } ] } }, { "id": "/id/document/22127", "doc_id": 22127, "rev_number": 3, "files": [ { "id": "/id/file/32979", "fileid": 32979, "datasetid": "document", "objectid": 22127, "filename": "preview.png", "mime_type": "image/png", "hash": "f3d121490af61d6e0264310a83ce98fa", "hash_type": "MD5", "filesize": 13742, "mtime": "2012-12-26 02:57:24", "url": "/3139/2/preview.png" } ], "eprint_id": 3139, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5584" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5584" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5584" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/39", "datestamp": "2007-08-23", "lastmod": "2023-07-12 21:17:50", "status_changed": "2009-09-25 02:52:19", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "van-Putten-M-H-P-M", "name": { "family": "van Putten", "given": "Maurice H. P. M." }, "orcid": "0000-0002-9212-411X", "show_email": "NO" } ] }, "title": "MHD in divergence form : a computational method for astrophysical flow", "ispublished": "unpub", "full_text_status": "public", "keywords": "Applied and Computational Mathematics", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe equations of MHD in curved space-time are presented in divergence form for the purpose of numerical implementation. This result follows from a covariant divergence form of the single fluid theory of electro-magneto-hydrodynamics in curved space-time with general constitutive relations.\r\n\r\nSome one- and two-dimensional shock computations are given. A pseudospectral method with weak smoothing is used in all of our computations. The pseudo-spectral method is constructed by consideration of Riemann problems in one dimension. The power of MHD in divergence form is brought about by using uniform grid-spacing and explicit time-stepping. The problems considered are shock-tube problems in transverse MHD with analytical comparison solution and a coplanar Riemann problem as discussed for nonrelativistic MHD in Brio and Wu [37]. In a limit of nonrelativistic velocities comparison is made of the results of the latter with those in [37]. In two dimensions cylindrically symmetric problems are considered for test of isotropy, independence of coordinate system and convergence (using comparison results in polar coordinates). We conclude with a computation of a shock induced vortex in jet flow with [...] 2.35, a relativistic jet computation with [...] 3.25 and, finally, computations on magnetic pressure dominated stagnation points in a 2D shock problem in nontransverse MHD.\r\n\r\nThis work is proposed for numerical study of astrophysical flows, and in particular as a \"vehicle\" towards the origin of jets.", "date": "1992", "date_type": "degree", "id_number": "CaltechETD:etd-08152007-144037", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08152007-144037", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-08-23", "doi": "10.7907/263j-a556", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-08-15", "thesis_defense_date": "1992-05-18", "thesis_approved_date": "2007-08-23", "review_status": "approved", "option_major": { "items": [ "appliedmath" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1992", "author_list": "van Putten, Maurice H. P. M." }, { "id": "/id/eprint/3601", "eprint_id": 3601, "rev_number": 8, "documents": [ { "id": "/id/document/6173", "doc_id": 6173, "rev_number": 3, "files": [ { "id": "/id/file/36936", "fileid": 36936, "datasetid": "document", "objectid": 6173, "filename": "Johnston_hm_1992.pdf", "mime_type": "application/pdf", "filesize": 6852064, "mtime": "2012-12-26 03:01:15", "url": "/3601/1/Johnston_hm_1992.pdf" } ], "eprint_id": 3601, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Johnston_hm_1992.pdf", "language": "en", "security": "public", "license": "other", "main": "Johnston_hm_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22711" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22711" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22711" } ] } }, { "id": "/id/document/22711", "doc_id": 22711, "rev_number": 3, "files": [ { "id": "/id/file/36934", "fileid": 36934, "datasetid": "document", "objectid": 22711, "filename": "preview.png", "mime_type": "image/png", "hash": "ad19da13db2ae518ba9f2bd505b3bb77", "hash_type": "MD5", "filesize": 8803, "mtime": "2012-12-26 03:01:15", "url": "/3601/2/preview.png" } ], "eprint_id": 3601, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6173" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6173" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6173" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/36/01", "datestamp": "2008-11-03", "lastmod": "2021-04-19 22:33:11", "status_changed": "2009-09-25 03:01:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Johnston-H-M", "name": { "family": "Johnston", "given": "Helen Margaret" }, "show_email": "NO" } ] }, "title": "Compact objects in the disk and globular clusters", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThis thesis presents a multi-wavelength study of compact objects in globular clusters and in the disk. It is divided into two sections, and contains seven independent chapters, linked by the general theme of the study of the evolution and distribution of recycled pulsars and low mass X-ray binaries.\n\nPart I deals with pulsars in globular clusters. Clusters appear to contain large numbers of pulsars, and this section is devoted to analyzing the pulsar content of the globular cluster system. The smearing of a pulsar signal in a binary orbit is analyzed numerically, and empirical relations between the observing time and the parameters of detectable binaries are presented. It appears that current searches should already have found a large fraction of cluster pulsars.\n\nIn Chapter 3, sensitive VLA images of four clusters are presented. No emission is detected from the dense cluster Liner 1, which suggests that the pulsar population of a cluster is not dependent only on its density. Seven unidentified sources are detected in or near the cores of three clusters. There appears to be no large population of pulsars in tight binaries.\n\nIn Chapter 4, the ultra-short period binary 411 1820-30 in NGC 6624 is detected at 1.4 GHz. The source is confirmed to be several arc seconds away from the cluster core, implying its negative period derivative cannot be due to gravitational acceleration by the cluster. It is suggested that identification of cluster X-ray sources via their radio emission is a potentially powerful tool.\n\nIn Chapter 5, a statistical analysis of all previous pulsar surveys, as well as new VLA and Westerbork observations, is used to derive the cluster pulsar luminosity function and the cluster density weighting function. The derived luminosity function is very similar to that of disk pulsars, and the density weighting function scales significantly less steeply than predicted by the tidal capture model. It is suggested that this may be due to the importance of single star-binary interactions.\n\nPart II presents optical spectroscopy of a variety of compact binaries in the disk. Chapter 6 presents observations of the X-ray nova A0620-00. The mass of the compact object is confirmed to be above the maximum allowed mass for a neutron star, and therefore must be a black hole. More stringent limits are placed on the black hole mass by analysis of the emission lines from the disk.\n\nChapter 7 presents spectroscopy of the recurrent nova U Scorpii, which has been argued to be a very massive white dwarf, M ~ 1.4 M[...]. As a candidate for a white dwarf which may collapse to form a neutron star, this object is highly interesting for understanding the evolution of millisecond pulsars and LMXBs. From analysis of the absorption lines, an upper limit is placed on the mass of the white dwarf: M [...] 0.9 M[...](3\u03c3). Hydrogen is also detected in absorption, suggesting that the observed high helium abundance in the emission lines is not due to the nature of the companion. Thus it appears there is no viable model for this interesting source.\n\nIn Chapter 8, radial velocities of nine disk LMXBs are presented. These are considered in the light of the direct formation model for LMXBs, where the neutron star is formed by the supernova explosion of a massive star in a binary system. With the inclusion of a random kick given to the neutron star at birth, the observations are found to be consistent with this model.\n", "date": "1992", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-152100", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-152100", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-03", "doi": "10.7907/828h-3x32", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "1992-05-04", "thesis_approved_date": "2008-11-03", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1992", "author_list": "Johnston, Helen Margaret" }, { "id": "/id/eprint/3667", "eprint_id": 3667, "rev_number": 12, "documents": [ { "id": "/id/document/6269", "doc_id": 6269, "rev_number": 3, "files": [ { "id": "/id/file/37558", "fileid": 37558, "datasetid": "document", "objectid": 6269, "filename": "Padgett_dl_1992.pdf", "mime_type": "application/pdf", "filesize": 7141093, "mtime": "2012-12-26 03:01:56", "url": "/3667/1/Padgett_dl_1992.pdf" } ], "eprint_id": 3667, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Padgett_dl_1992.pdf", "language": "en", "security": "public", "license": "other", "main": "Padgett_dl_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22807" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22807" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22807" } ] } }, { "id": "/id/document/22807", "doc_id": 22807, "rev_number": 3, "files": [ { "id": "/id/file/37556", "fileid": 37556, "datasetid": "document", "objectid": 22807, "filename": "preview.png", "mime_type": "image/png", "hash": "a34b3d3acabf070b87ac687dde0bb57e", "hash_type": "MD5", "filesize": 9828, "mtime": "2012-12-26 03:01:56", "url": "/3667/2/preview.png" } ], "eprint_id": 3667, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6269" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6269" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6269" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/36/67", "datestamp": "2008-11-06", "lastmod": "2021-04-16 23:15:50", "status_changed": "2009-09-25 03:03:08", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Padgett-D-L", "name": { "family": "Padgett", "given": "Deborah Lynne" }, "show_email": "NO" } ] }, "title": "Photospheric abundance analysis of low mass pre-main sequence stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "The atmospheres of low mass pre-main sequence stars are extremely valuable tools for probing the composition of the star-forming interstellar medium. This thesis investigation uses photospheric abundance analysis techniques to determine metal abundances both for individual weakly active T Tauri stars and the molecular clouds with which these stars are associated. Using the high resolution echelle spectrographs of the Palomar 1.5m and the Las Campanas Observatory 2.5m telescopes, high signal-to-noise ratio spectra have been obtained for 53 low mass pre-main sequence stars in six major northern and southern hemisphere star formation regions. Spectra were also taken of 14 main sequence stars with known effective temperatures and metallicity to serve as spectral standards. Equivalent widths of a large number of Fe I absorption lines have been measured, as well as lines of Ca I, Al I, V I, Ni I, Ti I, K I, and Li I. Temperature-sensitive line ratios of neutral iron and vanadium calibrated against the spectral standards are used to derive effective temperatures for 30 weak-line T Tauri stars, which are much improved over the low resolution spectral classifications found for these objects in the literature. Micro-turbulent velocities have also been found for 16 of the pre-main sequence stars in the sample. Several stars with abnormally high microturbulences for their spectral type have been found.
\r\n\r\nUsing these improved stellar parameters, metallicities of a large number of T Tauri stars have been determined for the first time. Abundance analyses of iron, aluminum, calcium, nickel, and titanium are performed on 30 low mass, pre-main sequence stars. In the star-formation regions of Taurus-Auriga, Orion, Chamaeleon, and Ophiuchus, which each contributed five or more association members to the young star survey, bulk metallicities have been determined. The results indicate that the current metal abundances in these clouds are near or slightly above solar values. Cloud material metallicities are then used to calibrate ultraviolet line-ofsight metal depletion studies for the Orion and \u03c1 Ophiuchi clouds.
\r\n\r\nThe final chapter of this work is a lithium abundance analysis for the entire sample of 53 pre-main sequence stars. Statistics performed on a subset of 37 T Tauri stars without veiling give a mean lithium abundance of 3.60 \u00b1 0.07 on the logarithimic scale relative to log N(H) = 12, and a few stars have derived abundances in excess of 4.0. The mean lithium values among pre-main sequence stars are considerably higher than the maximum values of 3.1 - 3.2 derived for young main sequence cluster stars, indicating that the processes of lithium destruction are quite rapid for low mass stars during the transition onto the main sequence. Although an appreciable spread in lithium abundances are found among the stars in each pre-main sequence star association, no significant difference in mean or maximum lithium abundances are seen between the clusters.
\r\n", "date": "1992", "date_type": "degree", "id_number": "CaltechETD:etd-09202008-104122", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09202008-104122", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-06", "doi": "10.7907/wxz8-y734", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" }, { "id": "Boesgaard-A-M", "name": { "family": "Boesgaard", "given": "Ann Merchant" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-20", "thesis_defense_date": "1991-10-31", "thesis_approved_date": "2008-11-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1992", "author_list": "Padgett, Deborah Lynne" }, { "id": "/id/eprint/3732", "eprint_id": 3732, "rev_number": 17, "documents": [ { "id": "/id/document/6348", "doc_id": 6348, "rev_number": 3, "files": [ { "id": "/id/file/38095", "fileid": 38095, "datasetid": "document", "objectid": 6348, "filename": "Zuo_l_1992.pdf", "mime_type": "application/pdf", "filesize": 5413308, "mtime": "2012-12-26 03:02:30", "url": "/3732/1/Zuo_l_1992.pdf" } ], "eprint_id": 3732, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Zuo_l_1992.pdf", "language": "en", "security": "public", "license": "other", "main": "Zuo_l_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22886" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22886" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22886" } ] } }, { "id": "/id/document/22886", "doc_id": 22886, "rev_number": 3, "files": [ { "id": "/id/file/38093", "fileid": 38093, "datasetid": "document", "objectid": 22886, "filename": "preview.png", "mime_type": "image/png", "hash": "669a084da59ad270865344839d5525da", "hash_type": "MD5", "filesize": 8658, "mtime": "2012-12-26 03:02:30", "url": "/3732/2/preview.png" } ], "eprint_id": 3732, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6348" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6348" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6348" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/32", "datestamp": "2008-11-06", "lastmod": "2021-04-23 20:31:31", "status_changed": "2009-09-25 03:04:22", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zuo-Lin", "name": { "family": "Zuo", "given": "Lin" }, "show_email": "NO" } ] }, "title": "QSO Absorption Lines and the Ionizing Field at High Redshifts", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "In this thesis we explore the relationship between the QSO absorption line systems and the metagalactic ionizing field at high redshifts.
\r\n\r\nIn the first introductory chapter we describe the recent developments in the field of QSO absorption lines and the ionizing radiation background. We concentrate on compiling the new observational results and address why studies of QSO absorption line systems and ionizing field are important to our understandings of the formation and evolution of the large scale structure of the universe.
\r\n\r\nIn the second chapter Markoff's method has been used to derive a general formalism to deal with the absorptions produced by randomly distributed discrete clouds, such as the QSO absorption line systems. Some analytical forms are obtained for the effective optical depth \u03c4eff, the count reduction factor fc, and the optical depth probability distribution function P(\u03c4). We demonstrate that the spectrum of ionizing background is very different from the intrinsic source spectrum. We calculate the QSO contributions to J\u03bdL(Zobs) by using simple analytical expressions. We show that because of the Lyman continuum absorption produced by QSO absorption line systems, it is very difficult to find a \"clear\" line of sight to conduct the Hell Gunn-Peterson test. We have also found that dust grains in the QSO damped Ly\u03b1 systems produce a marginally significant obscuration for z = 3 quasars: the count reduction factor is 1⁄1.7 at z = 3. The reddening is shown to be small for a flux limited QSO sample.
\r\n\r\nIn the following two chapters we discuss fluctuations and intensity correlation in the ionizing field. We derive the intensity probability distribution function P(J) for randomly distributed point sources. We show that absorptions by QSO absorption line systems reduce the total number of sources involved in producing the ionizing background and therefore enhance the fluctuation significantly, if QSOs are the main ionizing sources. We have calculated the intensity correlation function \u03bej for randomly distributed QSOs. The QSO Ly\u03b1 clouds can be used as intensity indicators to reveal the intensity correlation at high redshifts. We have measured the equivalent width correlation function \u03be1⁄w for several selected QSOs and have found, in some cases, strong correlation signals at small separations. Careful examination shows that such signals are mainly generated by the lines near the QSO emission redshifts. One explanation is that the high S⁄N near QSO emission red-shifts enable us to detect very weak lines which result in the correlation signal. The other explanation is that the correlated intensities of ionizing field near QSOs have caused the observed equivalent width correlation. If this latter explanation is correct, from the affected range by QSOs we conclude that J\u03bdL is less than 10-21 ergs s-1cm-2Hz-1sr-1 at z ~ 3.5.
\r\n\r\nThe last two chapters deal with the ionization structure of the QSO Ly\u03b1 clouds. We solve the coupled ionization balance and radiation transfer problem (the \"inverse HII region\" problem) for the non-uniform spherical absorbing clouds and calculate the HI column density distribution f(N). We show that with an appropriate density gradient in the clouds we can reproduce the observed overall power law distribution and the apparent excess of absorption systems with N \u2265 2 x 1020cm-2. The calculated f(N) is not sensitive to the input ionizing spectra and is a generic feature of the density profile. In our model all QSO absorption lines have the same origin: the ionized outer envelopes produce the Ly\u03b1 forest lines while the neutral cores result in damped Ly\u03b1 systems. We discuss the consequences of such models and propose star-forming dwarf galaxies as primary candidates for QSO absorption line systems. Our calculations also suggest that uniform cloud models are highly unlikely. To calculate the absorptions produced by HeI and HeII in QSO Ly\u03b1 clouds we also solve the ionization structure for the clouds containing both H and He. We explore the variation of HeI and HeII distributions under different input ionizing spectra and discuss how to get a self-consistent spectral shape for the ionizing background.
", "date": "1992", "date_type": "degree", "id_number": "CaltechETD:etd-09232008-081252", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232008-081252", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-06", "doi": "10.7907/vsk7-nv30", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-23", "thesis_defense_date": "1991-11-15", "thesis_approved_date": "2008-11-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1992", "author_list": "Zuo, Lin" }, { "id": "/id/eprint/3589", "eprint_id": 3589, "rev_number": 8, "documents": [ { "id": "/id/document/6161", "doc_id": 6161, "rev_number": 3, "files": [ { "id": "/id/file/36845", "fileid": 36845, "datasetid": "document", "objectid": 6161, "filename": "Picard_a_1991.pdf", "mime_type": "application/pdf", "filesize": 12683229, "mtime": "2012-12-26 03:01:10", "url": "/3589/1/Picard_a_1991.pdf" } ], "eprint_id": 3589, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Picard_a_1991.pdf", "language": "en", "security": "public", "license": "other", "main": "Picard_a_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22699" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22699" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22699" } ] } }, { "id": "/id/document/22699", "doc_id": 22699, "rev_number": 3, "files": [ { "id": "/id/file/36843", "fileid": 36843, "datasetid": "document", "objectid": 22699, "filename": "preview.png", "mime_type": "image/png", "hash": "9d830fce0fb6befa5b8322978bf334fb", "hash_type": "MD5", "filesize": 8072, "mtime": "2012-12-26 03:01:09", "url": "/3589/2/preview.png" } ], "eprint_id": 3589, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6161" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6161" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6161" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/89", "datestamp": "2008-11-03", "lastmod": "2021-04-19 22:35:57", "status_changed": "2009-09-25 03:01:17", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Picard-A", "name": { "family": "Picard", "given": "Alain" }, "show_email": "NO" } ] }, "title": "The large scale structure of the universe", "ispublished": "unpub", "full_text_status": "public", "abstract": "We present a catalogue of galaxies from COSMOS scans of 16 second epoch Palomar Observatory Sky Survey (POSS-II) plates. The surveys covers an area of 386 square degrees, and covers 150,000 galaxies in the magnitude range 16.5 \u2264 r \u2264 19.0. The plates are divided into a north galactic (7 plates, \u03b1 \u2248 15[superscript h]0[superscript m],\u03b4 \u2248 +30\u00b0(1950.0), b \u2248 65\u00b0) and south galactic (9 plates, \u03b1 \u2248 0[superscript h]20[superscript m], \u03b4 \u2248 +5\u00b0(1950.0), b \u2248 -55\u00b0) field.\n\nThe magnitude scale of each plate was brought to a common photometric system (Gunn r) using extensive CCD photometry. The total error in the zero point of the magnitude scale at the faint end is 0.06[superscript m].\n\nThe procedure for separating stars and galaxies is based on image parameters provided by the COSMOS machine and is completely objective. Visual tests indicate that the catalogue is 94% complete.\n\nWe have measured the angular correlation function of galaxies w(\u03b8). The north field is in good agreement with the results of the APM survey. The south field exhibits more power on large scales than the north field. We have performed several tests to determine the effect of possible systematic errors between the two fields and do not find any effect sufficiently large to account for the south field's excess power. The measured correlation function for both fields are incompatible with the predictions of the currently most popular model, cold dark matter (CDM).\n\nThe number counts of galaxies in the two fields are substantially different. Several tests have been performed to make sure that the effect is not the result of a systematic error in zero point of the magnitude system or due to extinction or obscuration. The natural scale for structures which might be responsible for this difference is 50h[superscript -1] Mpc. We do not know if this difference is a rare event; more fields need to be surveyed to address this important question.\n\nWe have developed an objective algorithm for detecting clusters of galaxies from our galaxy catalogue. The algorithm is based on fixed overdensities at varying angular scales, and is well-suited to detecting clusters over a large range of redshifts. We present a catalogue of clusters based on this algorithm, using an overdensity threshold obtained from comparing the cluster's densities to each field's overall back-ground density. The results are very sensitive to the choice of background density. The multiplicity function of the objective clusters agree well when referenced to each field's background density, but disagree sharply when referenced to the overall mean density of the survey.\n\nThe objective catalogue is compared with that of Abell's. Poor agreement is found between the two catalogues. It is not possible to choose a set of parameters in our catalogue which reproduces Abell's catalogue well.\n\nThe measurement of the galaxy-cluster correlation function w[subscript g-cl](\u03b8) is in good qualitative agreement with predictions of CDM, but more detailed comparisons with theory must wait for the acquisition of redshifts for a large fraction of the clusters.\n\nAt present, no theory is able to explain the amount of power on large scale observed in this survey.\n", "date": "1991", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-084234", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-084234", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-03", "doi": "10.7907/hv26-2889", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "1991-05-22", "thesis_approved_date": "2008-11-03", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1991", "author_list": "Picard, Alain" }, { "id": "/id/eprint/2662", "eprint_id": 2662, "rev_number": 10, "documents": [ { "id": "/id/document/4962", "doc_id": 4962, "rev_number": 2, "files": [ { "id": "/id/file/28809", "fileid": 28809, "datasetid": "document", "objectid": 4962, "filename": "Coppi_ps_1991.pdf", "mime_type": "application/pdf", "filesize": 17984809, "mtime": "2012-12-26 02:53:26", "url": "/2662/1/Coppi_ps_1991.pdf" } ], "eprint_id": 2662, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Coppi_ps_1991.pdf", "language": "en", "security": "public", "license": "other", "main": "Coppi_ps_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21512" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21512" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21512" } ] } }, { "id": "/id/document/15874", "doc_id": 15874, "rev_number": 3, "files": [ { "id": "/id/file/203720", "fileid": 203720, "datasetid": "document", "objectid": 15874, "filename": "Coppi_Paolo_1991.txt", "mime_type": "text/plain", "filesize": 1565, "mtime": "2016-08-22 21:16:15", "url": "/2662/2/Coppi_Paolo_1991.txt" } ], "eprint_id": 2662, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Coppi_Paolo_1991.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/21512", "doc_id": 21512, "rev_number": 2, "files": [ { "id": "/id/file/28807", "fileid": 28807, "datasetid": "document", "objectid": 21512, "filename": "preview.png", "mime_type": "image/png", "hash": "4bed88ba482874ba2d6ee133d81b5733", "hash_type": "MD5", "filesize": 8138, "mtime": "2012-12-26 02:53:26", "url": "/2662/3/preview.png" } ], "eprint_id": 2662, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4962" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4962" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4962" } ] } }, { "id": "/id/document/123091", "doc_id": 123091, "rev_number": 1, "files": [ { "id": "/id/file/368498", "fileid": 368498, "datasetid": "document", "objectid": 123091, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "c4beb54a6c9f41c71f6f11e8f2246624", "hash_type": "MD5", "filesize": 828, "mtime": "2021-06-23 22:20:02", "url": "/2662/4/indexcodes.txt" } ], "eprint_id": 2662, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15874" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15874" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15874" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/26/62", "datestamp": "2007-07-16", "lastmod": "2020-03-10 23:06:56", "status_changed": "2009-09-25 02:42:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "paolo.coppi@yale.edu", "id": "Coppi-Paolo-Severo", "name": { "family": "Coppi", "given": "Paolo Severo" }, "show_email": "NO" } ] }, "title": "Radiative processes in active galactic nuclei", "ispublished": "unpub", "full_text_status": "public", "keywords": "active galactic nuclei (AGN); gamm-ray sources; plasmas; radiation mechanisms; X-ray sources", "abstract": "A study of processes relevant to the electron-positron pair plasmas thought to exist in Active Galactic Nuclei is undertaken. The processes considered include: Compton scattering, pair annihilation, two photon pair production, synchrotron emission, e-e bremsstrahlung, and Coulomb scattering. Approximations used in the past to treat these processes in the context of a kinetic code are examined, and improvements are presented. A two-moment scattering formalism is presented to allow for important energy dispersion effects in scattering. This improved treatment of microphysical processes is implemented in a time-dependent, kinetic code incorporating Klein-Nishina effects on both the pair and photon distributions, relativistic thermal Comptonization, and synchrotron reabsorption.\r\n\r\nThe effects of pair plasma reprocessing on the emergent radiation spectrum are examined. Time-varying and stationary spectra are computed. Good qualitative agreement with previous calculations is found, except when the differences are attributable to the improved treatment of the microphysics. These differences can be substantial, particularly in the \"photon-starved\" regime where the effects of Coulomb scattering by suprathermal pairs off thermal pairs significantly modify the spectra. The spectral response of the pair plasma to variations in the particle injection is found to depend sensitively on the plasma parameters. A transitional spectrum may look very different from the spectra of either the stationary initial or final states. The highest energies (gamma-rays) are found to respond most rapidly to changes and should vary more than the X-rays. Pair plasmas can produce soft X-ray excesses. This happens under conditions independently favored by current pair plasma-Compton reflection models of the hard X-ray spectrum.\r\n", "date": "1991", "date_type": "degree", "id_number": "CaltechETD:etd-06202007-132612", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06202007-132612", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-07-16", "doi": "10.7907/GDMQ-Q829", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "advisor" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-06-20", "thesis_defense_date": "1990-10-23", "thesis_approved_date": "2007-07-16", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1991", "author_list": "Coppi, Paolo Severo" }, { "id": "/id/eprint/2690", "eprint_id": 2690, "rev_number": 8, "documents": [ { "id": "/id/document/5001", "doc_id": 5001, "rev_number": 3, "files": [ { "id": "/id/file/29068", "fileid": 29068, "datasetid": "document", "objectid": 5001, "filename": "Han_m_1991.pdf", "mime_type": "application/pdf", "filesize": 26453265, "mtime": "2012-12-26 02:53:42", "url": "/2690/1/Han_m_1991.pdf" } ], "eprint_id": 2690, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Han_m_1991.pdf", "language": "en", "security": "public", "license": "other", "main": "Han_m_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21551" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21551" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21551" } ] } }, { "id": "/id/document/21551", "doc_id": 21551, "rev_number": 3, "files": [ { "id": "/id/file/29066", "fileid": 29066, "datasetid": "document", "objectid": 21551, "filename": "preview.png", "mime_type": "image/png", "hash": "bc6443cc296bec499b7d2d475dc04a2b", "hash_type": "MD5", "filesize": 10371, "mtime": "2012-12-26 02:53:41", "url": "/2690/2/preview.png" } ], "eprint_id": 2690, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5001" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5001" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5001" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/26/90", "datestamp": "2007-07-18", "lastmod": "2021-04-16 23:30:11", "status_changed": "2009-09-25 02:43:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Han-M", "name": { "family": "Han", "given": "Mingsheng" }, "show_email": "NO" } ] }, "title": "The I-band Tully-Fisher relation and large-scale motions in the universe", "ispublished": "unpub", "full_text_status": "public", "abstract": "The ultimate goal of this thesis is to better understand the large-scale motions in the universe on scales beyond the Local-Supercluster, and also to better understand the Tully-Fisher relation as a distance indicator. Sixteen clusters of galaxies in redshifts range from 3000-10000 kms(-1) are studied as test points of the large-scale velocity field, using the I-band Tully-Fisher relation as distance indicator. A complete observational procedure and techniques of measuring cluster distance using the Tully-Fisher relation is investigated in detail, which involves many general topics in the photometric studies of galaxies. Major discussions and results in the thesis are summarized as:\n\n1. CCD surface photometry is described in detail. Errors and various effects (extinction, cosmological and seeing) on surface photometry are discussed. I-band surface photometry is carried out for some 280 galaxies in the thesis sample.\n\n2. The problem of internal absorption in spiral galaxies is investigated; new magnitude and isophotal-diameter corrections for internal absorption are derived.\n\n3. Different techniques for deriving cluster distances using Tully-Fisher relation are compared; distance bias due to sample selection effects is discussed at length; a Maximum-Likelihood method is given which is able to handle the sample selection effects.\n\n4. Global photometric properties of the cluster galaxies are examined; the problem of second parameter in the TF relation is investigated; a physical explanation for the TF relation and its dispersion is proposed.\n\n5. The peculiar velocity field as traced by the sample clusters is found to be highly non-random, and appears to be a coherent flow towards the general direction of the Great Attractor, with a flow amplitude of some 400~600 kms(-1) at the position of the Local Group.", "date": "1991", "date_type": "degree", "id_number": "CaltechETD:etd-06222007-113504", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06222007-113504", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-07-18", "doi": "10.7907/85nr-2g69", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "chair" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-06-22", "thesis_defense_date": "1991-05-01", "thesis_approved_date": "2007-07-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1991", "author_list": "Han, Mingsheng" }, { "id": "/id/eprint/1840", "eprint_id": 1840, "rev_number": 11, "documents": [ { "id": "/id/document/3069", "doc_id": 3069, "rev_number": 3, "files": [ { "id": "/id/file/18465", "fileid": 18465, "datasetid": "document", "objectid": 3069, "filename": "Carico_dp_1991.pdf", "mime_type": "application/pdf", "filesize": 9314671, "mtime": "2012-12-26 02:42:54", "url": "/1840/1/Carico_dp_1991.pdf" } ], "eprint_id": 1840, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Carico_dp_1991.pdf", "language": "en", "security": "public", "license": "other", "main": "Carico_dp_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/35727" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/35727" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/35727" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/18/40", "datestamp": "2007-05-16", "lastmod": "2020-03-10 23:39:05", "status_changed": "2009-09-25 02:17:21", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Carico-D-P", "name": { "family": "Carico", "given": "David Paul" }, "show_email": "NO" } ] }, "title": "Properties of infrared-luminous galaxies, or, how I spent seven summer vacations", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nGalaxies selected from the IRAS database having unusually high 60 - 100\u00b5m luminosities are studied at wavelengths ranging from ~1 - 1000\u00b5m. It is found that these galaxies differ significantly from normal, optically-selected galaxies, not only in their far-infrared luminosities, but in their near-infrared properties as well. A substantial excess emission at near-infrared wavelengths is attributed to emission from hot dust, with temperatures ~500 - 1000 K. Furthermore, this hot dust emission is confined to the central nuclear regions, within characteristic scale sizes ~1 - 3 kpc. This suggests that the bulk of the infrared luminosity, and hence the processes responsible for the extreme activity in infrared-luminous galaxies, is highly localized about galaxy nuclei. High resolution images of a number of these nuclei reveals a high percentage of double-nucleus sources amongst the most luminous galaxies, giving evidence that galaxy-galaxy interactions play a significant role in the generation of high infrared luminosities.\r\n\r\nThe distribution of the mass of, and luminosity from, dust in infrared-luminous galaxies is analyzed as a function of the temperature of the dust. It is found that, in galaxies for which the entire energy distribution is dominated by emission from dust heated to a steady-state, the mass of dust scales with steady-state temperature as [...], where [...] is typically in the range 6 - 6.5. Dust continues to contribute substantially to the total luminosity up to temperatures in excess of 300 K above the temperatures responsible for the peak in the infrared luminosity. At the lowest temperatures, however, it is very difficult to constrain the contribution to the observed emission: For the galaxies studied, the observations are consistent with models in which the amount of very cold dust ranges from essentially non-existent, to the dominant component of the total dust mass.", "date": "1991", "date_type": "degree", "id_number": "CaltechETD:etd-05162007-161518", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05162007-161518", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-16", "doi": "10.7907/XZPT-HV21", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cowan-E-W", "name": { "family": "Cowan", "given": "Eugene W." }, "role": "advisor" }, { "id": "Porter-F-C", "name": { "family": "Porter", "given": "Frank C." }, "role": "advisor" }, { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-16", "thesis_defense_date": "1990-08-09", "thesis_approved_date": "2007-05-16", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1991", "author_list": "Carico, David Paul" }, { "id": "/id/eprint/6291", "eprint_id": 6291, "rev_number": 16, "documents": [ { "id": "/id/document/12273", "doc_id": 12273, "rev_number": 5, "files": [ { "id": "/id/file/80450", "fileid": 80450, "datasetid": "document", "objectid": 12273, "filename": "Salmon_jk_1991.pdf", "mime_type": "application/pdf", "filesize": 10018418, "mtime": "2012-12-26 04:33:49", "url": "/6291/1/Salmon_jk_1991.pdf" } ], "eprint_id": 6291, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Salmon_jk_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/27294" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/27294" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/27294" } ] } }, { "id": "/id/document/12274", "doc_id": 12274, "rev_number": 3, "files": [ { "id": "/id/file/206650", "fileid": 206650, "datasetid": "document", "objectid": 12274, "filename": "Salmon_jk_1991.zip", "mime_type": "application/zip", "filesize": 23315723, "mtime": "2016-08-22 21:21:52", "url": "/6291/2/Salmon_jk_1991.zip" } ], "eprint_id": 6291, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Salmon_jk_1991.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/16427", "doc_id": 16427, "rev_number": 4, "files": [ { "id": "/id/file/206653", "fileid": 206653, "datasetid": "document", "objectid": 16427, "filename": "Salmon_jk_1991.pdf", "mime_type": "application/pdf", "filesize": 54447, "mtime": "2016-08-22 21:21:53", "url": "/6291/3/Salmon_jk_1991.pdf" } ], "eprint_id": 6291, "pos": 3, "format": "application/pdf", "format_desc": "Author OK 2012", "language": "en", "security": "internal", "license": "other", "main": "Salmon_jk_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/73538" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/73538" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/73538" } ] } }, { "id": "/id/document/27294", "doc_id": 27294, "rev_number": 2, "files": [ { "id": "/id/file/80448", "fileid": 80448, "datasetid": "document", "objectid": 27294, "filename": "preview.png", "mime_type": "image/png", "hash": 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"mtime": "2021-06-24 00:55:09", "url": "/6291/8/indexcodes.txt" } ], "eprint_id": 6291, "pos": 8, "placement": 8, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16427" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16427" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16427" } ] } } ], "eprint_status": "archive", "userid": 51, "dir": "disk0/00/00/62/91", "datestamp": "2011-04-11 22:30:33", "lastmod": "2020-03-10 23:11:56", "status_changed": "2011-04-11 22:30:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Salmon-John-K", "name": { "family": "Salmon", "given": "John K." }, "show_email": "NO" } ] }, "title": "Parallel hierarchical N-body methods", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Recent algorithmic advances utilizing hierarchical data structures have resulted\r\nin a dramatic reduction in the time required for computer simulation of N-body\r\nsystems with long-range interactions. Computations which required O(N^2) operations\r\ncan now be done in O(N log N) or O(N). We review these tree methods\r\nand find that they may be distinguished based on a few simple features.\r\nThe Barnes-Hut (BH) algorithm has received a great deal of attention, and\r\nis the subject of the remainder of the dissertation. We present a generalization of\r\nthe BH tree and analyze the statistical properties of such trees in detail. We also\r\nconsider the expected number of operations entailed by an execution of the BH\r\nalgorithm. We find an optimal value for m, the maximum number of bodies in a\r\nterminal cell, and confirm that the number of operations is O(N log N), even if\r\nthe distribution of bodies is not uniform.\r\nThe mathematical basis of all hierarchical methods is the multipole approximation.\r\nWe discuss multipole approximations, for the case of arbitrary, spherically\r\nsymmetric, and Newtonian Green's functions. We describe methods for computing\r\nmultipoles and evaluating multipole approximations in each of these cases,\r\nemphasizing the tradeoff between generality and algorithmic complexity.\r\nN-body simulations in computational astrophysics can require 10^6 or even\r\nmore bodies. Algorithmic advances are not sufficient, in and of themselves, to\r\nmake computations of this size feasible. Parallel computation offers, a priori, the\r\nnecessary computational power in terms of speed and memory. We show how the\r\nBH algorithm can be adapted to execute in parallel. We use orthogonal recursive\r\nbisection to partition space. The logical communication structure that emerges\r\nis that of a hypercube. A local version of the BH tree is constructed in each\r\nprocessor by iteratively exchanging data along each edge of the logical hypercube.\r\nWe obtain speedups in excess of 380 on a 512 processor system for simulations of\r\ngalaxy mergers with 180000 bodies. We analyze the performance of the parallel\r\nversion of the algorithm and find that the overhead is due primarily to interprocessor\r\nsynchronization delays and redundant computation. Communication is not\r\na significant factor.\r\n", "date": "1991", "date_type": "degree", "id_number": "CaltechTHESIS:04112011-113813016", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:04112011-113813016", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Tony Diaz", "deposited_on": "2011-04-11 22:30:33", "doi": "10.7907/3J5V-VR08", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Fox-G-C", "name": { "family": "Fox", "given": "Geoffrey C." }, "role": "advisor" }, { "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1990-12-06", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1991", "author_list": "Salmon, John K." }, { "id": "/id/eprint/3568", "eprint_id": 3568, "rev_number": 8, "documents": [ { "id": "/id/document/6134", "doc_id": 6134, "rev_number": 3, "files": [ { "id": "/id/file/36665", "fileid": 36665, "datasetid": "document", "objectid": 6134, "filename": "Stapelfeldt_kr_1991.pdf", "mime_type": "application/pdf", "filesize": 6186329, "mtime": "2012-12-26 03:00:59", "url": "/3568/1/Stapelfeldt_kr_1991.pdf" } ], "eprint_id": 3568, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Stapelfeldt_kr_1991.pdf", "language": "en", "security": "public", "license": "other", "main": "Stapelfeldt_kr_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22673" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22673" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22673" } ] } }, { "id": "/id/document/22673", "doc_id": 22673, "rev_number": 3, "files": [ { "id": "/id/file/36663", "fileid": 36663, "datasetid": "document", "objectid": 22673, "filename": "preview.png", "mime_type": "image/png", "hash": "c882bd7e80672450011cc98700c46ce8", "hash_type": "MD5", "filesize": 10410, "mtime": "2012-12-26 03:00:59", "url": "/3568/2/preview.png" } ], "eprint_id": 3568, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6134" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6134" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6134" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/68", "datestamp": "2008-10-31", "lastmod": "2021-04-16 22:28:33", "status_changed": "2009-09-25 03:00:56", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stapelfeldt-K-R", "name": { "family": "Stapelfeldt", "given": "Karl Roald" }, "show_email": "NO" } ] }, "title": "A multiwavelength observational investigation of Herbig-Haro objects and their exciting stars", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nHerbig-Haro objects are small optical emission line nebulae, shock-heated by collimated winds from young stars. In this thesis, near-infrared imaging and high resolution optical imaging spectroscopy have been used to investigate Herbig-Haro object shock structure. Four objects have been studied: HH 7-11, HH 12, HH 34, and HH 1. By a detailed comparison of emission line images and spatially complete kinematic maps, we find that although no single flow model can be applied to all regions, some regions do fit the existing models quite well. HH 7 is well-described as the working surface of a stellar jet, with both a bowshock and a jet terminus shock identified within it. The density of this jet is shown to be comparable to the density of the medium it is impacting. Based on the absence of 2[...] H2 line emission in the shocked wind material, H2 does not appear to be a major constituent of the outflowing winds. Where H2 emission is found, the associated [S II] emission tends to have lower radial velocities. The 1.64 [...] [Fe II] emission line has been imaged for the first time in HH objects. The [Fe II] images indicate extinction is not significant in determining the optical appearance of the HH objects studied, and thus the HH 34 bipolar outflow is indeed a one-sided jet system. The kinematics and H2 morphology of HH 12 argue for SVS 12 as this object's exciting star, a conclusion which strongly suggests that the observed proper motions in this object represent pattern motion rather than a material velocity.\n\nThe second part of this work is a study of the circumstellar material of two HH object exciting stars using millimeter-wave interferometry. High resolution [...]CO images suggest that the HH 34 and HH 111 exciting stars both possess circumstellar disks elongated perpendicular to the highly collimated optical jets emerging from these two sources. The masses of these disks are two to four times greater than the disk masses found for T Tauri stars, although the sizes are comparable. The stellar source masses are most likely less than 2 M[...]. The total weight of evidence argues that HH exciting stars represent an earlier stage of stellar evolution than T Tauri stars, and that large disk masses are being accreted onto the central star, dispersed by the outflow winds, and/or formed into planets during the earliest phases of the life of a star.\n", "date": "1991", "date_type": "degree", "id_number": "CaltechETD:etd-09162008-083954", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09162008-083954", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-31", "doi": "10.7907/2638-br68", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-16", "thesis_defense_date": "1991-05-28", "thesis_approved_date": "2008-10-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1991", "author_list": "Stapelfeldt, Karl Roald" }, { "id": "/id/eprint/3569", "eprint_id": 3569, "rev_number": 11, "documents": [ { "id": "/id/document/6135", "doc_id": 6135, "rev_number": 3, "files": [ { "id": "/id/file/36673", "fileid": 36673, "datasetid": "document", "objectid": 6135, "filename": "Rand_rj_1991.pdf", "mime_type": "application/pdf", "filesize": 6498842, "mtime": "2012-12-26 03:00:59", "url": "/3569/1/Rand_rj_1991.pdf" } ], "eprint_id": 3569, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Rand_rj_1991.pdf", "language": "en", "security": "public", "license": "other", "main": "Rand_rj_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22674" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22674" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22674" } ] } }, { "id": "/id/document/22674", "doc_id": 22674, "rev_number": 3, "files": [ { "id": "/id/file/36671", "fileid": 36671, "datasetid": "document", "objectid": 22674, "filename": "preview.png", "mime_type": "image/png", "hash": "935f2ca905b1637075595cd670ce4b6c", "hash_type": "MD5", "filesize": 8569, "mtime": "2012-12-26 03:00:59", "url": "/3569/2/preview.png" } ], "eprint_id": 3569, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6135" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6135" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6135" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/69", "datestamp": "2008-10-31", "lastmod": "2021-04-16 22:24:01", "status_changed": "2009-09-25 03:00:56", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rand-R-J", "name": { "family": "Rand", "given": "Richard J." }, "show_email": "NO" } ] }, "title": "The relationship between the density wave, molecular gas and star formation in M51", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\n\r\nA study is presented of the relationship between the density wave, molecular gas and star formation in the molecule-rich, grand-design spiral galaxy M51.\r\n\r\nAn interferometric map of CO emission covering most of the disk of M51 at 8\" resolution is presented. A narrow, two-arm spiral pattern is seen in the molecular gas. Streaming motions indicating the presence of a density wave can clearly be seen. Giant Molecular Associations (GMAs) of typical mass 3 x 10[superscript 7] M[...], first reported by Vogel, Kulkarni and Scoville, are seen in abundance along the arms. The virial theorem indicates that these GMAs are roughly gravitationally bound. A few unbound GMAs are also seen between the arms. There is evidence that these interarm GMAs form in a secondary compression of the density wave. Substructure in the GMAs is indicated by their CO spectra, which typically reveal a few discrete velocity components.\r\n\r\nHigher (2.5\") resolution maps of a small area south of the nucleus of M51 reveal patchy substructure along the southern molecular spiral arm and in the GMAs. The above-mentioned streaming motions are confirmed at this resolution. The one-dimensional velocity dispersion along the arms at this resolution is roughly 10 km s[superscript -1]. A more careful virial analysis confirms that the on-arm GMAs are bound while the interarm GMAs are unbound. The on-arm GMAs are shown to be stable against galactic tidal forces, while the interarm GMAs are close to the point of marginal stability. Along the spiral arm in this map, the detailed agreement between CO and H\u03b1 luminosity is poor. There are several possible explanations for this.\r\n\r\nTwo consequences of star formation on the state of the ISM of M51 are discussed. Using the new, 8\"-resolution VLA map of 21-cm emission, we find much new evidence in support of the idea of Tilanus and Allen that the HI is predominantly a product of dissociation in star-forming regions. The possibility is suggested that HI emission may be used as an indicator of star formation efficiency in molecule-rich galaxies.\r\n\r\nIRAS pointed observations of M51 are used to probe the origins of the infrared emission. Two independent tests indicate that a substantial fraction of the infrared emission originates in a cirrus component, and not due to dust heating by star-forming regions. One consequence of the existence of the cirrus component is that infrared emission cannot be used in a straightforward way to test the hypothesis of the triggering of star formation by a density wave.\r\n\r\nA kinematic study of the old-disk stars, and the molecular, neutral and ionized gas is presented. The old-disk stars, since they comprise most of the mass of the galaxy, trace the underlying gravitational perturbation. Long-slit spectroscopy of the absorption lines provides some evidence for radial streaming motions in the massive old-disk population. The amplitude of the motion at 85\" from the nucleus is greater than that expected from linear density wave theory. A possible explanation from nonlinear theory is given. Long-slit spectroscopy of the [...] and [NII] lines, along with kinematic information from our CO map and the high-resolution VLA map of 21-cm emission, clearly reveal streaming motions in the molecular, neutral and ionized gas. These motions are compared with the predictions of nonlinear density wave models.\r\n\r\nA quantitative analysis of possible GMA formation mechanisms, which draws on our morphological and kinematic observations of the molecular gas, is presented. Gravitational instability and collisional agglomeration are both viable mechanisms for GMA formation on the arms. The interarm gas is close to the point of marginal stability, and the postulated secondary compression of the density wave may be sufficient to cause either weak instabilities in the gas, or low-level orbit crowding, thereby explaining the unbound interarm GMAs. The relationship between GMA formation and the triggering of star formation is briefly addressed. Problems with the conclusion that the on-arm GMAs are gravitationally bound are discussed. Disruption of bound on-arm GMAs must be rapid since they are confined to narrow spiral arms. Although the arguments are by no means conclusive, the input power of star formation is a plausible mechanism for GMA disruption.\r\n", "date": "1991", "date_type": "degree", "id_number": "CaltechETD:etd-09162008-105121", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09162008-105121", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-31", "doi": "10.7907/c2j4-qh42", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-16", "thesis_defense_date": "1990-09-21", "thesis_approved_date": "2008-10-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1991", "author_list": "Rand, Richard J." }, { "id": "/id/eprint/5083", "eprint_id": 5083, "rev_number": 10, "documents": [ { "id": "/id/document/8057", "doc_id": 8057, "rev_number": 2, "files": [ { "id": "/id/file/49587", "fileid": 49587, "datasetid": "document", "objectid": 8057, "filename": "Stern_ja_1991.pdf", "mime_type": "application/pdf", "filesize": 6602495, "mtime": "2012-12-26 03:14:36", "url": "/5083/1/Stern_ja_1991.pdf" } ], "eprint_id": 5083, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Stern_ja_1991.pdf", "language": "en", "security": "public", "license": "other", "main": "Stern_ja_1991.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/24562" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/24562" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/24562" } ] } }, { "id": "/id/document/16534", "doc_id": 16534, "rev_number": 3, "files": [ { "id": "/id/file/204511", "fileid": 204511, "datasetid": "document", "objectid": 16534, "filename": "Stern_Jeffrey_1991.txt", "mime_type": "text/plain", "filesize": 2848, "mtime": "2016-08-22 21:17:45", "url": "/5083/2/Stern_Jeffrey_1991.txt" } ], "eprint_id": 5083, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Stern_Jeffrey_1991.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/24562", "doc_id": 24562, "rev_number": 2, "files": [ { "id": "/id/file/49585", "fileid": 49585, "datasetid": "document", "objectid": 24562, "filename": "preview.png", "mime_type": "image/png", "hash": "255f269471b7f46254bca39e0ba4d5fa", "hash_type": "MD5", "filesize": 8357, "mtime": "2012-12-26 03:14:36", "url": "/5083/3/preview.png" } ], "eprint_id": 5083, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/8057" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/8057" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/8057" } ] } }, { "id": "/id/document/124746", "doc_id": 124746, "rev_number": 1, "files": [ { "id": "/id/file/370176", "fileid": 370176, "datasetid": "document", "objectid": 124746, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "a3b17aaa0d86d9d987cf259e966fa371", "hash_type": "MD5", "filesize": 1315, "mtime": "2021-06-23 23:52:54", "url": "/5083/4/indexcodes.txt" } ], "eprint_id": 5083, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16534" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16534" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16534" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/50/83", "datestamp": "2004-12-20", "lastmod": "2020-03-10 23:01:20", "status_changed": "2009-09-25 03:32:45", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "Jeffrey.Stern@jpl.nasa.gov", "id": "Stern-J-A", "name": { "family": "Stern", "given": "Jeffrey Aaron" }, "show_email": "NO" } ] }, "title": "Fabrication and testing of NbN/MgO/NbN tunnel junctions for use as high-frequency heterodyne detectors", "ispublished": "unpub", "full_text_status": "public", "keywords": "Applied Physics", "abstract": "This thesis describes the development and testing of NbN/MgO/NbN tunnel junctions for use as superconductor-insulator-superconductor (SIS) mixers. SIS mixers are the most sensitive heterodyne detectors in the millimeter wavelength region. Most SIS mixers use Pb alloy tunnel junction. These tunnel junctions have several problems associated with the soft nature of Pb and its low superconducting transition temperature. NbN-based tunnel junctions are being developed to overcome these difficulties. These devices are intended to be used as mixers at millimeter and submillimeter wavelengths. This thesis describes the fabrication process involved in making NbN junctions, and the results of measurements on these devices. The purpose of these measurements is to determine the future possibilities of NbN tunnel junctions as high-frequency mixers.\r\n\r\nThe first chapter is an introduction to SIS mixers and explains how tunnel junction properties affect mixer performance. The basic theory of tunneling and mixing in SIS mixers is first presented. A description of quantum mixer theory is included in this presentation. This theory makes several interesting predictions that cannot be explained using classical theories. This is followed by a description of how real SIS tunnel junctions differ from ideal junctions. The physical origin of these differences is discussed, along with how they affect SIS mixer performance. Finally, the advantages and disadvantages of the various superconducting materials available are discussed. The decision to develop NbN devices is based on these material properties.\r\n\r\nThe second chapter describes the methods used to fabricate small-area NbN/MgO/NbN tunnel junctions. The chapter begins with a description of the various methods that have been used to deposit NbN films. Reactive magnetron sputtering is chosen as the best method for tunnel junction fabrication. Details on the vacuum systems and the methods used for depositing superconducting NbN are discussed. Next, the process used for depositing junction trilayers (NbN/MgO/NbN) is described. The probable growth mode of MgO on NbN is presented. The importance of this growth mode to the junction quality is explained in some detail. Next, standard junction processing steps are reported. The details and limitations of each step are put forth. The standard process allows for the fabrication of 1 [square micron] tunnel junctions. Finally, this chapter discusses several methods of fabaricating submicron junctions that are being pursued. The status of this work is given.\r\n\r\nThe third chapter describes the characterization of NbN films and NbN/Mg0/NbN tunnel junctions. Film properties are described first. The correlation of these properties to deposition conditions is discussed in some detail. Next, values for the various features of the I-V characteristic are given; typical and exceptional values are noted. How these features limit mixer results is described in detail. Several important device attributes were measured using superconducting-quantum-interference-devices (SQUIDs). These attributes are the junction's specific capacitance and the film's magnetic penetration depth. The theory and results of measuring specific capacitance and penetration depth are presented. Following the SQUID results is a large section on RP testing. Mixer tests were made at 205 GHz. The receiver design used, integral inductive tuning circuit used and results are discussed. These results are well understood, with the exception of the temperature dependence of the mixer performance. Finally, measurements of the uniformity of many junctions on a single wafer are presented. The importance of junction uniformity is also described.\r\n\r\nThe final chapter discusses the ultimate limits on NbN mixers, and tells what future work must be done to achieve these limits. The primary high-frequency limit on NbN junctions is the capacitance of NbN/MgO/NbN junctions. The limit imposed by the junction capacitance and circuits used to tune out this capacitance are discussed. Also, the low-frequency limits on NbN junctions are discussed. The status of submicron devices is presented. Junction area is the most immediate limitation on NbN mixer results. The possibility of using other barrier materials to increase the RC speed of NbN junctions is presented. Finally, the possibility of operating NbN junctions at temperatures above 4.2 K is discussed.", "date": "1991", "date_type": "degree", "id_number": "CaltechETD:etd-12202004-091326", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-12202004-091326", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-12-20", "doi": "10.7907/AZ4Q-DF35", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-12-20", "thesis_defense_date": "1990-08-01", "thesis_approved_date": "2004-12-20", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1991", "author_list": "Stern, Jeffrey Aaron" }, { "id": "/id/eprint/2743", "eprint_id": 2743, "rev_number": 10, "documents": [ { "id": "/id/document/5054", "doc_id": 5054, "rev_number": 3, "files": [ { "id": "/id/file/29464", "fileid": 29464, "datasetid": "document", "objectid": 5054, "filename": "Miller_mc_1990.pdf", "mime_type": "application/pdf", "filesize": 4570165, "mtime": "2012-12-26 02:54:01", "url": "/2743/1/Miller_mc_1990.pdf" } ], "eprint_id": 2743, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Miller_mc_1990.pdf", "language": "en", "security": "public", "license": "other", "main": "Miller_mc_1990.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21604" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21604" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21604" } ] } }, { "id": "/id/document/21604", "doc_id": 21604, "rev_number": 3, "files": [ { "id": "/id/file/29462", "fileid": 29462, "datasetid": "document", "objectid": 21604, "filename": "preview.png", "mime_type": "image/png", "hash": "3907bfa2f848dba904c5afa0ce96ad7f", "hash_type": "MD5", "filesize": 9022, "mtime": "2012-12-26 02:54:01", "url": "/2743/2/preview.png" } ], "eprint_id": 2743, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5054" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5054" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5054" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/27/43", "datestamp": "2007-07-19", "lastmod": "2021-04-16 23:22:38", "status_changed": "2009-09-25 02:44:02", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Miller-Michael-Coleman", "name": { "family": "Miller", "given": "Michael Coleman" }, "show_email": "NO" } ] }, "title": "Radiative transfer in very strong magnetic fields", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe study of the cooling of neutron stars has been undertaken by many researchers in the past twenty-five years, but this study has been made difficult by the inherent theoretical and observational uncertainties; most observations of their thermal X-ray flux have yielded only upper limits. More sensitive satellites such as ROSAT and AXAF may provide more positive flux information, and it is important to know how to interpret these data in terms of surface temperature. One of the most important factors in this interpretation is the effect of the surface magnetic field.\r\n\r\nYoung neutron stars are believed to have extremely strong magnetic fields, on the order of 10(12)G. These fields dominate the physics of the atmosphere. In particular, atoms in the atmospheres of neutron stars have much greater binding energies than in the zero-field case, and they are constrained to move along the field lines. We use a multiconfigurational Hartree-Fock code, modified for very strong magnetic fields, to calculate wavefunctions, energies and oscillator strengths for several atoms in representative values of the magnetic field.\r\n\r\nWe then use these simulations to construct model atmospheres for neutron stars. Because of the low mass necessary for optical depth unity in the soft X-rays (typically [...]) and because of the short time scale for gravitational separation (~ 1 - 100s), the photosphere is likely to consist of a pure element. Numerous processes could cause many elements to be important, so we investigate atmospheres consisting of pure hydrogen, helium, carbon, nitrogen and silicon in magnetic fields of 9.4 x 10(11)G, 2.35 x 10(12)G, and 4.7 x 10(12)G.\r\n\r\nWe also use the high-field energies to investigate soft X-ray lines in gamma-ray bursts. Highly ionized elements could create absorption lines in the 1-15keV range, and the identification of such lines in conjunction with cyclotron lines would determine the magnetic field and gravitational redshift on the surface of the star, which would provide clues to the equation of state on the interior. We conclude with a discussion of the prospect of identifying these lines with future satellites.", "date": "1990", "date_type": "degree", "id_number": "CaltechETD:etd-06272007-101041", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06272007-101041", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-07-19", "doi": "10.7907/9t01-q903", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-06-27", "thesis_defense_date": "1990-05-22", "thesis_approved_date": "2007-07-19", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1990", "author_list": "Miller, Michael Coleman" }, { "id": "/id/eprint/3444", "eprint_id": 3444, "rev_number": 15, "documents": [ { "id": "/id/document/5979", "doc_id": 5979, "rev_number": 4, "files": [ { "id": "/id/file/35629", "fileid": 35629, "datasetid": "document", "objectid": 5979, "filename": "Myers_st_1990.pdf", "mime_type": "application/pdf", "filesize": 8686628, "mtime": "2012-12-26 02:59:57", "url": "/3444/1/Myers_st_1990.pdf" } ], "eprint_id": 3444, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Myers_st_1990.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22519" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22519" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22519" } ] } }, { "id": "/id/document/22519", "doc_id": 22519, "rev_number": 3, "files": [ { "id": "/id/file/35627", "fileid": 35627, "datasetid": "document", "objectid": 22519, "filename": "preview.png", "mime_type": "image/png", "hash": "2ac23929037e35313daf840dd42e934f", "hash_type": "MD5", "filesize": 10016, "mtime": "2012-12-26 02:59:57", "url": "/3444/2/preview.png" } ], "eprint_id": 3444, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5979" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5979" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5979" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/44", "datestamp": "2008-09-15", "lastmod": "2023-01-19 00:13:41", "status_changed": "2009-09-25 02:58:30", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Myers-Steven-Theodore", "name": { "family": "Myers", "given": "Steven Theodore" }, "show_email": "NO" } ] }, "title": "A Search for Anisotropy in the Cosmic Microwave Background on Angular Scales of 1 to 30 Arcminutes", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Observations at a frequency of 20 GHz from the Owens Valley Radio Observatory with the 40-meter diameter radiotelescope are used to place limits on the anisotropy of the cosmic microwave background radiation, believed to be a relic from the Big Bang. Two experiments, designated NCP and RING, were performed with the former consisting of deep measurements in 8 fields at the declination \u03b4 = 89\u00b0 and the latter a survey of 96 fields at declination \u03b4 = 88\u00b0 10'42\". Bayesian statistical analysis of the 8 NCP field observations place a 95% confidence upper limit of \u03b4T/T < 1.9 x 10-5 (in fractions of the microwave background temperature 2.735 K) and 4.2 x 10-5 for 99.87% confidence (3\u03c3) on the amplitude of fluctuations with a characteristic correlation length of 2'.6. The 96 fields of the RING experiment were observed in an interlocked ring-like geometry to enhance the sensitivity of the experiment to larger-scale anisotropies. Because of the larger area of sky covered, this data was more susceptible to contamination by discrete extragalactic radio sources and separate lower frequency observations were used to identify and correct for the contributions of these objects. The statistical analysis of the RING data results in the limits on the anisotropy of 2.5 < \u03b4T/T < 5.0 x 10-5 (95%) and 1.9 < \u03b4T/T < 6.1 x 10-5 (99.87%) for fluctuations with a correlation angle of 2'.6. Because of the high probability of residual discrete source contamination, these results are treated as upper limits on intrinsic background fluctuations. These experiments constrain the amplitude to be less than 3 x 10-4 for correlation angles between 0'.1 and 30' (95%). The implications for cosmology and theories of galaxy formation are discussed, and models without significant non-baryonic matter and/or non-standard recombination are excluded by the observations.\r\n", "date": "1990", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-135630", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-135630", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-15", "doi": "10.7907/p4e7-rw11", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "chair" }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "orcid": "0000-0003-3820-1740", "role": "member" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1990-03-27", "thesis_approved_date": "2008-09-15", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1990", "author_list": "Myers, Steven Theodore" }, { "id": "/id/eprint/3555", "eprint_id": 3555, "rev_number": 10, "documents": [ { "id": "/id/document/6120", "doc_id": 6120, "rev_number": 3, "files": [ { "id": "/id/file/36570", "fileid": 36570, "datasetid": "document", "objectid": 6120, "filename": "Wilson_cd_1990.pdf", "mime_type": "application/pdf", "filesize": 34859746, "mtime": "2012-12-26 03:00:54", "url": "/3555/1/Wilson_cd_1990.pdf" } ], "eprint_id": 3555, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Wilson_cd_1990.pdf", "language": "en", "security": "public", "license": "other", "main": "Wilson_cd_1990.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22660" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22660" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22660" } ] } }, { "id": "/id/document/22660", "doc_id": 22660, "rev_number": 3, "files": [ { "id": "/id/file/36568", "fileid": 36568, "datasetid": "document", "objectid": 22660, "filename": "preview.png", "mime_type": "image/png", "hash": "b10d4905b2992e846b9bfedda2b77ceb", "hash_type": "MD5", "filesize": 7795, "mtime": "2012-12-26 03:00:54", "url": "/3555/2/preview.png" } ], "eprint_id": 3555, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6120" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6120" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6120" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/35/55", "datestamp": "2008-10-31", "lastmod": "2021-04-16 22:24:09", "status_changed": "2009-09-25 03:00:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wilson-C-D", "name": { "family": "Wilson", "given": "Christine Diana" }, "show_email": "NO" } ] }, "title": "Star formation and the interstellar medium in M33", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nNew millimeter-wave and optical data are used to study high-mass star formation and its relationship with the interstellar medium in the inner 4' radius of the nearby spiral galaxy M33. The total mass of molecular hydrogen in this region is 3.4x10[superscript 7] M[...], roughly twice the mass in atomic hydrogen. The predicted atomic hydrogen column density from atomic mantles of molecular clouds is similar to the observed mean atomic hydrogen column density. Thus probably only a small fraction of the atomic hydrogen is in a diffuse component not directly associated with molecular clouds.\r\n\r\nThe properties of 38 individual molecular clouds in M33 (velocity widths, diameters, peak brightness temperatures, and masses) are very similar to those of Galactic molecular clouds. Masses derived from the virial theorem and from the integrated CO fluxes agree to within 10%, which implies that the value of the conversion factor from CO flux to H[subscript 2] column density, \u03b1, is the same in M33 and the Galaxy. This is the first direct measurement of the value of \u03b1 in an external galaxy.\r\n\r\nThe mass distribution of clouds in M33 is consistent with that derived in the Galaxy for M = 0.8 - 4 x 10[superscript 5] M[...], but shows a total lack of clouds with masses greater than 4 x 10[superscript 5] M[...]. A simple model is proposed to explain the high-mass cutoff to the mass distribution as arising from the competing processes of cloud growth through accretion and cloud destruction due to star formation. Comparison of the flux detected with the interferometer with single dish data indicates that 50% of the molecular gas resides in structures less massive than 0.8 x10[superscript 5] M[...], in contrast to the Galaxy where only 15% of the molecular gas mass is in these smaller structures.\r\n\r\n41 OB associations each containing at least ten blue stars have been identified in this region of M33. The associations have mean radii of 40 pc, masses in stars of mass > 20 M[...] of 600 M[...], and ages of 8x10[superscript 6] yr. No evidence is found for a gradient in the ratio of blue to red supergiants in the inner two kiloparsecs of M33, despite a factor of two decrease in the metallicity over this range of radius. The blue luminosity function for stars in the field is deficient at bright magnitudes relative to the luminosity function for stars in associations. In addition, the associations in the northern arm contain no stars more massive than 20 M[...] while associations in the southern arm contain several stars with masses of 60 M[...]. These differences may be due to a sudden cessation of star formation resulting in a larger mean age for the stars or to a smaller upper mass cutoff to the initial mass function in the field and the northern arm.\r\n\r\nThe offset between the molecular and atomic gas peaks in the southern spiral arm is consistent with streaming motions expected as the gas enters a spiral density wave. In addition, the OB associations in the southern spiral arm show a weak age gradient perpendicular to the arm, consistent with the presence of a density wave. However, the northern arm has an age gradient running along the arm, as would be expected for a stochastic star formation arm.\r\n\r\nA comparison of the spatial distributions of the H\u03b1, CO, and HI emission peaks indicates that the atomic gas is probably formed via photo-dissociation of the molecular gas by recent high-mass star formation. Roughly two-thirds of the molecular clouds with M > 0.5 x 10[superscript 5] M[...] contain recent massive star formation with inferred high-mass star formation rates for individual clouds ranging from 5x10[superscript -6] to 5x10[superscript -4] M[...] yr[superscript -1]. The photo-dissociating flux produced by these stars is sufficient to produce the amount of atomic gas near the molecular clouds if the molecular clouds have a clumped structure.\r\n\r\nThe high-mass star formation rate and efficiency are measured by combining optical, far-infrared, and millimeter data. The high-mass star formation rate calculated from the H\u03b1 emission is 0.007 M[...] yr[superscript -1] over an area of 5 kpc[superscript 2], which corresponds to a total star formation rate of 0.04 M[...] yr[superscript -1]. The star formation rate obtained from the far-infrared emission agrees with the rate obtained from the H\u03b1 emission to within a factor of two. A lower limit to the high-mass star formation rate obtained from number counts of blue stars is consistent with the rates obtained from H\u03b1 and far-infrared emission. The southern spiral arm and the molecular complexes have similar star formation efficiencies to regions of the galaxy containing little molecular gas. Thus the large amount of star formation occurring in the spiral arms of M33 is due to the presence of large amounts of molecular gas and not to an increased star formation efficiency.\r\n", "date": "1990", "date_type": "degree", "id_number": "CaltechETD:etd-09152008-110204", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09152008-110204", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-31", "doi": "10.7907/sqk4-dx41", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-15", "thesis_defense_date": "1990-05-09", "thesis_approved_date": "2008-10-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1990", "author_list": "Wilson, Christine Diana" }, { "id": "/id/eprint/2640", "eprint_id": 2640, "rev_number": 13, "documents": [ { "id": "/id/document/4935", "doc_id": 4935, "rev_number": 4, "files": [ { "id": "/id/file/28623", "fileid": 28623, "datasetid": "document", "objectid": 4935, "filename": "Canzian_b_1990.pdf", "mime_type": "application/pdf", "filesize": 19798501, "mtime": "2012-12-26 02:53:16", "url": "/2640/1/Canzian_b_1990.pdf" } ], "eprint_id": 2640, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Canzian_b_1990.pdf", "language": "en", "security": "internal", "license": "other", "main": "Canzian_b_1990.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21485" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21485" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21485" } ] } }, { "id": "/id/document/21485", "doc_id": 21485, "rev_number": 3, "files": [ { "id": "/id/file/28621", "fileid": 28621, "datasetid": "document", "objectid": 21485, "filename": "preview.png", "mime_type": "image/png", "hash": "5f08810e79003a4aabd42c84c600c69e", "hash_type": "MD5", "filesize": 10248, "mtime": "2012-12-26 02:53:16", "url": "/2640/2/preview.png" } ], "eprint_id": 2640, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4935" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4935" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4935" } ] } }, { "id": "/id/document/135894", "doc_id": 135894, "rev_number": 2, "files": [ { "id": "/id/file/389057", "fileid": 389057, "datasetid": "document", "objectid": 135894, "filename": "canzian-bj_1990.pdf", "mime_type": "application/pdf", "hash": "88b211c3bdb86e5380996fa84d6c90bf", "hash_type": "MD5", "filesize": 14188619, "mtime": "2022-01-27 00:38:57", "url": "/2640/3/canzian-bj_1990.pdf" } ], "eprint_id": 2640, "pos": 3, "placement": 3, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "canzian-bj_1990.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/135895", "doc_id": 135895, "rev_number": 1, "files": [ { "id": "/id/file/389061", "fileid": 389061, "datasetid": "document", "objectid": 135895, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "36de315c83e1b8ff34242c4730feb501", "hash_type": "MD5", "filesize": 41699, "mtime": "2022-01-27 00:59:19", "url": "/2640/4/indexcodes.txt" } ], "eprint_id": 2640, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/135894" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/135894" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/135894" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/26/40", "datestamp": "2007-07-10", "lastmod": "2022-01-27 00:56:02", "status_changed": "2009-09-25 02:42:10", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Canzian-Blaise-J", "name": { "family": "Canzian", "given": "Blaise J." }, "show_email": "NO" } ] }, "title": "Molecular Gas and Star Formation in the Central Regions of Virgo Spiral Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "The central regions of eight normal spiral galaxies in the Virgo Cluster spanning a wide range of morphological types have been observed in CO (J = 1 \u2192 0) emission using the Owens Valley mm-wave interferometer. Broadband optical and H\u03b1 CCD photometry was obtained using the Palomar 60-inch telescope.
\r\n\r\nThe H\u2082 masses in the central five kiloparsecs of the spirals are large, typically several 10\u2078 solar masses, far exceeding the atomic hydrogen masses. H\u2082 densities in the cloud complexes are comparable to those of Galactic center complexes such as Sgr B2. Molecular gas comprises a substantial fraction of the dynamical mass of the central regions. The gas mass fraction, typically 5-15% at 2.5 kiloparsec radius, increases to 15-30% at the center. Molecular gas in the interferometer maps is concentrated in structures with scale lengths of only 400-750 parsecs. Such massive gas disks are, nonetheless, dynamically stable. The H\u2082 masses may be overestimated in some spirals because of cloud heating. The main source of heating is probably dissipation of turbulence, which is probably greater at the centers of spirals based on CO line widths.
\r\n\r\nCurrent central star formation rates are about a few solar masses per year. The star formation rate in the central regions of most of the spirals has been relatively constant over a Hubble time, although some galaxies are currently undergoing star formation bursts. Several mechanisms are suggested that could supply enough gas to maintain current star formation rates. The current rate of star formation is well correlated with the mean square molecular gas surface density computed from interferometer maps. Such a correlation is expected if cloud-cloud collisions or another stimulation mechanism acting between clouds is the principle means to produce high-mass stars where the concentration of clouds is greatest. The B luminosity is better correlated with the total gas mass surface density, which supports a stochastic or independent mode of forming intermediate-mass stars in the general cloud population.
", "date": "1990", "date_type": "degree", "id_number": "CaltechETD:etd-06182007-104442", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06182007-104442", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-07-10", "doi": "10.7907/pcga-sm96", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "chair" }, { "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "orcid": "0000-0001-5390-8563", "role": "member" }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "member" }, { "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "id": "Sargent-A-I", "name": { "family": "Sargent", "given": "Anneila Isabel" }, "orcid": "0000-0002-4633-5098", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-06-18", "thesis_defense_date": "1990-05-25", "thesis_approved_date": "2007-07-10", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1990", "author_list": "Canzian, Blaise J." }, { "id": "/id/eprint/2578", "eprint_id": 2578, "rev_number": 24, "documents": [ { "id": "/id/document/4855", "doc_id": 4855, "rev_number": 4, "files": [ { "id": "/id/file/28093", "fileid": 28093, "datasetid": "document", "objectid": 4855, "filename": "Budge_kg_1990.pdf", "mime_type": "application/pdf", "filesize": 15838101, "mtime": "2012-12-26 02:52:47", "url": "/2578/1/Budge_kg_1990.pdf" } ], "eprint_id": 2578, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Budge_kg_1990.pdf", "language": "en", "security": "internal", "license": "other", "main": "Budge_kg_1990.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/135888" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/25/78", "datestamp": "2007-07-06", "lastmod": "2022-01-26 20:57:56", "status_changed": "2009-09-25 02:40:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kgbudge@lanl.gov", "id": "Budge-Kent-Grimmett", "name": { "family": "Budge", "given": "Kent Grimmett" }, "show_email": "YES" } ] }, "title": "A Non-LTE Analysis of a Sample of O Stars Selected from Galactic OB Associations", "ispublished": "unpub", "full_text_status": "public", "keywords": "spectroscopy, stellar atmospheres, stellar atmosphere models", "abstract": "The tables of non-LTE line profiles and equivalent widths published by Mihalas and his collaborators [33], [7], [35] have been revised and extended to four different values of the abundance ratio He/H. Bolometric corrections have been calculated for V magnitudes. The theoretical line profiles have been fit to echelle spectrograms of 22 galactic O stars by \u03c7\u00b2 minimization. It is found that the stars with the lowest surface gravities are fitted best by theoretical spectra with unexpectedly high helium abundances (He/H ~ 0.50), while the stars with higher surface gravities are fitted best by theoretical spectra with He/H ~ 0.10, the accepted cosmic ratio. This suggests a systematic failure of conventional non-LTE, plane-parallel models for the more luminous O stars, probably as a result of the neglect of geometrical dilution.
\r\n\r\nThe formula, log He/H = 1.1234-0.4791 log g, gives a good fit to the relation between the apparent helium abundance and log g. Using this relationship, the apparent abundances have been reduced to what are probably true abundances relative to the normal cosmic abundance. It is found that there is no significant difference in the average helium abundances of the associations observed. However, the stars HD 12993, HD 242908, and HD 193595 may be blue stragglers with moderately enhanced helium abundance (He/H ~ 0.19).
\r\n\r\nRelative carbon abundances have been determined empirically by comparison of the CIV 5812\u00c5 and HeII 4542\u00c5 equivalent widths. It is found that the association Cyg 0B2 is overabundant in carbon by ~50%. Likewise, the blue straggler HD 236894 is underabundant in carbon by a factor of two.
\r\n\r\nThe estimated effective temperatures of the sample are compared to the previously accepted calibration of MK spectral types to the effective temperature. Estimates of the radii and masses of the stars in the sample have been calculated from their physical parameters and their absolute visual magnitudes.
", "date": "1990", "date_type": "degree", "id_number": "CaltechETD:etd-06132007-132124", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06132007-132124", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship" }, { "agency": "San Diego Supercomputer Center" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-07-06", "doi": "10.7907/A24K-G089", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "advisor" }, { "id": "Boesgaard-A-M", "name": { "family": "Boesgaard", "given": "Ann Merchant" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "orcid": "0000-0002-8744-3298", "role": "chair" }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "member" }, { "email": "jlc@astro.caltech.edu", "id": "Cohen-J-G", "name": { "family": "Cohen", "given": "Judith G." }, "orcid": "0000-0002-8039-4673", "role": "member" }, { "id": "Boesgaard-A-M", "name": { "family": "Boesgaard", "given": "Ann Merchant" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-06-13", "thesis_defense_date": "1990-02-16", "thesis_approved_date": "2007-07-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1990", "author_list": "Budge, Kent Grimmett" }, { "id": "/id/eprint/2134", "eprint_id": 2134, "rev_number": 10, "documents": [ { "id": "/id/document/3882", "doc_id": 3882, "rev_number": 2, "files": [ { "id": "/id/file/22721", "fileid": 22721, "datasetid": "document", "objectid": 3882, "filename": "Steidel_cc_1990.pdf", "mime_type": "application/pdf", "filesize": 14517477, "mtime": "2012-12-26 02:47:22", "url": "/2134/1/Steidel_cc_1990.pdf" } ], "eprint_id": 2134, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Steidel_cc_1990.pdf", "language": "en", "security": "public", "license": "other", "main": "Steidel_cc_1990.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20530" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20530" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20530" } ] } }, { "id": "/id/document/16529", "doc_id": 16529, "rev_number": 3, "files": [ { "id": "/id/file/202589", "fileid": 202589, "datasetid": "document", "objectid": 16529, "filename": "Steidel_Charles_1990.txt", "mime_type": "text/plain", "filesize": 524, "mtime": "2016-08-22 21:15:35", "url": "/2134/2/Steidel_Charles_1990.txt" } ], "eprint_id": 2134, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Steidel_Charles_1990.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/20530", "doc_id": 20530, "rev_number": 2, "files": [ { "id": "/id/file/22719", "fileid": 22719, "datasetid": "document", "objectid": 20530, "filename": "preview.png", "mime_type": "image/png", "hash": "3be451b2e8b3a3856a4c4fa7858811e9", "hash_type": "MD5", "filesize": 10547, "mtime": "2012-12-26 02:47:22", "url": "/2134/3/preview.png" } ], "eprint_id": 2134, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3882" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3882" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3882" } ] } }, { "id": "/id/document/122159", "doc_id": 122159, "rev_number": 1, "files": [ { "id": "/id/file/367553", "fileid": 367553, "datasetid": "document", "objectid": 122159, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "d13c844a2dc06e41d2e7ff1864c87845", "hash_type": "MD5", "filesize": 298, "mtime": "2021-06-23 21:49:09", "url": "/2134/4/indexcodes.txt" } ], "eprint_id": 2134, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16529" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16529" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16529" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/21/34", "datestamp": "2004-05-27", "lastmod": "2019-12-21 04:21:15", "status_changed": "2009-09-25 02:27:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steidel-Charles-Colville", "name": { "family": "Steidel", "given": "Charles Colville" }, "orcid": "0000-0002-4834-7260", "show_email": "NO" } ] }, "title": "Spectroscopic Observations of High Redshift QSOs: Galaxies and the Intergalactic Medium at Early Epochs", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe thesis consists primarily of 4 parts, which are separate but related insofar as each makes use of spectra of high redshift QSOs in order to investigate the properties of intervening gaseous material. Briefly summarized, the sections are as follows:
\r\n\r\nI. Wide-slit spectrophotometry of a sample of very high redshift QSOs is used to establish that the cumulative effect of the Lyman [alpha] forest of absorption lines is statistically the same in all of the QSOs. By combining these results with high resolution observations of QSO Lyman [alpha] forests, a new upper limit on the density of generally distributed intergalactic neutral hydrogen (the Gunn-Peterson limit) is obtained. Implications for the nature of the intergalactic medium and the baryonic mass density of the universe are discussed.
\r\n\r\nII. Observations of a number of high redshift QSOs close to each other on the plane of the sky are presented; based on the occurrence of heavy element absorption systems over a narrow range of redshifts in each of the spectra, evidence for the presence of a huge, elongated supercluster of galaxies at z = 2 is discussed.
\r\n\r\nIII. Results of a survey for heavy element absorption systems at the largest observable redshift (2.7 < z < 3.8) are presented; the data are combined with the very large survey for C IV absorption recently completed by Sargent, Boksenberg, and Steidel (1988). The data show very clear evolution of the heavy element absorbers with time over the redshift range 1.5 < z < 3.5. The changes are interpreted as a gradual evolution of the heavy element abundances in gas associated with sites where galaxies have formed. The implications for galaxy formation and evolution are discussed.
\r\n\r\nIV. Moderate dispersion spectra of a sample of Lyman limit absorption systems at z \u2248 3 have been obtained in order to determine the heavy element abundances and other physical parameters of the gas clouds responsible for the high redshift, heavy-element absorption systems in the spectra of QSOs. Photoionization models are used to conclude that the clouds are ionized primarily by the metagalactic UV flux, which has a spectral energy distribution comparable to that of AGNs. The abundances of C, 0, and Si are in general between 0.001 and 0.01 of the solar abundances, comparable to the most metal-poor stars in the halo of the Galaxy. The clouds have sizes in the range 1- 15 kpc and masses in the range 106 - 109 M\u2609. The clouds are discussed within the context of the hypothesis that the heavy element absorption systems are associated with the extended halos of high redshift galaxies. Diffuse gas in the form of such clouds may account for a significant fraction of the baryonic material in the universe, and it has probably played an important role in the evolution of galaxies over time.
\r\n", "date": "1990", "date_type": "degree", "id_number": "CaltechETD:etd-05272004-134241", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05272004-134241", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-05-27", "doi": "10.7907/MK1V-9803", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-05-27", "thesis_defense_date": "1989-08-22", "thesis_approved_date": "2004-05-27", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1990", "author_list": "Steidel, Charles Colville" }, { "id": "/id/eprint/8780", "eprint_id": 8780, "rev_number": 18, "documents": [ { "id": "/id/document/54606", "doc_id": 54606, "rev_number": 3, "files": [ { "id": "/id/file/156703", "fileid": 156703, "datasetid": "document", "objectid": 54606, "filename": "ZHANG_XH_1990.pdf", "mime_type": "application/pdf", "hash": "d72d2e57c70ca5ec5e7d90caf0d0d698", "hash_type": "MD5", "filesize": 41593213, "mtime": "2015-03-17 23:23:39", "url": "/8780/1/ZHANG_XH_1990.pdf" } ], "eprint_id": 8780, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "ZHANG_XH_1990.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 1660, "dir": "disk0/00/00/87/80", "datestamp": "2015-03-18 14:38:26", "lastmod": "2022-11-09 19:20:05", "status_changed": "2015-03-18 14:38:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zhang-Xiao-He", "name": { "family": "Zhang", "given": "Xiao-He" }, "show_email": "NO" } ] }, "title": "Multipole moments in general relativity and dynamical perturbations of black-hole magnetospheres", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis consists of two parts. In Part I, we develop a multipole moment formalism in general relativity and use it to analyze the motion and precession of compact bodies. More specifically, the generic, vacuum, dynamical gravitational field of the exterior universe in the vicinity of a freely moving body is expanded in positive powers of the distance r away from the body's spatial origin (i.e., in the distance r from its timelike-geodesic world line). The expansion coefficients, called \"external multipole moments,'' are defined covariantly in terms of the Riemann curvature tensor and its spatial derivatives evaluated on the body's central world line. In a carefully chosen class of de Donder coordinates, the expansion of the external field involves only integral powers of r ; no logarithmic terms occur. The expansion is used to derive higher-order corrections to previously known laws of motion and precession for black holes and other bodies. The resulting laws of motion and precession are expressed in terms of couplings of the time derivatives of the body's quadrupole and octopole moments to the external moments, i.e., to the external curvature and its gradient.
\r\n\r\nIn part II, we study the interaction of magnetohydrodynamic (MHD) waves in a black-hole magnetosphere with the \"dragging of inertial frames\" effect of the hole's rotation - i.e., with the hole's \"gravitomagnetic field.\" More specifically: we first rewrite the laws of perfect general relativistic magnetohydrodynamics (GRMHD) in 3+1 language in a general spacetime, in terms of quantities (magnetic field, flow velocity, ...) that would be measured by the ''fiducial observers\u201d whose world lines are orthogonal to (arbitrarily chosen) hypersurfaces of constant time. We then specialize to a stationary spacetime and MHD flow with one arbitrary spatial symmetry (e.g., the stationary magnetosphere of a Kerr black hole); and for this spacetime we reduce the GRMHD equations to a set of algebraic equations. The general features of the resulting stationary, symmetric GRMHD magnetospheric solutions are discussed, including the Blandford-Znajek effect in which the gravitomagnetic field interacts with the magnetosphere to produce an outflowing jet. Then in a specific model spacetime with two spatial symmetries, which captures the key features of the Kerr geometry, we derive the GRMHD equations which govern weak, linealized perturbations of a stationary magnetosphere with outflowing jet. These perturbation equations are then Fourier analyzed in time t and in the symmetry coordinate x, and subsequently solved numerically. The numerical solutions describe the interaction of MHD waves with the gravitomagnetic field. It is found that, among other features, when an oscillatory external force is applied to the region of the magnetosphere where plasma (e+e-) is being created, the magnetosphere responds especially strongly at a particular, resonant, driving frequency. The resonant frequency is that for which the perturbations appear to be stationary (time independent) in the common\r\nrest frame of the freshly created plasma and the rotating magnetic field lines. The\r\nmagnetosphere of a rotating black hole, when buffeted by nonaxisymmetric magnetic fields anchored in a surrounding accretion disk, might exhibit an analogous resonance. If so then the hole's outflowing jet might be modulated at resonant frequencies \u03c9=(m/2) \u03a9H where m is an integer and \u03a9H is the hole's angular velocity.
\r\n", "date": "1990", "date_type": "degree", "id_number": "CaltechTHESIS:03172015-154851912", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03172015-154851912", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Bianca Rios", "deposited_on": "2015-03-18 14:38:26", "doi": "10.7907/ra46-aj38", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1989-06-13", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1990", "author_list": "Zhang, Xiao-He" }, { "id": "/id/eprint/8009", "eprint_id": 8009, "rev_number": 26, "documents": [ { "id": "/id/document/43694", "doc_id": 43694, "rev_number": 3, "files": [ { "id": "/id/file/130046", "fileid": 130046, "datasetid": "document", "objectid": 43694, "filename": "Yurtsever_1989.pdf", "mime_type": "application/pdf", "hash": "779f0b1e6e1f13acd8fbdd26aae8882b", "hash_type": "MD5", "filesize": 60435056, "mtime": "2013-10-24 22:32:57", "url": "/8009/1/Yurtsever_1989.pdf" } ], "eprint_id": 8009, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Yurtsever_1989.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"archival" } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/80/09", "datestamp": "2013-10-24 23:02:59", "lastmod": "2022-01-11 23:44:11", "status_changed": "2013-10-24 23:02:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yurtsever-Ulvi-Hamit", "name": { "family": "Yurtsever", "given": "Ulvi Hamit" }, "show_email": "NO" } ] }, "title": "Singularities and Horizons in the Collisions of Gravitational Waves", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis presents a study of the dynamical, nonlinear interaction of colliding gravitational waves, as described by classical general relativity. It is focused mainly on two fundamental questions: First, what is the general structure of the singularities and Killing-Cauchy horizons produced in the collisions of exactly plane-symmetric gravitational waves? Second, under what conditions will the collisions of almost-plane gravitational waves (waves with large but finite transverse sizes) produce singularities?
\r\n\r\nIn the work on the collisions of exactly-plane waves, it is shown that Killing horizons in any plane-symmetric spacetime are unstable against small plane-symmetric perturbations. It is thus concluded that the Killing-Cauchy horizons produced by the collisions of some exactly plane gravitational waves are nongeneric, and that generic initial data for the colliding plane waves always produce \"pure\" spacetime singularities without such horizons. This conclusion is later proved rigorously (using the full nonlinear theory rather than perturbation theory), in connection with an analysis of the asymptotic singularity structure of a general colliding plane-wave spacetime. This analysis also proves that asymptotically the singularities created by colliding plane waves are of inhomogeneous-Kasner type; the asymptotic Kasner axes and exponents of these singularities in general depend on the spatial coordinate that runs tangentially to the singularity in the non-plane-symmetric direction.
\r\n\r\nIn the work on collisions of almost-plane gravitational waves, first some general properties of single almost-plane gravitational-wave spacetimes are explored. It is shown that, by contrast with an exact plane wave, an almost-plane gravitational wave cannot have a propagation direction that is Killing; i.e., it must diffract and disperse as it propagates. It is also shown that an almost-plane wave cannot be precisely sandwiched between two null wavefronts; i.e., it must leave behind tails in the spacetime region through which it passes. Next, the occurrence of spacetime singularities in the collisions of almost-plane waves is investigated. It is proved that if two colliding, almost-plane gravitational waves are initially exactly plane-symmetric across a central region of sufficiently large but finite transverse dimensions, then their collision produces a spacetime singularity with the same local structure as in the exact-plane-wave collision. Finally, it is shown that a singularity still forms when the central regions are only approximately plane-symmetric initially. Stated more precisely, it is proved that if the colliding almost-plane waves are initially sufficiently close to being exactly plane-symmetric across a bounded central region of sufficiently large transverse dimensions, then their collision necessarily produces spacetime singularities. In this case, nothing is now known about the local and global structures of the singularities.
", "date": "1989", "date_type": "degree", "id_number": "CaltechTHESIS:10242013-145903390", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10242013-145903390", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.36.1662" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.37.2803" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.37.2790" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.38.1706" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.38.1731" }, { "description": "Article adapted for Chapter 7.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.40.329" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_on": "2013-10-24 23:02:59", "doi": "10.7907/zm5n-g882", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" }, { "email": "preskill@caltech.edu", "id": "Preskill-J-P", "name": { "family": "Preskill", "given": "John P." }, "orcid": "0000-0002-2421-4762", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1988-09-29", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"2013-10-25 22:15:11", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "zucker_m@ligo.mit.edu", "id": "Zucker-Michael-Edward", "name": { "family": "Zucker", "given": "Michael Edward" }, "show_email": "NO" } ] }, "title": "Experiments with a Laser Interferometric Gravitational Wave Antenna", "ispublished": "unpub", "full_text_status": "public", "keywords": "LIGO, laser, interferometer, gravitational, gravity", "abstract": "Sources and effects of astrophysical gravitational radiation are explained briefly to motivate discussion of the Caltech 40 meter antenna, which employs laser interferometry to monitor proper distances between inertial test masses. Practical considerations in construction of the apparatus are described. Redesign of test mass systems has resulted in a reduction of noise from internal mass vibrations by up to two orders of magnitude at some frequencies. A laser frequency stabilization system was developed which corrects the frequency of an argon ion laser to a residual fluctuation level bounded by the spectral density \u221as\u03bd(f) \u2264 60 \u00b5Hz/\u221aHz, at fluctuation frequencies near 1.2 kHz. These and other improvements have contributed to reducing the spectral density of equivalent gravitational wave strain noise to \u221aSh(f) \u2248 10\u207b\u00b9\u2079/\u221a Hz at these frequencies.
\r\n\r\nFinally, observations made with the antenna in February and March of 1987 are described. Kilohertz-band gravitational waves produced by the remnant of the recent supernova are shown to be theoretically unlikely at the strength required for confident detection in this antenna (then operating at poorer sensitivity than that quoted above). A search for periodic waves in the recorded data, comprising Fourier analysis of four 105-second samples of the antenna strain signal, was used to place new upper limits on periodic gravitational radiation at frequencies between 305 Hz and 5 kHz. In particular, continuous waves of any polarization are ruled out above strain amplitudes of 1.2 x 10\u207b\u00b9\u2078 R.M.S. for waves emanating from the direction of the supernova, and 6.2 x 10\u207b\u00b9\u2079 R.M.S. for waves emanating from the galactic center, between 1.5 and 4 kilohertz. Between 305 Hz and 5kHz no strains greater than 1.2 x 10\u207b\u00b9\u2077 R.M.S. were detected from either direction. Limitations of the analysis and potential improvements are discussed, as are prospects for future searches.
", "date": "1989", "date_type": "degree", "id_number": "CaltechTHESIS:10252013-143448203", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10252013-143448203", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department", "LIGO" ] }, "deposited_by": "Dan Anguka", "deposited_on": "2013-10-25 22:15:11", "doi": "10.7907/T5D0-4N31", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "Ronald W. P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "Ronald W. P." }, "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "orcid": "0000-0002-9656-4032", "role": "member" }, { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "role": "member" }, { "id": "Gomez-R", "name": { "family": "Gomez", "given": "Ricardo" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1988-07-01", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1989", "author_list": "Zucker, Michael Edward" }, { "id": "/id/eprint/3433", "eprint_id": 3433, "rev_number": 31, "documents": [ { "id": "/id/document/76375", "doc_id": 76375, "rev_number": 3, "files": [ { "id": "/id/file/216301", "fileid": 216301, "datasetid": "document", "objectid": 76375, "filename": "Barsony 02232017 Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "43ae433b834333b71c2ed94f64d19c73", "hash_type": "MD5", "filesize": 852, "mtime": "2017-02-23 21:28:41", "url": "/3433/3/Barsony 02232017 Thesis Permission Form.txt" } ], "eprint_id": 3433, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Barsony 02232017 Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", 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"archive", "userid": 2, "dir": "disk0/00/00/34/33", "datestamp": "2008-09-18", "lastmod": "2020-04-30 00:51:44", "status_changed": "2009-09-25 02:58:21", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mbarsony@seti.org", "id": "Barsony-Mary-Anne", "name": { "family": "Barsony", "given": "Mary Anne" }, "show_email": "YES" } ] }, "title": "Outflows in High Mass Star-Forming Regions", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "In the last decade, observations of star-forming regions in the millimeter wavelength range have led to the discovery of supersonic molecular outflows from embedded infrared sources, a heretofore unsuspected, but now generally accepted, phase in the star formation process. In order to better understand the outflow phenomenon in high mass (i.e., high luminosity) pre-main sequence stars, the three sources S87, LkH\u03b1101, and S106 were chosen for closer study. Observations from the recently completed Owens Valley Radio Observatory's millimeter wave interferometer afford us the highest spatial-resolution, molecular line (CS J=2\u21921 and 13CO J=1\u21920) maps of these sources to date. The OVRO maps were combined with data from the 14 m FCRAO millimeter wave radio telescope, the VLA, IRAS, and the Palomar 5 m and 1.5 m optical telescopes.
\r\n\r\nA synthesis of the data reveals that although all three pre-main sequence objects are the sources of powerful, ionized stellar winds, only one, S87/IRS1, currently drives a bipolar molecular outflow. The inferred mass loss rates in the winds of S87/IRS1, LkH\u03b1101, and S106 IR are 1.8 x 10-5, 1.7 x 10-6, 1.1 x 10-5 M\u2609 yr-1, with corresponding wind velocities of 160, 350, and 200 km s-1. In all cases the wind velocities are lower, and the mass loss rates higher, than for main sequence stars of the same spectral types. Radiation pressure is inadequate to drive these winds, which can be anisotropic in their velocity fields.
\r\n\r\nThe existence of massive, large-scale (r \u2248 1016 cm) disks, necessary for numerous proposed molecular outflow models, can now be ruled out. Only one of the many proposed molecular outflow models is consistent with the new observations (K\u00f6nigl 1982).
\r\n\r\nAlthough the observed winds can disperse a good portion of the cloud cores they inhabit, they cannot completely destroy these cores. Consequently, outflows from pre-main sequence stars alone cannot account for the dispersal of molecular clouds, as some investigators have suggested.
\r\n\r\nTwo glaring and intriguing problems remain to be solved in this field: the origin of the supersonic turbulence observed throughout a molecular cloud, and the driving mechanism of the powerful, ionized winds found in the high-mass, pre-main sequence stars.
\r\n", "date": "1989", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-084535", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-084535", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-18", "doi": "10.7907/FDFC-0Q12", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "chair" }, { "email": "gab@gps.caltech.edu", "id": "Blake-G-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1988-09-23", "thesis_approved_date": "2008-09-18", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1989", "author_list": "Barsony, Mary Anne" }, { "id": "/id/eprint/2308", "eprint_id": 2308, "rev_number": 16, "documents": [ { "id": "/id/document/4359", "doc_id": 4359, "rev_number": 5, "files": [ { "id": "/id/file/25187", "fileid": 25187, "datasetid": "document", "objectid": 4359, "filename": "Dowling_te_1989.pdf", "mime_type": "application/pdf", "filesize": 7524601, "mtime": "2012-12-26 02:49:55", "url": "/2308/1/Dowling_te_1989.pdf" } ], "eprint_id": 2308, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Dowling_te_1989.pdf", "language": "en", "security": "internal", "license": "other", "main": "Dowling_te_1989.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20945" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20945" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20945" } ] } }, { "id": "/id/document/20945", "doc_id": 20945, "rev_number": 3, "files": [ { "id": "/id/file/25185", "fileid": 25185, "datasetid": "document", "objectid": 20945, "filename": "preview.png", "mime_type": "image/png", "hash": "757a38dde47bea56652010a24b533e44", "hash_type": "MD5", "filesize": 7169, "mtime": "2012-12-26 02:49:55", "url": "/2308/2/preview.png" } ], "eprint_id": 2308, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4359" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4359" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4359" } ] } }, { "id": "/id/document/134537", "doc_id": 134537, "rev_number": 2, "files": [ { "id": "/id/file/380658", "fileid": 380658, "datasetid": "document", "objectid": 134537, "filename": "dowling_te_1989.pdf", "mime_type": "application/pdf", "hash": "a3e038f7eba5c431f0a11c242356ec55", "hash_type": "MD5", "filesize": 4492248, "mtime": "2021-07-14 16:47:07", "url": "/2308/3/dowling_te_1989.pdf" } ], "eprint_id": 2308, "pos": 3, "placement": 3, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "dowling_te_1989.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/134538", "doc_id": 134538, "rev_number": 1, "files": [ { "id": "/id/file/380664", "fileid": 380664, "datasetid": "document", "objectid": 134538, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "ebfd1e33327c6cc4c3240ef080e1da83", "hash_type": "MD5", "filesize": 18627, "mtime": "2021-07-14 17:47:22", "url": "/2308/4/indexcodes.txt" } ], "eprint_id": 2308, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/134537" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/134537" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/134537" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/23/08", "datestamp": "2007-05-31", "lastmod": "2021-07-14 17:41:49", "status_changed": "2009-09-25 02:34:03", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dowling-Timothy-Edward", "name": { "family": "Dowling", "given": "Timothy Edward" }, "show_email": "NO" } ] }, "title": "A Dynamical Study of Jupiter's Great Red Spot", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science", "abstract": "This work is presented in the form of two related papers. In the first paper we investigate layer thickness variations in Jupiter's atmosphere by tracking absolute vorticity (\u03b6 + f) along streamlines of the Great Red Spot (GRS) and White Oval BC. The ratio of absolute vorticity to layer thickness, called the potential vorticity, is conserved following the motion. By observing Lagrangian variations of absolute vorticity, we may infer variations in layer thickness. The data thus obtained are a useful diagnostic that will help differentiate between models of Jovian vortices. We interpret the observed layer thickness variations using a simple \"1-1/2\" layer model in which a thin upper weather layer, which contains the vortices, overlies a much deeper layer, which is meant to model the deep atmosphere. In this model, layer thickness variations are directly coupled to motions in the deep atmosphere, and we use the data to infer the deep motions. In the first paper we interpret the data, using the quasi-geostrophic equations. In the second paper we reinterpret the data, using the more general shallow water equations. Most current models of the GRS are cast in terms of the 1-1/2 layer model, and they start by prescribing the motions in the deep atmosphere. Here we are able to derive the deep motions using the same 1-1/2 layer model assumptions, up to a constant that depends on the unknown static stability of Jupiter's troposphere. None of the current prescriptions for the deep motions are in qualitative agreement with the observations over the full range of latitudes observed. We study the 1-1/2 layer model numerically, using both the derived deep motions and the prescribed deep motions of current models. Only the present model, based on observations, yields Lagrangian absolute vorticity profiles that agree with those obtained in the first paper. A model run that starts with the observed zonally averaged cloud-top winds and derived deep motions shows instability, which naturally leads to the genesis and maintenance of a large, isolated vortex similar to the GRS.
", "date": "1989", "date_type": "degree", "id_number": "CaltechETD:etd-05302007-084208", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05302007-084208", "related_url": { "items": [ { "description": "Article adapted for Paper 1.", "type": "doi", "url": "https://doi.org/10.1175/1520-0469(1988)045%3C1380:pvaltv%3E2.0.co;2" }, { "description": "Article adapted for Paper 2.", "url": "https://doi.org/10.1175/1520-0469(1989)046%3C3256:jgrsaa%3E2.0.co;2" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-31", "doi": "10.7907/whc3-mh91", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "advisor" }, { "email": "dmuhlema@caltech.edu", "id": "Muhleman-D-O", "name": { "family": "Muhleman", "given": "Duane Owen" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "dmuhlema@caltech.edu", "id": "Muhleman-D-O", "name": { "family": "Muhleman", "given": "Duane Owen" }, "role": "chair" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "orcid": "0000-0002-2035-9198", "role": "member" }, { "email": "leonard@caltech.edu", "id": "Leonard-A", "name": { "family": "Leonard", "given": "Anthony" }, "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "id": "Zurek-Richard-W", "name": { "family": "Zurek", "given": "Richard W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-30", "thesis_defense_date": "1988-11-10", "thesis_approved_date": "2007-05-31", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. 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From detailed comparisons of their photospheric absorption line profiles observed at high signal-to-noise with the NLTE model atmosphere line profiles of Kudritzki, et al., in Munich, West Germany, the photospheric effective temperatures (Teff), surface gravities (g), and helium abundances (y) were derived. Placement of the CSPN in the distance-independent log(g) - log(Teff) diagram allowed central star masses and evolutionary ages to be deduced via comparisons with published evolutionary model calculations. Spectroscopic distances to the CSPN were estimated from the best fit model fluxes, leading to dynamical expansion ages for the surrounding nebulae which were typically much greater than the corresponding CSPN evolutionary ages. Two possible reasons for this timescale disagreement were quantitatively investigated: (1) the nebulae could have experienced a phase of rapid photo-ionization of material ejected while the stars were still on the AGB, or (2) the AGB - CSPN evolutionary transition times could have been increased by small additional amounts of residual envelope material remaining after the superwind mass loss phase.
\r\n\r\nAn important preliminary phase of this project was the design and construction of a CCD echelle spectrograph for the Palomar 1.5 m telescope. The spectrograph was designed to cover the wavelength range 3200 \u00c5 to 7000 \u00c5, utilizing 57 diffracted orders from the echelle grating. Fused quartz prism cross-dispersing elements and an all-transmitting camera lens system contribute to the extremely high throughput of the instrument; the combined telescope and echelle spectrograph efficiency is approximately 20% from above the atmosphere. Details of the echelle spectrograph optical and mechanical designs are presented.
\r\n\r\nThe scientific objectives of the CSPN study with this new instrument required a thorough investigation into the data reduction process for CCD echelle spectra, and a set of Fortran subroutines were written for this purpose as part of the FIGARO data reduction package. The philosophy and algorithms employed in these routines are discussed, and a detailed description of each of the commands is provided in an Appendix for future reference.
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Beverly" }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "id": "Shectman-S-A", "name": { "family": "Shectman", "given": "Stephen Alan" }, "orcid": "0000-0002-8681-6136", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "1988-05-17", "thesis_approved_date": "2008-11-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. 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"eprint_status": "archive", "userid": 87, "dir": "disk0/00/00/74/24", "datestamp": "2013-01-22 23:37:33", "lastmod": "2021-04-16 23:01:34", "status_changed": "2013-01-22 23:37:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Grossman-Erich-Nathan", "name": { "family": "Grossman", "given": "Erich Nathan" }, "show_email": "NO" } ] }, "title": "A Far-Infrared Heterodyne Spectrometer for Airborne Astronomy", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "note": "Thesis file (PDF) missing pp. 94.", "abstract": "The design and construction of a novel heterodyne spectrometer for airborne astronomy in the 50 \u00b5m - 200 \u00b5m wavelength range is described. along with laboratory measurements of its performance. A bulk, extrinsic Ge:Ga photoconductor is used as the mixer. Its low bandwidth, determined by the hole recombination rate, necessitates the use of a continuously tunable local oscillator. This is provided by a far-infrared laser sideband generator, which is based on a GaAs Schottky diode mounted at the feed of a comer-cube antenna, the latter combination acting as a reflective FIR modulator.
\r\n\r\nThe first chapter of this thesis describes the astronomical and technical context of the project - in particular, the constraints which the astronomical goals set on the instrument, and the advantages and drawbacks of each of the various broad instrumental strategies that are available for spectrometer design. The chapter's last section provides a very brief overview of our most successful laboratory results, which are described at greater length in chapters 2- 4. In chapter two we describe the performance of Ge:Ga mixers as heterodyne mixers. We report on an extensive series of measurements of bandwidth, photoconductive gain, and direct detection responsivity for a series of highly compensated, NTD detectors grown specifically for this purpose. Chapter two also describes a nunber of experiments on FIR heterodyne performance, made using the direct, attenuated laser, rather than the output of the sideband generator, as the local oscillator. These confirm the expectation that germanium photoconductors are capable of quantum-limited noise performance with quantum efficiencies of ~10%, at much lower LO powers than required for Schottky diodes. Our best achieved noise temperature is TN(DSB) = 655K at PLO = 1.6\u00b5W, a factor of > 25 lower than the best reported corresponding figure for Schottky diodes.
\r\n\r\nChapter 3 describes the operating principles and construction of our FIR laser, which formed a basic tool in nearly all our laboratory experiments. A brief discussion of the Lorenz instability in FIR lasers is also given, in connection with various observations we have made of spontaneous pulsations and excess low-frequency noise on the laser output, and which have recently been the subject of considerable study by other researchers. Chapter four describes FIR laser sideband generation using small-area Schottky diodes and comer-cube antennas. The construction and performance of our corner-cubes is outlined, including the first direct measurement of the main beam efficiency of a corner-cube antenna in the FIR, and a comparison with theory. The construction and measured performance of the rest of the sideband generator is also described. A detailed, quantitative model has been developed for the conversion efficiency obtainable from Schottky diodes in this application. We find that the low conversion efficiency (-39 db) measured in our experiments, and comparable to that found by other researchers, is inherent in the diode and well predicted by the model. For our particular experiment, the model predicts -28 db loss due to the diode, plus approximately -10 db loss due to the antenna coupling efficiency. The dependence of conversion efficiency on diode parameters is studied and guidelines for future optimization derived. Unfortunately, the severe conversion loss we measure, combined with low FIR laser power and (somewhat less significantly) poor optics transmission, leads to our presently available LO power being inadequate to obtain astronomically useful sensitivity, by a large factor.
", "date": "1988", "date_type": "degree", "id_number": "CaltechTHESIS:01222013-150156111", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01222013-150156111", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "NASA", "grant_number": "NAGW-107" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Caltech Submillimeter Observatory", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2013-01-22 23:37:33", "doi": "10.7907/79cv-bm83", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "email": "mcc@caltech.edu", "id": "Cross-M-C", "name": { "family": "Cross", "given": "Michael Clifford" }, "role": "member" }, { "email": "rutledge@caltech.edu", "id": "Rutledge-D-B", "name": { "family": "Rutledge", "given": "David B." }, "role": "member" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1987-10-07", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1988", "author_list": "Grossman, Erich Nathan" }, { "id": "/id/eprint/6690", "eprint_id": 6690, "rev_number": 27, "documents": [ { "id": "/id/document/13653", "doc_id": 13653, "rev_number": 5, "files": [ { "id": "/id/file/88654", "fileid": 88654, "datasetid": "document", "objectid": 13653, "filename": "Finger_mh_1988.pdf", "mime_type": "application/pdf", "filesize": 6161674, "mtime": "2012-12-26 04:38:54", "url": "/6690/3/Finger_mh_1988.pdf" } ], "eprint_id": 6690, "pos": 3, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Finger_mh_1988.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/105617", "doc_id": 105617, "rev_number": 3, "files": [ { "id": "/id/file/323112", "fileid": 323112, "datasetid": "document", "objectid": 105617, "filename": "Finger_mh_1988.zip", "mime_type": "application/x-zip", "hash": "0ecc9cc97bfee01623fe3a298ede6c28", "hash_type": "MD5", "filesize": 15038064, "mtime": "2020-01-24 01:49:56", "url": "/6690/4/Finger_mh_1988.zip" } ], "eprint_id": 6690, "pos": 4, "placement": 4, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "TIFFs", "language": "en", "security": "internal", "license": "other", "main": "Finger_mh_1988.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/127059", "doc_id": 127059, "rev_number": 1, "files": [ { "id": "/id/file/372493", "fileid": 372493, "datasetid": "document", "objectid": 127059, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "0e0bbf738ec93bcfa072c764f4d5d016", "hash_type": "MD5", "filesize": 32192, "mtime": "2021-06-24 01:23:34", "url": "/6690/5/indexcodes.txt" } ], "eprint_id": 6690, "pos": 5, "placement": 5, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/13653" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13653" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13653" } ] } } ], "eprint_status": "archive", "userid": 1854, "dir": "disk0/00/00/66/90", "datestamp": "2011-09-28 16:21:00", "lastmod": "2021-04-16 23:24:30", "status_changed": "2011-09-28 16:21:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mark.h.finger@nasa.gov", "id": "Finger-Mark-Harold", "name": { "family": "Finger", "given": "Mark Harold" }, "show_email": "NO" } ] }, "title": "The Imaging of Extra-Galactic Low-Energy Gamma-Ray Sources: Prospects, Techniques, and Instrumentation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "The handful of extra-galactic low-energy gamma-ray sources so far observed are all active galaxies, which are expected to dominate future detections. The nature of these compact, highly luminous sources is at present not clear; however, they may be powered by massive black holes. Many of these sources may produce their peak luminosity in the 0.5 to 5.0 MeV energy band, and observation in this energy range will be important in revealing the nature of their central power-house.
\r\n\r\nImproved understanding of the nature of active galaxies will require detailed observations of 10-20 sources, while understanding of their gamma-ray luminosity function and its evolution will require the detection of ~100 sources. From x-ray number counts and the presently available information about active galaxy spectra, we estimate the hard x-ray and low-energy gamma-ray number source-flux relation N(>S) for active galaxies. Instruments capable of detecting ~100 active galaxies at low-energy gamma-ray energies are achievable. These instruments will, however, be observing sources with fluxes some 10\u207b\u00b3 - 10\u207b\u2074 times lower than their instrumental background level, and will require careful control of systematic errors.
\r\n\r\nThe angular resolution of an instrument, as well as its sensitivity, can limit the number of sources it can observe. We present an investigation of the angular resolution requirements for future low-energy gamma-ray instruments. We find that the strictest requirements arise not from the need to resolve detectable sources, but from the need to control the level of direction-to-direction fluctuations in the diffuse background level. We conclude that gamma-ray instruments capable of detecting 100 active galaxies must have sub-degree angular resolution.
\r\n\r\nWe propose use of the coded aperture imaging technique as a method of achieving accurate control of systematic errors and fine angular resolution without unduly increasing the time needed to conduct full-sky surveys. This is a technique that employs a partially opaque mask to spatially modulate the source flux incident upon a position-sensitive photon detector. We present an analysis of coded aperture imaging for instruments that employ masks based on hexagonal uniformly redundant arrays. Rotation of such a mask allows complete, position-by-position background subtraction on short time-scales, and removes the periodic ambiguity inherent in uniformly redundant arrays.
\r\n\r\nAn instrument, the Gamma-ray Imaging Payload, has been built that employs these imaging techniques. The primary detector of the instrument is a 41 cm diameter by 5 cm thick NaI(Tl) Anger camera. We describe the design and testing of the instrument in detail. Preliminary results from a balloon flight of the instrument are shown, demonstrating its imaging performance.
", "date": "1988", "date_type": "degree", "id_number": "CaltechTHESIS:09272011-105853397", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09272011-105853397", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NGR 05-002-160" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Space Radiation Laboratory", "Astronomy Department" ] }, "deposited_on": "2011-09-28 16:21:00", "doi": "10.7907/yagn-1j29", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "chair" }, { "id": "Peck-C-W", "name": { "family": "Peck", "given": "Charles W." }, "role": "member" }, { "email": "boehm@caltech.edu", "id": "Boehm-F-H", "name": { "family": "Boehm", "given": "Felix H." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1987-08-18", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"archive", "userid": 50, "dir": "disk0/00/00/74/86", "datestamp": "2013-02-20 23:43:48", "lastmod": "2021-04-16 22:25:01", "status_changed": "2013-02-20 23:43:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Morris-Michael-Scott", "name": { "family": "Morris", "given": "Michael Scott" }, "show_email": "NO" } ] }, "title": "The R +\u025bR\u00b2 Cosmology", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis presents the study of a model cosmology based on the R +\u025bR\u00b2 gravitational Lagrangian. It may be roughly divided into two distinct parts. First, the classical inflationary scenario is developed. Then, the formalism of quantum cosmology is employed to determine initial conditions for the classical model.
\r\n\r\nIn the work on the classical model, the evolution equations for an isotropic and homogeneous universe are solved to exhibit both early-time inflation and a smooth transition to subsequent radiation-dominated behavior. Then perturbations on this isotropic background are evolved through the model to provide constraints on the model parameters from the observational limits on anisotropy today. This study concludes that such an inflationary model will prove a viable description for our universe if the initial Hubble parameter Hi is bounded from below, Hi > 10\u207b\u2075 lPl\u207b\u00b9, and if \u025b > 10\u00b9\u00b9 lPl\u00b2.
\r\n\r\nIn the work on the wave function, the two boundary conditions of Vilenkin (\"tunneling from nothing\") and Hartle and Hawking (\"no boundary\") are compared. The wave functions obtained are restricted to the initial edge of classical Lorentzian inflationary trajectories as distributions over initial conditions for the classical inflationary model. It is found that Vilenkin's wave function prefers the universe to undergo a great deal of inflation, whereas Hartle and Hawking's wave function prefers the universe to undergo little inflation. Finally, both boundary conditions are shown to require that inhomogeneous perturbative modes start out in their ground states.
", "date": "1988", "date_type": "degree", "id_number": "CaltechTHESIS:02202013-144403198", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:02202013-144403198", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1103/physrevd.34.2934" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1103/physrevd.39.1511" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_on": "2013-02-20 23:43:48", "doi": "10.7907/h44f-9639", "alt_title": { "items": [ "The R +\u025bR^2 Cosmology" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "preskill@caltech.edu", "id": "Preskill-J-P", "name": { "family": "Preskill", "given": "John P." }, "role": "member" }, { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1988-05-20", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Braunstein-Samuel-Leon", "name": { "family": "Braunstein", "given": "Samuel Leon" }, "show_email": "NO" } ] }, "title": "Novel Quantum States and Measurements", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "i) The quantum mechanics of higher order parametric amplifiers is studied. It is shown that these devices produce meaningful quantum states; numerical calculations are performed that demonstrate the convergence of matrix elements associated with these states. Further, the correspondence between the classical and quantum evolution for these devices is studied and the differences explained by a kind of \"quantum diffusion.\" Finally, the possibility of producing ordinary squeezed light with these devices is noted.
\r\n\r\nii) The generation of squeezed light always involves some scheme that amounts to pumping electromagnetic modes at near twice their natural frequency. When the pump is itself treated quantum mechanically, extra noise is introduced that ultimately limits the amount of squeezing achievable. Detailed calculations are carried out in this regard for the parametric amplifier. It is found that the pump's initial phase noise is responsible for this limit.
\r\n\r\niii) Quantum-mechanical measurements are usually described by applying the standard quantum rules to a measurement model. They can also be described by a formalism that uses mathematical objects called Effects and Operations. These two descriptions should be equivalent. D'Espagnat has raised a question about the usage of this formalism of Effects and Operations for repeated measurements. This question is cleared up, and the source of the discrepancy is given a simple interpretation.
\r\n\r\niv) Usually, an inequality that is chained becomes a weaker inequality. Chaining the Bell inequality, however, leads to stronger violations by quantum mechanics. Further, a new kind of Bell inequality, based on the information obtained in a measurement, is derived. This information Bell inequality can be used to formulate tests of local realism in very general circumstances, e.g., higher spin versions of the EPR experiment. These new inequalities yield an interpretation for the size of their violation and lead to the formulation of a hierarchy of Bell inequalities for which two-particle Bell inequalities play a special role.
\r\n", "date": "1988", "date_type": "degree", "id_number": "CaltechETD:etd-06192009-150752", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06192009-150752", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1103/physreva.35.1659" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1103/physreva.38.4696" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1007/bf00661312" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" }, { "agency": "NSF" }, { "agency": "Office of Naval Research (ONR)" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-06-22", "doi": "10.7907/9K1B-7X39", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Caves-C", "name": { "family": "Caves", "given": "Carlton" }, "role": "advisor" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "politzer@theory.caltech.edu", "id": "Politzer-H-D", "name": { "family": "Politzer", "given": "Hugh David" }, "role": "chair" }, { "id": "Caves-C", "name": { "family": "Caves", "given": "Carlton" }, "role": "member" }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "Ronald W. P." }, "role": "member" }, { "email": "bsimon@caltech.edu", "id": "Simon-B-M", "name": { "family": "Simon", "given": "Barry M." }, "role": "member" }, { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "role": "member" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-06-19", "thesis_defense_date": "1988-05-17", "thesis_approved_date": "2009-06-22", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1988", "author_list": "Braunstein, Samuel Leon" }, { "id": "/id/eprint/3411", "eprint_id": 3411, "rev_number": 14, "documents": [ { "id": "/id/document/5946", "doc_id": 5946, "rev_number": 4, "files": [ { "id": "/id/file/35379", "fileid": 35379, "datasetid": "document", "objectid": 5946, "filename": "Porter_ac_1988.pdf", "mime_type": "application/pdf", "filesize": 15601668, "mtime": "2012-12-26 02:59:44", "url": "/3411/1/Porter_ac_1988.pdf" } ], "eprint_id": 3411, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Porter_ac_1988.pdf", "language": "en", "security": "internal", "license": "other", "main": "Porter_ac_1988.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Porter-Alain-Cheyney", "name": { "family": "Porter", "given": "Alain Cheyney" }, "show_email": "NO" } ] }, "title": "Isophotometry of Brightest Elliptical Galaxies in Rich Clusters", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "This thesis presents ellipse-fitting isophotometry of 175 brightest elliptical galaxies in Abell clusters (BCEs). Galaxy structure is traced to an average major axis of 50 kpc, and some galaxies are traced beyond 100 kpc. The data consist not only of major- and minor-axis surface brightness profiles but also of isophote ellipticity, major axis position angle, and centroid position profiles.
\r\n\r\nAlmost all BCEs have some local structure that does not show in an azimuthally averaged brightness profile. However, local structure shows no correlation with global parameters such as galaxy luminosity or size. These results echo similar earlier findings for field ellipticals.
\r\n\r\nThe average ellipticity of a BCE is a strongly increasing function of physical radius as are most individual ellipticity profiles. This distinguishes BCEs as a class from other elliptical galaxies and explains why cD halos as a class are highly flattened. The deficit of large round isophotes is so marked that the isoluminosity surfaces of BCEs at large radii cannot be drawn from a population of randomly oriented oblate spheroids. This is the first sample of galaxies for which such an exclusion has been possible.
\r\n\r\nThe distinction of the isophotes from an oblate population becomes possible over the same range of radii (20-30 kpc) at which the isophotes become significantly aligned with the global position angle of the cluster. These results confirm and further quantify the long-suspected origin of BCEs in cluster material. The detection of nonconcentric light in 20% of the BCEs in the sample suggests that some galaxy construction continues to the present day.
\r\n\r\nParticular attention has been paid to the morphology of cD halos. The inner edges of these halos range from sharp to very gradual, are almost always associated with sudden ellipticity increases, and often also with isophote twists or nonconcentric light. This indicates that they have some dynamically significant identity, perhaps as material accreted from the cluster.
\r\n\r\nAn analytic method for separating the light distributions of overlapping binary galaxies has been derived and applied to images of 12 such systems. It is based solely on the assumption that each galaxy in the pair has point-reflection symmetry about its own center. Nonconcentric light is a probe of interactions between the members of the pair.
\r\n", "date": "1988", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-112224", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-112224", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" }, { "agency": "ARCS Foundation" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-17", "doi": "10.7907/3WWA-4575", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "chair" }, { "email": "srk@astro.caltech.edu", "id": "Kulkarni-S-R", "name": { "family": "Kulkarni", "given": "Shrinivas R." }, "role": "member" }, { "email": "djorgovski@caltech.edu", "id": "Djorgovski-G", "name": { "family": "Djorgovski", "given": "George" }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1987-12-09", "thesis_approved_date": "2008-09-17", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1988", "author_list": "Porter, Alain Cheyney" }, { "id": "/id/eprint/3410", "eprint_id": 3410, "rev_number": 23, "documents": [ { "id": "/id/document/5945", "doc_id": 5945, "rev_number": 3, "files": [ { "id": "/id/file/35371", "fileid": 35371, "datasetid": "document", "objectid": 5945, "filename": "Wang_h_1988.pdf", "mime_type": "application/pdf", "filesize": 15399334, "mtime": "2012-12-26 02:59:44", "url": "/3410/1/Wang_h_1988.pdf" } ], "eprint_id": 3410, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Wang_h_1988.pdf", "language": "en", "security": "internal", "license": "other", "main": "Wang_h_1988.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/109240" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/109240" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/109240" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/10", "datestamp": "2008-09-16", "lastmod": "2021-04-16 23:33:05", "status_changed": "2009-09-25 02:57:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "haimin.wang@njit.edu", "id": "Wang-Haimin", "name": { "family": "Wang", "given": "Haimin" }, "orcid": "0000-0002-5233-565X", "show_email": "YES" } ] }, "title": "Magnetic Fields and Supergranule Velocity Fields on the Quiet Sun", "ispublished": "unpub", "full_text_status": "public", "keywords": "Sun, magnetic fields, velocity fields, solar atmosphere", "abstract": "I have carried out detailed study on the quiet sun magnetic fields and super-granule velocity fields. This thesis consists of 6 themes. 1. I studied the statistical properties of quiet sun magnetic fields, including size distribution, evolution, flux budget of magnetic flux elements, and the magnetic diffusion constant. From the observations, I derived that the magnetic diffusion constant is \u2264150 km\u00b2/sec in the quiet region. I found that cancelling features and Ephemeral Regions are major sources of magnetic flux disappearance and replenishment. 2. I studied the supergranule velocity fields. Supergranule vertical velocities have a r.m.s. speed of 0.03 km/s. By observing the evolution of individual supergranule cells, I found that the average lifetime of supergranules is \u226550 hours. 3. I measured the contrast of faculae near the solar limb. The measurements show no obvious contrast increase or decrease near the solar limb. The observation fits neither the \"hot wall\" nor \"hot cloud\" fluxtube model. 4. I measured the separation velocities of new bipoles. The observed values are several times smaller than the values estimated by the theory of magnetic buoyancy. 5. I applied the local correlation tracking technique to BBSO Videomagnetogram data and detected an approximate radial intranetwork flow pattern. 6. I studied the relationship between magnetic fields and convection velocity fields. I found that ephemeral regions have a light tendency to emerge at or near the boundaries of supergranules; supergranules have the same scale, correlation lifetime and mean horizontal speed in the enhanced network region as in the mixed polarity quiet sun; the velocity of moving magnetic features that surround sunspots is consistent with the direct Doppler measurement.", "date": "1988", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-111823", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-111823", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1007/bf00171711" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1007/bf00148532" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1007/bf00206424" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "https://doi.org/10.1007/bf00148204" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "https://doi.org/10.1007/bf00148723" }, { "description": "Article adapted for Chapter 7.", "type": "doi", "url": "https://doi.org/10.1007/bf00147252" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-16", "doi": "10.7907/1cja-6j65", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "role": "chair" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1988-04-25", "thesis_approved_date": "2008-09-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1988", "author_list": "Wang, Haimin" }, { "id": "/id/eprint/3407", "eprint_id": 3407, "rev_number": 16, "documents": [ { "id": "/id/document/5942", "doc_id": 5942, "rev_number": 3, "files": [ { "id": "/id/file/35349", "fileid": 35349, "datasetid": "document", "objectid": 5942, "filename": "Kumar_p_1988.pdf", "mime_type": "application/pdf", "filesize": 5510201, "mtime": "2012-12-26 02:59:43", "url": "/3407/1/Kumar_p_1988.pdf" } ], "eprint_id": 3407, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Kumar_p_1988.pdf", "language": "en", "security": "internal", "license": "other", "main": "Kumar_p_1988.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/105836" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/105836" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/07", "datestamp": "2008-09-16", "lastmod": "2021-04-19 22:29:08", "status_changed": "2009-09-25 02:57:57", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kumar-Pawan", "name": { "family": "Kumar", "given": "Pawan" }, "show_email": "NO" } ] }, "title": "Excitation and Damping of Solar P-Modes", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "I have carried out detailed analysis of the interaction of acoustic radiation with homogeneous turbulence in order to understand the excitation of solar p-modes by turbulent convection. The most significant outcome of this investigation is the finding that, for certain types of forced turbulences, the absorption of acoustic waves is no greater than a free turbulence, whereas the emission is always enhanced by a factor M\u207b\u00b2, where M is the Mach number of the turbulence. Turbulent convection in the sun is an example of this kind of turbulence. This leads to the conclusion that energies in solar p-modes, due to their interaction with the convection, should be approximately equal to the thermal energy in a resonant eddy. This is found to be in good agreement with the observations. The ideas developed in the above work have been applied to explain the recently observed absorption of acoustic waves by sunspots as well. Work has also been carried out to determine the probability distribution function for the time averaged energy of stochastically excited modes. We hope to learn about the nature of the excitation and damping processes for the solar modes by comparing this theoretically determined distribution with the observations.
\r\n\r\nIn an effort towards resolving the overstability question of solar p-modes, I have investigated the effectiveness of 3-mode couplings, the most plausible process for limiting the amplitudes of overstable modes. The 3-mode coupling mechanism is also a good candidate for exciting fundamental modes which are found to be linearly stable, but are observed to have energies comparable to p-modes of similar frequencies. The issue of mode stability remains inconclusive due to the unknown energies of modes with period ~3.5 minutes. However, we find the fundamental modes to be damped as a result of mode couplings and hence they require excitation by a mechanism other than the overstability.
\r\n", "date": "1988", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-090628", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-090628", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/166108" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1086/166345" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-16", "doi": "10.7907/q6y2-3263", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Franklin-J-N", "name": { "family": "Franklin", "given": "Joel N." }, "role": "member" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1987-08-21", "thesis_approved_date": "2008-09-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"creators": { "items": [ { "id": "Wengler-Michael-James", "name": { "family": "Wengler", "given": "Michael James" }, "show_email": "NO" } ] }, "title": "Heterodyne Detection with Superconducting Tunnel Diodes", "ispublished": "unpub", "full_text_status": "public", "keywords": "SIS heterodyne mixer radioastronomy low-noise reciever superconducting tunnel junction", "abstract": "Heterodyne receivers based on superconductor-insulator-superconductor (SIS) tunnel diodes are the most sensitive available for near-millimeter wavelengths. Since the late seventies, receivers based on SISs have been used for millimeter band observations at radio observatories around the world. The work described here was carried out with the elusive goal in mind of developing ideal SIS receivers for radioastronomy. This thesis describes one researcher's path towards this goal.
\r\n\r\nIn the first chapter, a basic description of SIS diodes, their interaction with radiation, and heterodyne detection are given. The important detailed results of J. R. Tucker's tunnel diode heterodyne theory are described, since subsequent chapters rely on Tucker's work quite heavily. Throughout this introductory chapter, extremely simple (by comparison with the algebraic theoretical results) physical models are used to describe superconductivity, SISs, photon-assisted tunneling, and heterodyne detection. It is the author's experience that these physical models can be used to derive correct theoretical results, long before these results are proved rigorously.
\r\n\r\nThe second chapter presents a fully quantum mechanical theory of heterodyne detection with diodes. This theory was developed because Tucker's theory for tunnel diodes predicts a greater mixer sensitivity than is possible considering Heisenberg's uncertainty principle for radiation. Tucker does not quantize the radiation incident on the SIS, although his treatment of the isolated tunnel diode is completely quantum mechanical. In chapter 2, the quantization of radiation is carried out for heterodyne diode detectors. The formalism is shown to obey quantum limits on sensitivity. Finally, an ideal SIS mixer is shown to have noise properties identical to those of optical mixers based on ideal photodiodes.
\r\n\r\nIn possession of an apparently complete theory for SIS mixers, the third chapter presents a sampling of numerical results from that theory. Four different non-ideal tunnel diodes are used for these calculations so that a quantitative feel for the importance of diode quality can be achieved. The effects of dc and LO bias, signal and image source admittance, frequency of operation, and junction quality are all explored. This information will be useful for the proper engineering of SIS mixers. Finally, the fully optimized performance of the four tunnel diodes is presented as frequency is varied. It is shown that reasonably good quality lead-alloy SISs should behave like photodiodes up to frequencies as high as 1500 GHz.
\r\n\r\nFinally, chapter 4 presents a prototype open-structure SIS mixer. Measurements in the laboratory show this mixer to be quite sensitive for signal frequencies from 115 to 761 GHz. Unlike all other SIS receivers, in which the diode is mounted across a waveguide, this mixer relies on the bowtie-on-quartz antenna structure, which has been investigated by D. B. Rutledge and his students. This difference is essential to the multi-octave spectral coverage of this mixer. It is probable that waveguide designs will never achieve good results above 500 GHz, and as of now, there are no SIS-waveguide mixers which operate well above 300 GHz. Tests at the Owens Valley Radio Observatory verify the suitablility of this mixer for radioastronomy, but these tests have been limited to frequencies of 260 GHz and lower.
", "date": "1988", "date_type": "degree", "id_number": "CaltechETD:etd-02012007-084647", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-02012007-084647", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "NASA" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-02-09", "doi": "10.7907/TYQQ-RZ71", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "email": "wlj@caltech.edu", "id": "Johnson-W-L", "name": { "family": "Johnson", "given": "William Lewis" }, "role": "member" }, { "id": "McGill-T-C", "name": { "family": "McGill", "given": "Thomas C." }, "role": "member" }, { "email": "rutledge@caltech.edu", "id": "Rutledge-D-B", "name": { "family": "Rutledge", "given": "David B." }, "role": "member" }, { "email": "vahala@caltech.edu", "id": "Vahala-K-J", "name": { "family": "Vahala", "given": "Kerry J." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-02-01", "thesis_defense_date": "1987-06-05", "thesis_approved_date": "2007-02-09", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1988", "author_list": "Wengler, Michael James" }, { "id": "/id/eprint/5302", "eprint_id": 5302, "rev_number": 34, "documents": [ { "id": "/id/document/8686", "doc_id": 8686, "rev_number": 6, "files": [ { "id": "/id/file/53483", "fileid": 53483, "datasetid": "document", "objectid": 8686, "filename": "Ojakangas_gw_1988.pdf", "mime_type": "application/pdf", "filesize": 6860814, "mtime": "2012-12-26 03:18:14", "url": "/5302/1/Ojakangas_gw_1988.pdf" } ], "eprint_id": 5302, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original / No OCR", "language": "en", "security": "internal", "license": "other", "main": "Ojakangas_gw_1988.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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Episodic Volcanism of Tidally Heated Satellites with an Application to Io. II. Thermal State of an Ice Shell on Europa. III. Polar Wander of a Synchronously Rotating Satellite with Application to Europa", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science; Geophysics", "abstract": "Two examples of planetary bodies that may have coupled thermal and dynamical evolutions are investigated. The work is presented in three individual papers.
\r\n\r\nThe first example is that of a tidally heated satellite in an orbital resonance, for which the tidal dissipation rate is a strongly increasing function of the internal temperature. For such a satellite, a feedback mechanism exists between the orbital and thermal energies, which may lead to periodic variations in tidal heating within the satellite and its orbital eccentricity. A simple model of this mechanism is presented in the first paper and is applied specifically to Io.
\r\n\r\nThe second example is that of an ice shell on Europa, which is decoupled from the silicate core by a layer of liquid water. In the second paper, the spatially varying thickness that such a shell would have in thermal equilibrium with tidal dissipation within it, surface solar insolation and heat flow from the core is calculated for reasonable rheological laws for ice. The contribution of these variations in ice thickness to Europa's inertia tensor is estimated, and the implications for nonsynchronous rotation of Europa are discussed. In the third paper, a detailed dynamical model is developed, which demonstrates that such a shell may exhibit large\u2014scale polar wander as it approaches thermal equilibrium, because of the destabilizing effect of the variations in ice thickness on the inertia tensor of the shell.
\r\n\r\nThe abstracts of the three papers are reproduced below.
\r\n\r\nEpisodic Volcanism of Tidally Heated Satellites with Application to Io
\r\n\r\nA simple model of the coupled thermal and orbital evolution of a tidally heated satellite in an orbital resonance is presented and applied specifically to Io. The model quantitatively demonstrates how a feedback mechanism between the orbital and thermal energy of such a satellite can lead to periodic variations in surface heatflow and orbital eccentricity. The convective heatflow and (k/Q) of the satellite are parameterized as local power laws of the temperature, where Q is the quality factor and k is the second-degree tidal potential Love number. The time evolution of the model is determined by two nonlinear equations: an equation governing the orbital eccentricity, and a simple heat-balance equation determining the temperature. A linear stability analysis reveals that the time-independent solution is unstable if n > m + p, where n and m are the exponents in the power laws for (k/Q) and convective heatflow, respectively, and p is the ratio of the convective cooling time scale to the time scale for equilibration of the eccentricity. Numerical integration of the nonlinear equations reveals behavior in qualitative agreement with this relation. Laboratory data on near-solidus peridotites suggest 20 \u227e n \u227e 30, and parameterized convection schemes suggest m ~ 10. Since p is of order unity, it follows that tidally heated satellites are probably in the unstable regime if they are operating near the solidus. It is thus probable that Io has no thermal steady state. The model is made more realistic by (1) arresting the reduction of (k/Q) at low temperature, and (2) arresting the growth of temperature at the mantle solidus and allowing volcanism to remove the excess heat. When the second modification is included, the unstable regime becomes periodic. In addition, a global k substantially larger than the elastic value is possible for a mostly solid Io because the body may begin to behave viscously when the tidal period is longer than, or comparable to, the Maxwell time. This requires a solid-state viscosity of \u227e 4 x 10\u00b9\u2075 Pa s, which may be achievable with a small amount of partial melt. The model can easily be adjusted to pass through Io's current observed heatflow (1-2 W m\u207b\u00b2) and eccentricity (~ 0.004) for reasonable choices of parameters (Q/k)min ~ 100, (Q/k)max ~ few x 10\u00b3 solidus viscosity ~ 10\u00b9\u2075\u201310\u00b9\u2077 Pas, and QJ within the required dynamical bounds. The periods of high heatflow and acceptable eccentricity typically have duration of ~ 20-20 myr, separated in time by ~ 80-100 myr. Spatial heterogeneities in Io's thermal structure are likely to make the behavior more complicated. The model predicts that Io's mean motion may be currently increasing, a possibility suggested by recent estimates of \u1e45\u2081 from eclipse data. Since Europa's eccentricity mimics that of Io, the model also implies that the tidal stresses in Europa's ice shell may have recently been large enough to produce the observed fracturing. The episodic heating mechanism may be responsible for the resurfacing of Enceladus < 10\u2079 years ago.
\r\n\r\nThermal State of an Ice Shell on Europa
\r\n\r\nWe consider a model of Europa consisting of an ice shell that is decoupled from a silicate core by a layer of liquid water. The thickness of the shell is calculated as a function of colatitude and longitude, assuming that a state of conductive equilibrium exists with the incident annual average solar insolation, tidal dissipation within the shell, and heat flow from the core. Ice thickness profiles are calculated for each of two plausible rheological behaviors for ice: the Maxwell rheology and the generalized flow law rheology. In both cases the strong temperature\u2014dependence of the dissipation rate is explicitly included as well as the temperature\u2014dependence of the thermal conductivity of ice. Because of the strong temperature dependence of the dissipation rate, nearly all of the tidal dissipation is concentrated in the lowermost few kilometers of the shell. Even though the effective Q of the greater part of the shell is >> 100 in our models, average shell thicknesses do not exceed 25 km. Thus, if the total thickness of H\u2082O which mantles Europa is \u2273 25 km, none of the models admit the possibility of a completely frozen H\u2082O layer. The total dissipation rates in our models are comparable to those of a constant Q model with Q ~ 10. The thickness profiles are relatively insensitive to heat flow from the core. The second degree spherical harmonic components of the ice thickness are given and the resulting contributions to the quantities (B-A)/C and (B-C)/A of Europa are estimated. Although the contribution to (B-A)/C is perhaps larger than the permanent value needed to prevent nonsynchronous rotation, its dependence on the shell's orientation relative to synchroneity suggests that very slow nonsynchronous rotation will persist, with reorientation of the shell relative to the satellite-planet direction occurring on a timescale \u2273 the thermal diffusion timescale for the shell (~10\u2077 yr). The existence of a significant \"fossil\" bulge on the shell due to long-term elastic behavior of its outer, coldest regions would eliminate nonsynchronous rotation. Since the contribution to ((B-C)/A) of the thickness variations in most of our models is > 0, Europa may experience polar wander as thermal equilibrium is approached, if the above is the most important permanent contribution to ((B-C)/A). The magnitudes of the principal moment differences are insensitive to the details of the parameterization of the tidal dissipation.
\r\n\r\nPolar Wander of a Synchronously Rotating Satellite with Application to Europa
\r\n\r\nAn ice shell on Europa that is decoupled from the silicate core by a layer of liquid water has a thermal-equilibrium thickness profile that varies with position over its surface, because of spatial variations in the surface temperature and tidal dissipation within the ice (see previous paper). The second spherical harmonic degree components of these thickness variations and of any fossil rotational and tidal bulges present on the shell contribute to the inertia tensor of the body. The problem is that of a planetary elastic lithosphere that is topographically loaded from below. Following the development of Willemann and Turcotte (1981) we develop equations describing the variations in the inertia tensor of a body, which are caused by the addition of second harmonic degree topography to the base of the crust. Applied to the case of an ice shell on Europa, it is found for many choices of parameters that a state of thermal equilibrium for the shell will involve an orientation of Europa's principal axes of inertia (when the hydrostatic bulges are relaxed), which is unusual for a synchronously rotating satellite. Specifically, the intermediate and maximum principal moments are reversed. To reach the preferred orientation for synchronous satellites, a thermal equilibrium ice shell must execute a net reorientation of ninety degrees about the satellite\u2014planet direction. We present a simple model of a rigid, synchronously rotating satellite in a circular orbit for which the difference between the intermediate and maximum principal moments is linear in time, passing through zero when t = 0. The model demonstrates that the expected reorientation is indeed dynamically favored.
\r\n\r\nWe then consider a more realistic model, including the effects of various torques which act to couple the motions of the core, shell, and liquid water layer, as well as the effect of viscous dissipation which arises in the shell due to the predicted polar wander. It is found that the Poincar\u00e9 torque, gravitational coupling, and the torque due to viscous shear in the liquid water layer are unable to induce significant motion of the core during polar wander of the shell. However, the Poincar\u00e9 torque exerted on the liquid water layer by the shell is believed to cause the liquid water layer to reorient in coincidence with the shell. The model suggests that viscous friction in the shell eliminates the possibility that polar wander will occur unless preexisting fractures (e.g., due to tidal stresses (Crawford and Stevenson, 1988)) extend from the surface to a depth where the ice behaves viscously on the polar wander time scale. If the temperature Tf at the base of the fractured region is as high as ~ 140-145 K, the model indicates that polar wander occurs on a time scale of 10\u2076-10\u2075 y (shorter as Tf increases) after the sign of the difference between the maximum and intermediate principal moments reverses. In the absence of dissipation, polar wander would occur in ~ few x 10\u00b3 y. Polar wander must occur on a time scale significantly shorter than ~ 10\u2077 y, or the thickness profile of the ice will be in continuous equilibrium with its thermal environment regardless of its orientation, and the mechanism driving the polar wander will be virtually eliminated. It is likely that events of large scale polar wander occur episodically, separated in time by periods on the order of the time scale for thermal diffusion through the shell (~ 10\u2077 y), although a state of slow, continuous drifting of the pole is also possible. The time scale of viscous flow of topography at the base of the ice is also near 10\u2077 y. If dissipation in the shell due to polar wander is a few orders of magnitude smaller than our simple model suggests, polar wander as described here is a much more effective means for fracturing the ice than is tidal flexing, and it may contribute to producing the observed global fracture systems in Europa's ice.
\r\n", "date": "1988", "date_type": "degree", "id_number": "CaltechTHESIS:10162009-112521312", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10162009-112521312", "related_url": { "items": [ { "description": "Article adapted for Chapter I.", "type": "doi", "url": "https://doi.org/10.1016/0019-1035(86)90163-6" }, { "description": "Article adapted for Chapter II.", "type": "doi", "url": "https://doi.org/10.1016/0019-1035(89)90052-3" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Gayle Hammer", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Tony Diaz", "deposited_on": "2009-10-16 21:30:53", "doi": "10.7907/RMD6-XM66", "alt_title": { "items": [ "Episodic Volcanism of Tidally Heated Satellites with an Application to Io", "Thermal State of an Ice Shell on Europa", "Polar Wander of a Synchronously Rotating Satellite with Application to Europa" ] }, "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "advisor" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "chair" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Hager-B-H", "name": { "family": "Hager", "given": "Bradford H." }, "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1987-09-18", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "geophys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1988", "author_list": "Ojakangas, Gregory Wayne" }, { "id": "/id/eprint/7452", "eprint_id": 7452, "rev_number": 26, "documents": [ { "id": "/id/document/35139", "doc_id": 35139, "rev_number": 3, "files": [ { "id": "/id/file/111202", "fileid": 111202, "datasetid": "document", "objectid": 35139, "filename": "Friedson_aj_1987.pdf", "mime_type": "application/pdf", "hash": "405fb10c2aae2b412604820c6f1d00ff", "hash_type": "MD5", "filesize": 33130951, "mtime": "2013-01-29 23:19:54", "url": "/7452/1/Friedson_aj_1987.pdf" } ], "eprint_id": 7452, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Friedson_aj_1987.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"eprint_status": "archive", "userid": 87, "dir": "disk0/00/00/74/52", "datestamp": "2013-01-29 23:54:33", "lastmod": "2021-04-16 22:20:00", "status_changed": "2013-01-29 23:54:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Friedson-Andrew-James", "name": { "family": "Friedson", "given": "Andrew James" }, "show_email": "NO" } ] }, "title": "I. Meridional Energy Balance of Uranus. II. Viscosity of Rock-Ice Mixtures. III. The Thermosphere of Titan", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science; Physics", "abstract": "Part I:
\r\n\r\nThe seasonal meridional energy balance and thermal structure of the atmosphere of Uranus is investigated using a two-dimensional radiative-convective-dynamical model. Diurnal-average temperatures and heat fluxes are calculated as a function of pressure, latitude, and season. In addition to treating radiation and small-scale convection in a manner typical of conventional radiative-convective models, the dynamical heat fluxes due to large-scale baroclinic eddies are included and parameterized using a mixing length formulation (Stone, 1972; Ingersoll and Porco, 1978). The atmosphere is assumed to be bounded below by an adiabatic, fluid interior with a single value of potential temperature at all latitudes. The internal heat flux is found to vary with latitude and season. The total internal power and the global enthalpy storage rate are seen to oscillate in phase with a period of 1/2 Uranian year. On an annual-average basis, equatorward heat transport can take place in both the atmosphere and the convective interior. For a weak internal heat source, the meridional transport takes place predominantly in the atmosphere. If the internal heat source is larger, a greater share of the transport is taken up by the interior. For a value of the internal heat near the current upper limit for Uranus (~27% of the absorbed sunlight), about 1/3 of the equatorward heat transport at mid-latitudes occurs in the interior. For a given internal heat source, placing the peak of the solar heating at high altitudes or depositing the solar energy into a narrow altitude range favors heat transport by the atmosphere over the interior. Deep penetration of sunlight favors transport by the interior. For the time corresponding to the Voyager 2 Uranus encounter, the effective temperature at the south (sunlit) pole is calculated to be ~1.5 K higher than that at the equator. Horizontal contrasts of the mean 450-900 mbar temperature are found to be less than \u2264 1.5 K, in fair agreement with Voyager 2 IRIS results (Hanel et al., 1986), but the model fails to reproduce the local minimum in this temperature seen at 30\u00b0S. Nevertheless, it is concl uded that meridional heat transport in the atmosphere is efficient in keeping seasonal horizontal temperature contrasts below those predicted by radiative-convective models (Wallace, 1983).
\r\n\r\nPart II:
\r\n\r\nTheory and experiments are used to establish lower and upper bounds on the ratio of actual viscosity to pure ice viscosity for a suspension of rock particles in a water ice matrix. For typical conditions encountered in icy satellites, this ratio is of order ten or possibly larger, depending on unknown factors such as the particle size distribution. It is shown that even this modest increase in viscosity may be enough to have caused a failure of solidstate convective self-regulation early in the evolution of a homogeneous, rock-water ice satellite, provided the satellite is large enough and sufficiently silicate-rich. The criteria for this failure are satisfied by Ganymede and are marginal for Callisto, if the silicates are hydrated. Failure of self-regulation means that the viscosity is too high for the interior to remain completely solid and eliminate the heat production of long-lived radioisotopes by solid state convection. Partial melting of the ice then occurs. It is further shown that satellites of this size may then undergo runaway differentiation into a rock core and almost pure ice mantle, because the gravitational energy release is sufficient to melt nearly all the ice, and the Rayleigh-Taylor instability time scale is short. (Although the high pressure phases of ice melt, the resulting water quickly refreezes at a higher level.) We conjecture that these results explain the striking surface dissimilarity of Ganymede and Callisto, if these satellites accreted cold and undifferentiated. Ganymede may have gone supercritical (melted and differentiated) because of a failure of self-regulation, whereas Callisto remained undifferentiated to the present day. Like all proposed explanations for the Ganymede-Callisto dichotomy, this conjecture cannot be quantified with confidence, because of inadequate or incomplete observations, theory and experimental data.
\r\n\r\nPart III:
\r\n\r\nThe diurnal variation of the vertical structure of Titan's thermosphere is calculated through simultaneous solution of the equations of heat transfer and hydrostatic equilibrium. The temperature and density profiles are found above the mesopause. The dynamical response of the thermosphere to heating is for the most part neglected. Nevertheless, we are able to draw some interesting qualitative and quantitative conclusions regarding the vertical structure. Heating of the upper thermosphere occurs primarily through absorption of solar Lyman \u03b1 radiation by methane, with an additional amount of heating (\u2264 20%) due to low-energy magnetospheric electron precipitation. The heat is conducted downward to the mesopause, where it is removed by IR cooling due principally to acetylene. The mesopause is found to occur where the density is 2.2 x 1012 cm-3 (736 km) and has a temperature of ~110 K. The exospheric temperature is unlikely to exceed 225 K in the course of a Titan day. The diurnally averaged exospheric temperature is in the range 187-197 K, depending on the amount of magnetospheric electron heating that is included in the model. The amplitude of the diurnal variation is found to be \u2264 28 K. We find that the vertical extent of the hydrogen cloud is too large to be explained in terms of simple thermal escape of hydrogen from a ~225 K exosphere and conclude that other processes must be important for populating or heating the neutral torus.
", "date": "1987", "date_type": "degree", "id_number": "CaltechTHESIS:01292013-151449809", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01292013-151449809", "related_url": { "items": [ { "description": "Article adapted for Part I, Chapter 3.", "type": "doi", "url": "https://doi.org/10.1016/0019-1035(87)90010-8" }, { "description": "Article adapted for Part II.", "type": "doi", "url": "https://doi.org/10.1016/0019-1035(83)90124-0" }, { "description": "Article adapted for Part III.", "type": "doi", "url": "https://doi.org/10.1029/ja089ia01p00085" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2013-01-29 23:54:33", "doi": "10.7907/65ch-hj35", "alt_title": { "items": [ "Meridional Energy Balance of Uranus", "Viscosity of Rock-Ice Mixtures", "The Thermosphere of Titan" ] }, "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "yly@gps.caltech.edu", "id": "Yung-Y-L", "name": { "family": "Yung", "given": "Yuk L." }, "role": "chair" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "email": "duane.muhleman@gmail.com", "id": "Muhleman-D-O", "name": { "family": "Muhleman", "given": "Duane Owen" }, "role": "member" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1986-08-08", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1987", "author_list": "Friedson, Andrew James" }, { "id": "/id/eprint/4554", "eprint_id": 4554, "rev_number": 21, "documents": [ { "id": "/id/document/7374", "doc_id": 7374, "rev_number": 2, "files": [ { "id": "/id/file/45041", "fileid": 45041, "datasetid": "document", "objectid": 7374, "filename": "Kirk_rl_1987.pdf", "mime_type": "application/pdf", "filesize": 17917757, "mtime": "2012-12-26 03:09:41", "url": "/4554/1/Kirk_rl_1987.pdf" } ], "eprint_id": 4554, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Kirk_rl_1987.pdf", "language": "en", "security": "public", "license": "other", "main": "Kirk_rl_1987.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23899" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23899" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23899" } ] } }, { "id": "/id/document/16111", "doc_id": 16111, "rev_number": 3, "files": [ { "id": "/id/file/204388", "fileid": 204388, "datasetid": "document", "objectid": 16111, "filename": "Kirk_Randolph_Livingston_1987.txt", "mime_type": "text/plain", "filesize": 2568, "mtime": "2016-08-22 21:17:27", "url": "/4554/2/Kirk_Randolph_Livingston_1987.txt" } ], "eprint_id": 4554, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Kirk_Randolph_Livingston_1987.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/23899", "doc_id": 23899, "rev_number": 2, "files": [ { "id": "/id/file/45039", "fileid": 45039, "datasetid": "document", "objectid": 23899, "filename": "preview.png", "mime_type": "image/png", "hash": "785ffeb77f19b6152ddc2b256dcd5838", "hash_type": "MD5", "filesize": 12983, "mtime": "2012-12-26 03:09:41", "url": "/4554/3/preview.png" } ], "eprint_id": 4554, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7374" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7374" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7374" } ] } }, { "id": "/id/document/124384", "doc_id": 124384, "rev_number": 1, "files": [ { "id": "/id/file/369814", "fileid": 369814, "datasetid": "document", "objectid": 124384, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "980d07e7c62b2e68d5a0025a67444d4b", "hash_type": "MD5", "filesize": 1284, "mtime": "2021-06-23 23:31:11", "url": "/4554/4/indexcodes.txt" } ], "eprint_id": 4554, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16111" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16111" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16111" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/45/54", "datestamp": "2006-12-12", "lastmod": "2020-03-10 19:15:09", "status_changed": "2009-09-25 03:20:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "rkirk@usgs.gov", "id": "Kirk-Randolph-Livingstone", "name": { "family": "Kirk", "given": "Randolph Livingstone" }, "show_email": "YES" } ] }, "title": "I. Thermal Evolution of Ganymede and Implications for Surface Features. II. Magnetohydrodynamic Constraints on Deep Zonal Flow in the Giant Planets. III. A Fast Finite-Element Algorithm for Two-Dimensional Photoclinometry", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science; Physics", "abstract": "The work is divided into three independent papers:
\r\n\r\nPAPER I:
\r\n\r\nThermal evolution models are presented for Ganymede, assuming a mostly differentiated initial state of a water ocean overlying a rock layer. The only heat sources are assumed to be primordial heat (provided by accretion) and the long-lived radiogenic heat sources in the rock component. As Ganymede cools, the ocean thins, and two ice layers develop, one above composed of ice I, and the other below composed of high-pressure polymorphs of ice. Subsolidus convection proceeds separately in each ice layer, its transport of heat calculated using a simple parameterized convection scheme and the most recent data on ice rheology. The model requires that the average entropy of the deep ice layer exceed that of the ice I layer. If the residual ocean separating these layers becomes thin enough, then a Rayleigh-Taylor-like (\"diapiric\") instability may ensue, driven by the greater entropy of the deeper ice and merging the two ice mantles into a single convective layer. This instability is not predicted by linear analysis but occurs for plausible finite amplitude perturbations associated with large Rayleigh number convection. The resulting warm ice diapirs may lead to a dramatic \"heat pulse\" at the surface and to fracturing of the lithosphere, and may be directly or indirectly responsible for resurfacing and grooved terrain formation on Ganymede. The timing of this event depends rather sensitively on poorly known rheological parameters but could be consistent with chronologies deduced from estimated cratering rates. Irrespective of the occurrence or importance of the heat pulse, we find that lithospheric fracturing requires rapid stress loading (on a timescale \u227e 104) years). Such a timescale can be realized by warm ice diapirism, but not directly by gradual global expansion. In the absence of any quantitative and self-consistent model for the resurfacing of Ganymede by liquid water, we favor resurfacing by warm ice flows,which we demonstrate to be physically possible, a plausible consequence of our models, compatible with existing observations, and a hypothesis testable by Galileo. We discuss core formation as an alternative driver for resurfacing, and conclude that it is less attractive. We also consider anew the puzzle of why Callisto differs so greatly from Ganymede, offering several possible explanations. The models presented do not provide a compelling explanation for all aspects of Ganymedean geological evolution, since we have identified several potential problems, most notably the apparently extended period of grooved terrain formation (several hundred million years), which is difficult to reconcile with the heat pulse phenomenon.
\r\n\r\nPAPER II:
\r\n\r\nThe observed zonal flows of the giant planets will, if they penetrate below the visible atmosphere, interact significantly with the planetary magnetic field outside the metalized core. The appropriate measure of this interaction is the Chandrasekhar number Q = (H2)/(4\u03c0\u03c1\u03bd\u03b12\u03bb) (where H = radial component of the magnetic field, \u03bd = eddy viscosity, \u03bb = magnetic diffusivity, \u03b1-1 = lengthscale on which \u03bb varies); at depths where Q \u2273 1 the velocity will be forced to oscillate on a small lengthscale or decay to zero. We estimate the conductivity due to semiconduction in H2 (Jupiter, Saturn) and ionization in H2O (Uranus, Neptune) as a function of depth; the value \u03bb \u2243 1010 cm2s-1 needed for Q = 1 is readily obtained well outside the metallic core (where \u03bb \u2243 102 cm2s-1).
\r\n\r\nThese assertions are quantified by a simple model of the equatorial zonal jet in which the flow is assumed uniform on cylinders concentric with the spin axis, and the viscous and magnetic torques on each cylinder are balanced. We solve this \"Taylor constraint\" simultaneously with the dynamo equation to obtain the velocity and magnetic field in the equatorial plane. With this model we reproduce the widely differing jet widths of Jupiter and Saturn (though not the flow at very high or low latitudes) using \u03bd = 2500 cm2s-1, consistent with the requirement that viscous dissipation not exceed the specific luminosity. A model Uranian jet consistent with the limited Voyager data can also be constructed, with appropriately smaller \u03bd, but only if one assumes a two-layer interior. We tentatively predict a wide Neptunian jet.
\r\n\r\nFor Saturn (but not Jupiter or Uranus) the model has a large magnetic Reynolds number where Q = 1 and hence exhibits substantial axisymmetrization of the field in the equatorial plane. This effect may or may not persist at higher latitudes. The one-dimensional model presented is only a first step. Variation of the velocity and magnetic field parallel to the spin axis must be modeled in order to answer several important questions, including: 1) What is the behavior of flows at high latitudes, whose Taylor cylinders are interrupted by the region with Q \u2273 1? 2) To what extent is differential rotation in the envelope responsible for the spin-axisymmetry of Saturn's magnetic field?
\r\n\r\nPAPER III:
\r\n\r\nIt is shown that the problem of two-dimensional photoclinometry (PC) -- the reconstruction of a surface z(x,y) from a brightness image B(x,y) -- may be formulated in a natural way in terms of finite elements. The resulting system of equations is underdetermined as a consequence of the lack of boundary conditions for z, but a unique solution may be chosen by minimizing a function S expressing the \"roughness\" of the surface. An efficient PC algorithm based on this formulation is presented, requiring ~ 10.66 (four-byte) memory locations and ~104 floating multiplications/additions per pixel, and incorporating: 1) Minimization of the roughness by the penalty method, which yields the smallest set of equations. 2) Iterative solution of the nonlinear equations by Newton's method. 3) Solution of the linearized equations by an inner iterative cycle of successive over-relaxation, which takes advantage of the extreme sparseness of the system. 4) Multigridding, in which the solutions to the smaller problems obtained by reducing the resolution are used recursively to greatly speed convergence at the higher resolutions, and 5) A rapid noniterative initial estimate of z obtained by exploiting the special symmetry of the equations obtained in the first linearization.
\r\n\r\nThe algorithm is extensively demonstrated on 200 by 200 pixel synthetic \"images\" generated from digital topographic data for northern Utah over a range of phase angles. Rms error in the solution is ~ 22 m, out of ~ 660 m total relief. The error is dominated by \"stripes\" with the same azimuth as the light source, resulting from use of the roughness criterion in lieu of boundary conditions; the rms error along profiles parallel to the stripes is only ~ 2-8 m, depending on the phase angle. Satisfactory solutions are obtained even in the presence of quantization error, noise, and moderate blur in the image.
\r\n\r\nApplications of the PC algorithm to both remote sensing and photomicrography are sketched; a photoclinometric map of a low-relief Precambrian era fossil is presented as an example of the latter. Prospects for dealing with photometrically inhomogeneous surfaces, and an extension of the method to the analysis of side-looking radar data (\"radarclinometry\") are also discussed.
", "date": "1987", "date_type": "degree", "id_number": "CaltechETD:etd-11142006-131417", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-11142006-131417", "related_url": { "items": [ { "description": "Article adapted for Part I.", "type": "doi", "url": "https://doi.org/10.1016/0019-1035(87)90009-1" }, { "description": "Article adapted for Part II.", "type": "doi", "url": "https://doi.org/10.1086/165248" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-12-12", "doi": "10.7907/T5PT-S948", "alt_title": { "items": [ "Thermal Evolution of Ganymede and Implications for Surface Features", "Magnetohydrodynamic Constraints on Deep Zonal Flow in the Giant Planets", "A Fast Finite-Element Algorithm for Two-Dimensional Photoclinometry" ] }, "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "email": "djs@gps.caltech.edu", "id": "Stevenson-D-J", "name": { "family": "Stevenson", "given": "David John" }, "role": "member" }, { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "member" }, { "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "member" }, { "email": "kirschvink@caltech.edu", "id": "Kirschvink-J-L", "name": { "family": "Kirschvink", "given": "Joseph L." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-11-14", "thesis_defense_date": "1987-01-09", "thesis_approved_date": "2006-12-12", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1987", "author_list": "Kirk, Randolph Livingstone" }, { "id": "/id/eprint/3408", "eprint_id": 3408, "rev_number": 15, "documents": [ { "id": "/id/document/5943", "doc_id": 5943, "rev_number": 3, "files": [ { "id": "/id/file/35357", "fileid": 35357, "datasetid": "document", "objectid": 5943, "filename": "Lind_kr_1987.pdf", "mime_type": "application/pdf", "filesize": 11243279, "mtime": "2012-12-26 02:59:43", "url": "/3408/1/Lind_kr_1987.pdf" } ], "eprint_id": 3408, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Lind_kr_1987.pdf", "language": "en", "security": "public", "license": "other", "main": "Lind_kr_1987.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22483" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22483" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22483" } ] } }, { "id": "/id/document/22483", "doc_id": 22483, "rev_number": 3, "files": [ { "id": "/id/file/35355", "fileid": 35355, "datasetid": "document", "objectid": 22483, "filename": "preview.png", "mime_type": "image/png", "hash": "016b6d087180d2b7357788e0a3fc84af", "hash_type": "MD5", "filesize": 8953, "mtime": "2012-12-26 02:59:43", "url": "/3408/2/preview.png" } ], "eprint_id": 3408, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5943" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5943" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5943" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/08", "datestamp": "2008-09-12", "lastmod": "2021-04-16 22:26:24", "status_changed": "2009-09-25 02:57:58", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lind-Kevin-Robert", "name": { "family": "Lind", "given": "Kevin Robert" }, "show_email": "NO" } ] }, "title": "Observations and Gas Dynamics of Extragalactic Radio Jets", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "This thesis is a combined observational and theoretical study of extragalactic radio jets. Jets are defined observationally as extended, center-brightened features, which are observed in radio images at all resolution scales. They are defined theoretically as momentum-dominated, well-collimated plasma flows. There is now little debate as to the basic interpretation of radio jets as actual plasma outflows, but the detailed dynamics of the jets, or even whether the kiloparsec-scale jets are relativistic, are still uncertain. The resolution of the details of the physics of jets requires improved radio images, especially at the base of the jet, and detailed models of jets. Maps of the base of the radio jet can only be obtained with VLBI observations; detailed jet models require numerical simulations on a supercomputer.
\r\n\r\nThe observational work was a large global VLBI observation of the N galaxy 3C371. The goal was to detect and, if possible, map the underlying jet. This was done, and the results compared with a previous VLBI map, and with maps from other interferometers at lower resolution. No conclusions could be drawn regarding the nature of the jet, although it was clear that the jet was active, and appeared to vary on short time scales.
\r\n\r\nThe theoretical work was in two parts, both of which were directed toward refining existing theories. The first part was to calculate the emission for relativistically moving patterns which themselves contain relativistic flows, to determine how much the flux as a function of viewing angle may vary between realistic models of the knots in relativistic jets. It was found that considerable variation was possible, and that superluminal expansion rates were not necessarily good determiners of the bulk flow rate. The second part was to develop a code to simulate axisymmetric magnetized jets propagating into a uniform medium. This was implemented for the case of toroidal field only, and run for a moderately magnetized injected jet. It was found that, although most of the jet dynamics was determined by the nonmagnetic forces, the influence of the magnetic tension focused the flow sufficiently to significantly increase the speed of advance of the jet.
\r\n", "date": "1987", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-091639", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-091639", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/wnqa-gn45", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "chair" }, { "email": "dscohen@caltech.edu", "id": "Cohen-D-S", "name": { "family": "Cohen", "given": "Donald S." }, "role": "member" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "id": "Sturtevant-B", "name": { "family": "Sturtevant", "given": "Bradford" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1986-11-20", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1987", "author_list": "Lind, Kevin Robert" }, { "id": "/id/eprint/3345", "eprint_id": 3345, "rev_number": 18, "documents": [ { "id": "/id/document/5866", "doc_id": 5866, "rev_number": 3, "files": [ { "id": "/id/file/34835", "fileid": 34835, "datasetid": "document", "objectid": 5866, "filename": "Chou_d_1987.pdf", "mime_type": "application/pdf", "filesize": 2417034, "mtime": "2012-12-26 02:59:14", "url": "/3345/1/Chou_d_1987.pdf" } ], "eprint_id": 3345, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Chou_d_1987.pdf", "language": "en", "security": "public", "license": "other", "main": "Chou_d_1987.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22406" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22406" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22406" } ] } }, { "id": "/id/document/22406", "doc_id": 22406, "rev_number": 3, "files": [ { "id": "/id/file/34833", "fileid": 34833, "datasetid": "document", "objectid": 22406, "filename": "preview.png", "mime_type": "image/png", "hash": "dc2b5a94b5244e577488d02d377bbb9d", "hash_type": "MD5", "filesize": 10431, "mtime": "2012-12-26 02:59:14", "url": "/3345/2/preview.png" } ], "eprint_id": 3345, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5866" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5866" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5866" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/45", "datestamp": "2008-09-10", "lastmod": "2021-04-16 22:21:13", "status_changed": "2009-09-25 02:57:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chou-Dean-Yi", "name": { "family": "Chou", "given": "Dean-Yi" }, "show_email": "NO" } ] }, "title": "Development and Evolution of Magnetic Fields in Active Regions on the Sun", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "The purpose of this thesis is to investigate the development and evolution of magnetic fields in new active regions on the sun. The major observations are digital magnetograms of the line-of-sight component of magnetic fields made with the high sensitivity videomagnetograph at the Big Bear Solar Observatory, and H\u03b1 filtergrams with the 1/4 \u00c5 H\u03b1 Zeiss filter.
\r\n\r\nThis thesis consists of three themes. First, the separation velocity of emerging magnetic flux is investigated. I measure the separation velocities of opposite polarities of 24 new bipoles, and compare them with the theoretical values estimated by the present theory of magnetic buoyancy. The predicted velocities are higher than those observed. Second, the cooling time scale of growing sunspots is studied. I define the cooling time scale and derive it from the measurements of intensity and magnetic field strength of sunspots. The cooling time scales of the ten growing sunspots studied range from 0.5 to 9 hr. I also estimate the cooling time scale from two models, the Inhibition Model and the Alfven Wave Model, based on linear theory. Both models give cooling times of about 0.05 hr. Third, nonadiabatic effects in convective instabilities in thin flux tubes are examined. I study the convective instabilities in thin flux tubes by including a nonadiabatic term. I find that a flux tube is convectively stable for any field strength.
", "date": "1987", "date_type": "degree", "id_number": "CaltechETD:etd-09052008-154229", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09052008-154229", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1007/bf00148204" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1086/164940" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/rkc8-g529", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "member" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-05", "thesis_defense_date": "1986-09-11", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1987", "author_list": "Chou, Dean-Yi" }, { "id": "/id/eprint/3230", "eprint_id": 3230, "rev_number": 15, "documents": [ { "id": "/id/document/5721", "doc_id": 5721, "rev_number": 3, "files": [ { "id": "/id/file/33878", "fileid": 33878, "datasetid": "document", "objectid": 5721, "filename": "Finn_ls_1987.pdf", "mime_type": "application/pdf", "filesize": 10456516, "mtime": "2012-12-26 02:58:17", "url": "/3230/1/Finn_ls_1987.pdf" } ], "eprint_id": 3230, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Finn_ls_1987.pdf", "language": "en", "security": "public", "license": "other", "main": "Finn_ls_1987.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22263" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22263" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22263" } ] } }, { "id": "/id/document/15958", "doc_id": 15958, "rev_number": 3, "files": [ { "id": "/id/file/204030", "fileid": 204030, "datasetid": "document", "objectid": 15958, "filename": "Finn_Lee_Samuel_1987.txt", "mime_type": "text/plain", "filesize": 2179, "mtime": "2016-08-22 21:16:37", "url": "/3230/2/Finn_Lee_Samuel_1987.txt" } ], "eprint_id": 3230, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Finn_Lee_Samuel_1987.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/22263", "doc_id": 22263, "rev_number": 3, "files": [ { "id": "/id/file/33876", "fileid": 33876, "datasetid": "document", "objectid": 22263, "filename": "preview.png", "mime_type": "image/png", "hash": "d45e59503a9f931d390b06d3c7d9235e", "hash_type": "MD5", "filesize": 8399, "mtime": "2012-12-26 02:58:16", "url": "/3230/3/preview.png" } ], "eprint_id": 3230, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5721" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5721" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5721" } ] } }, { "id": "/id/document/123477", "doc_id": 123477, "rev_number": 1, "files": [ { "id": "/id/file/368890", "fileid": 368890, "datasetid": "document", "objectid": 123477, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "bc6f5a72f8ec9aa7dde1f1e796343786", "hash_type": "MD5", "filesize": 1083, "mtime": "2021-06-23 22:41:12", "url": "/3230/4/indexcodes.txt" } ], "eprint_id": 3230, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15958" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15958" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15958" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/30", "datestamp": "2008-09-09", "lastmod": "2020-03-10 23:39:06", "status_changed": "2009-09-25 02:54:54", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "lsfinn@psu.edu", "id": "Finn-Lee-Samuel", "name": { "family": "Finn", "given": "Lee Samuel" }, "show_email": "YES" } ] }, "title": "Relativistic Stellar Pulsations", "ispublished": "unpub", "full_text_status": "public", "keywords": "Stellar pulsations; neutron stars; gravitational waves", "abstract": "This thesis consists of studies on the topic of relativistic stellar pulsations.
\r\n\r\ni) A new formalism for the numerical study of g-modes in neutron stars is developed. This formalism avoids pitfalls associated with previous formalisms when applied to the study of these low-frequency modes. The formalism involves a new choice of perturbation variables, the introduction of an \"instantaneous gravity\" approximation to the field outside the star, and an energy principle for determining gravitational radiation damping times. The formalism is used to study g-modes that arise because of chemical inhomogeneities in neutron star crusts. g-mode frequencies associated with chemical inhomogeneities are found to be much higher than those associated with finite temperature.
\r\n\r\nii) The relativistic Cowling approximation, introduced by McDermott, Van Horn, and Scholl (1983) and analogous to the Newtonian Cowling approximation, is refined to make it more accurate in the regime of highly relativistic stars. The approximation is used to prove a host of useful theorems regarding the non-radial modes of relativistic stars.
\r\n\r\niii) Realistic neutron stars have a solid crust, and this will seriously affect their g-modes. The first steps toward developing a theory of non-radial relativistic pulsations in stars with a solid crust is reported on here: the calculation of the shear strain and stress during a pulsation, the introduction of the shear stress into the Einstein field equations as a source and to the equations of motion as a force, and the development of a Lagrangian and variational principle for studying non-radial relativistic pulsations in stars with a solid crust.
\r\n\r\niv) Solar five-minute oscillations are a weak source of gravitational radiation. The inner part of the solar system is actually in the transition zone of the solar oscillation gravitational field, and future space-based beam detectors might be able to measure the solar \"transition-zone radiation.\" The transition-zone gravitational field is explored for four relativistic gravity theories: a spin-zero theory (Nordst\u00f8m's theory), a spin-one theory (analogous to electromagnetism), a spin-two theory (general relativity), and a mixed spin-zero/spin-one theory (Jordan-Brans-Dicke theory). From the transition-zone gravitational field, it is possible to determine experimentally the spin content of relativistic gravity.
\r\n", "date": "1987", "date_type": "degree", "id_number": "CaltechETD:etd-08262008-093129", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08262008-093129", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1093/mnras/222.3.393" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1093/mnras/227.2.265" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1093/mnras/232.2.259" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "https://doi.org/10.1088/0264-9381/2/3/014" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/T7VS-8648", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "kgl@caltech.edu", "id": "Libbrecht-K-G", "name": { "family": "Libbrecht", "given": "Kenneth George" }, "role": "member" }, { "id": "Zachariasen-F", "name": { "family": "Zachariasen", "given": "Fredrik" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-26", "thesis_defense_date": "1987-05-11", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1987", "author_list": "Finn, Lee Samuel" }, { "id": "/id/eprint/7484", "eprint_id": 7484, "rev_number": 21, "documents": [ { "id": "/id/document/35488", "doc_id": 35488, "rev_number": 3, "files": [ { "id": "/id/file/112102", "fileid": 112102, "datasetid": "document", "objectid": 35488, "filename": "Rudy 1987.pdf", "mime_type": "application/pdf", "hash": "5da27226c4e16e298e81c68c5c09acb2", "hash_type": "MD5", "filesize": 28898031, "mtime": "2013-02-20 18:38:40", "url": "/7484/1/Rudy 1987.pdf" } ], "eprint_id": 7484, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Rudy 1987.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/35489", 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"archive", "userid": 50, "dir": "disk0/00/00/74/84", "datestamp": "2013-02-20 18:57:24", "lastmod": "2021-04-16 22:22:22", "status_changed": "2013-02-20 18:57:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rudy-Donald-James", "name": { "family": "Rudy", "given": "Donald James" }, "show_email": "NO" } ] }, "title": "Mars: High Resolution VLA Observations at Wavelengths of 2 and 6 cm and Derived Properties", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science; Physics", "abstract": "Observations of Mars at wavelengths of 2 and 6cm were made using the VLA in its A configuration. Two seasons were observed; late spring in the northern hemisphere (LS ~ 60\u00b0) and early summer in the southern summer (LS ~ 300\u00b0). The sub-earth latitudes were 25\u00b0N and 25\u00b0S, for each of these seasons respectively. So the geometry for viewing the polar region was optimal in each case. Whole-disk brightness temperatures were estimated to be 193.2 K \u00b1 1.0 at 2 cm and 191.2 K \u00b1 0.6 at 6 cm for the northern data set and 202.2 K \u00b1 l.0 at 2 cm and 195.4 K \u00b1 0.6 at 6 cm for the southern data set (formal errors only). Since measurements of the polarized flux were taken at the same time, whole-disk effective dielectric constants could be estimated and from these, estimates of sub-surface densities could be made. The results of these calculations at 2cm yielded whole-disk effective dielectric constants of 2.34 \u00b1 0.05 and 2.02 \u00b1 0.03 which imply sub-surface densities of 1.24 g cm-3 \u00b1 0.06 and 1.02 g cm-3 \u00b1 0.05 for the north and south, respectively. The same calculations at 6 cm yielded effective densities of 1.45 g cm-3 \u00b1 0.10 and 1.31 g cm-3 \u00b1 0.07 from effective dielectric constants of 2.70 \u00b1 0.09 and 2.48 \u00b1 0.06 for the north and south data sets, respectively.
\r\n\r\nFrom the mapped data these parameters were also estimated as a function of latitude between latitudes of 15\u00b0S and 60\u00b0N for the north data set; and between latitudes of 30\u00b0N and 60\u00b0S for the south data set. A region in which the brightness temperature behaves in an anomalous manner was discovered in both data sets. This region lies between about 10\u00b0S and 40\u00b0S. Here the brightness temperatures at both wavelengths in both data sets appears lower, by 4 K to 8 K, than a nominal model would predict. In addition to the effective dielectric constant and sub-surface density the radio absorption length of the sub-surface was estimated. The radio absorption length for most of these latitudes was about 15 wavelengths with formal errors on the order of 5 or 10 wavelengths. This is true for both data sets. The estimation of the effective dielectric constant at most latitudes was between 2 and 3.5 with only slight differences between the two different wavelengths. The two data sets show the same relative trends, but are off by a scaling factor.
\r\n\r\nThese estimates of the dielectric constant lead to estimation of the sub-surface densities as a function of latitude. Most calculations of the sub-surface density yielded results between 1 and 2 g cm-3 with errors on the order of 0.5 g cm-3. These results seem to imply that the sub-surface is not much different than the surface as observed by the Viking and Mariner missions. In line with this, an examination of the correlation of the dielectric constant at each wavelength with the thermal inertia, determined by the Viking infrared measurements, shows a relatively strong correlation, at both wavelengths, for the North data set. The South data set, however, shows little to nocorrelation between the radio parameters and the thermal inertia. Since the South data set is primarily composed of latitudes which contain the anomalous region, it is not suprising that the South data set shows no correlation.
\r\n\r\nIn addition, the thermal-radiative model used to estimate the above parameters was used to estimate the variability of the whole-disk brightness temperature of Mars. This was done in an effort to establish a background for those astronomers wishing to use Mars as a calibration source. The parameters investigated for their effect on the whole-disk brightness temperature of Mars were: the sub-earth longitude, the sub-earth latitude, the sub-earth time of day, the dielectric constant, and the radio absorption length. A nominal model was first created which established the variation of the brightness temperature as a function of season and radio absorption length. A nominal value of 2.2 was used for the dielectric constant, and the sub-earth latitude was set at 0\u00b0N and the sub-earth longitude was set at 75\u00b0W. The sub-earth time of day was held at noon for this nominal model. This is equivalent to a 0\u00b0 phase angle. The most important geometric factor was the sub-earth latitude. The error in estimating the whole-disk brightness temperature of Mars by using the wrong sub-earth latitude can be as large as 5 to 10%. The charts presented will be useful to estimate the whole-disk brightness temperature which the thermal model would predict. It is believed that the error in this estimate is less than or equal to 5 K.
\r\n", "date": "1987", "date_type": "degree", "id_number": "CaltechTHESIS:02202013-103037890", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:02202013-103037890", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_on": "2013-02-20 18:57:24", "doi": "10.7907/3g59-p796", "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "api@gps.caltech.edu", "id": "Ingersoll-A-P", "name": { "family": "Ingersoll", "given": "Andrew P." }, "role": "chair" }, { "email": "aalbee@gps.caltech.edu", "id": "Albee-A-L", "name": { "family": "Albee", "given": "Arden Leroy" }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Murray-B-C", "name": { "family": "Murray", "given": "Bruce C." }, "role": "member" }, { "email": "duane.muhleman@gmail.com", "id": "Muhleman-D-O", "name": { "family": "Muhleman", "given": "Duane Owen" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1987-03-02", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1987", "author_list": "Rudy, Donald James" }, { "id": "/id/eprint/3413", "eprint_id": 3413, "rev_number": 14, "documents": [ { "id": "/id/document/5948", "doc_id": 5948, "rev_number": 3, "files": [ { "id": "/id/file/35394", "fileid": 35394, "datasetid": "document", "objectid": 5948, "filename": "Edelson_r_1987.pdf", "mime_type": "application/pdf", "filesize": 18973688, "mtime": "2012-12-26 02:59:45", "url": "/3413/1/Edelson_r_1987.pdf" } ], "eprint_id": 3413, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Edelson_r_1987.pdf", "language": "en", "security": "public", "license": "other", "main": "Edelson_r_1987.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22488" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22488" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22488" } ] } }, { "id": "/id/document/22488", "doc_id": 22488, "rev_number": 3, "files": [ { "id": "/id/file/35392", "fileid": 35392, "datasetid": "document", "objectid": 22488, "filename": "preview.png", "mime_type": "image/png", "hash": "89e57f0e00e3f986eb2f3e540b989c18", "hash_type": "MD5", "filesize": 9398, "mtime": "2012-12-26 02:59:45", "url": "/3413/2/preview.png" } ], "eprint_id": 3413, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5948" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5948" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5948" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/13", "datestamp": "2008-09-17", "lastmod": "2021-11-05 23:00:53", "status_changed": "2009-09-25 02:58:03", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Edelson-Richard-Allen", "name": { "family": "Edelson", "given": "Richard Allen" }, "show_email": "NO" } ] }, "title": "Broadband Properties of Active Galactic Nuclei", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "The broadband radio-infrared-optical-ultraviolet properties of active galactic nuclei are used to investigate the nature of the central engine and the surrounding environment. Optically selected quasars (which have \u03b1̅IR = -1.09; S\u03bd \u221d \u03bd\u03b1) and Seyfert 1 galaxies (\u03b1̅IR = -1.15) tend to have relatively flat infrared spectra and low reddenings, while most Seyfert 2 galaxies (\u03b1̅IR = -1.56) and other dusty objects have steep infrared spectra and larger reddenings. The infrared spectra of most luminous radio-quiet active galaxies turn over near ~80 \u00b5m. It appears that the infrared spectra of most quasars and luminous Seyfert 1 galaxies are dominated by unreprocessed radiation from a synchrotron self-absorbed source of order a light day across, about the size of the hypothesized accretion disk. Seyfert 2 galaxies and other reddened objects have infrared spectra which appear to be dominated by thermal emission from warm (~50 K) dust, probably in the disk of the underlying galaxy. A broad emission feature, centered near 5 \u00b5m, is present in many luminous quasars and Seyfert 1 galaxies.
\r\n\r\nHighly polarized objects (\"blazars\") can be strongly variable at far-infrared wavelengths over time scales of months. There is no conclusive evidence for far-infrared variations in normal (low-polarization) quasars or Seyfert galaxies, although low-level flickering (at the ~30% peak-to-peak level) cannot be ruled out.
\r\n\r\nSeyfert galaxies tend to have steep radio spectra (\u03b1rad \u2248 -0.7). The radio spectra of Seyfert 1 galaxies often flatten out near 2 cm. There is no significant difference in the mean radio luminosities of Seyfert 1 and 2 galaxies. There are of order 105 Seyfert galaxies/Gpc3, most of which have 6 cm luminosities between 1037.0 and 1039.4 ergs/s and 60 \u00b5m luminosities between 1042.2 and 1045.0 ergs/s. The Seyfert 2 galaxy radio luminosity function cuts off sharply below 1037.4 ergs/s.
", "date": "1987", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-113501", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-113501", "related_url": { "items": [ { "description": "Article adapted for Chapter Two.", "type": "doi", "url": "https://doi.org/10.1086/164479" }, { "description": "Article adapted for Chapter Three.", "type": "doi", "url": "https://doi.org/10.1086/184763" }, { "description": "Article adapted for Chapter Four.", "type": "doi", "url": "https://doi.org/10.1086/165004" }, { "description": "Article adapted for Chapter Five.", "type": "doi", "url": "https://doi.org/10.1086/165627" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-17", "doi": "10.7907/gtk1-3n45", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "chair" }, { "id": "Moffet-A-T", "name": { "family": "Moffet", "given": "Alan Theodore" }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "orcid": "0000-0002-0438-3323", "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1986-11-12", "thesis_approved_date": "2008-09-17", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1987", "author_list": "Edelson, Richard Allen" }, { "id": "/id/eprint/4890", "eprint_id": 4890, "rev_number": 13, "documents": [ { "id": "/id/document/7787", "doc_id": 7787, "rev_number": 2, "files": [ { "id": "/id/file/47837", "fileid": 47837, "datasetid": "document", "objectid": 7787, "filename": "Blake_ga_1986.pdf", "mime_type": "application/pdf", "filesize": 18425174, "mtime": "2012-12-26 03:12:40", "url": "/4890/1/Blake_ga_1986.pdf" } ], "eprint_id": 4890, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Blake_ga_1986.pdf", "language": "en", "security": "public", "license": "other", "main": "Blake_ga_1986.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/24298" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/24298" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/24298" } ] } }, { "id": "/id/document/12121", "doc_id": 12121, "rev_number": 3, "files": [ { "id": "/id/file/204455", "fileid": 204455, "datasetid": "document", "objectid": 12121, "filename": "Blake_Geoffrey_A_1986.txt", "mime_type": "text/plain", "filesize": 907, "mtime": "2016-08-22 21:17:37", "url": "/4890/2/Blake_Geoffrey_A_1986.txt" } ], "eprint_id": 4890, "pos": 2, "format": "text/plain", "format_desc": "author ok 2004", "language": "en", "security": "internal", "license": "other", "main": "Blake_Geoffrey_A_1986.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/24298", "doc_id": 24298, "rev_number": 2, "files": [ { "id": "/id/file/47835", "fileid": 47835, "datasetid": "document", "objectid": 24298, "filename": "preview.png", "mime_type": "image/png", "hash": "fe3c3a5d3c6e547af04cdb1b12125076", "hash_type": "MD5", "filesize": 10397, "mtime": "2012-12-26 03:12:40", "url": "/4890/3/preview.png" } ], "eprint_id": 4890, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7787" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7787" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7787" } ] } }, { "id": "/id/document/124584", "doc_id": 124584, "rev_number": 1, "files": [ { "id": "/id/file/370014", "fileid": 370014, "datasetid": "document", "objectid": 124584, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "b7d8bd9070552aead23ed5fc46c0983d", "hash_type": "MD5", "filesize": 482, "mtime": "2021-06-23 23:43:08", "url": "/4890/4/indexcodes.txt" } ], "eprint_id": 4890, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/12121" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/12121" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/12121" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/48/90", "datestamp": "2003-12-12", "lastmod": "2020-03-10 23:02:07", "status_changed": "2009-09-25 03:27:53", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "gab@gps.caltech.edu", "id": "Blake-Geoffrey-A", "name": { "family": "Blake", "given": "Geoffrey A." }, "show_email": "NO" } ] }, "title": "On the Chemical Composition of Interstellar Molecular Clouds: A Millimeter and Submillimeter Spectral Line Survey of OMC-1", "ispublished": "unpub", "full_text_status": "public", "keywords": "Chemistry", "abstract": "The same basic principles govern the chemical and physical evolution of systems throughout the universe. However, the dissimilar conditions on the Earth and in the interstellar medium lead to remarkably different chemical compositions for these two environments. While less familiar than terrestrial chemistry, the study of the chemical composition of the interstellar medium is important because it bears directly on the understanding of phenomena as diverse as star formation, galactic structure and dynamics, and the cosmological origin of the universe, in addition to providing a unique opportunity to investigate a number of fundamental chemical and physical processes.
\r\n\r\nWe present here results from a millimeter and submillimeter spectral line survey of the core of the Orion molecular cloud (OMC-1). The millimeter-wave survey, conducted at the Owens Valley Radio Observatory (OVRO), covers a 55 GHz interval in the 1.3 mm (230 GHz) atmospheric window and contains emission from 29 molecules. Together with the frequency selective submillimeter observations of H2D+ (372.4 GHz), Cl (492.2 GHz), NH3 (572.5 GHz), and HCl (625.9 GHz) performed aboard NASA's Kuiper Airborne Observatory, over 800 emission lines have been detected from 33 chemically distinct species during the course of this work. The uniformly calibrated results from the unique and extensive OVRO spectral line survey place significant constraints on models of interstellar chemistry, and have allowed the chemical composition of the various regions in OMC-1 to be definitively characterized.
\r\n\r\nA global analysis of the observed abundances has shown that the markedly different chemical compositions of the kinematically distinct Orion subsources may be simply interpreted in the framework of an evolving, initially quiescent, gas-phase chemistry influenced by the process of massive star formation. The chemical composition of the extended Orion cloud complex is similar to that found in a number of other objects, but the central regions of OMC-1 have had their chemistry selectively altered by the high velocity outflow from the young star(s) embedded deep within the interior of the molecular cloud. Detailed arguments are presented in this thesis which relate the seemingly disparate chemical compositions of the individual regions to each other and to the expected physical manifestations of the circumstellar mass loss, and which suggest that similar mechanisms may operate in other molecular clouds as well.
\r\n\r\nBy performing supporting laboratory spectroscopy to supplement existing millimeter-wave catalogues only 33 of the over 800 lines remain unidentified, in contradiction to earlier expectations which had predicted that the near millimeter-wave spectrum of molecular clouds would contain hundreds of strong, unidentifiable emission features. It is probable that a number of the unidentified lines left in the OVRO survey are due to transitions between states of either isotopically substituted or highly excited abundant and complex molecules such as CH3OH, CH3OCH3, and HCOOCH3 whose rotational spectra are poorly known at present. The very small percentage and weak strength of the unidentified lines implies that the dominant chemical constituents visible at millimeter wavelengths have been identified in the Orion molecular cloud.
\r\n\r\nAlso presented are high resolution laboratory millimeter, submillimeter, and far-infrared absorption spectra of the transient molecular species OH, CN, HOC+, and HCO, The zero-field pure rotational spectrum of the OH radical was observed, for the first time, with a frequency agile far-infrared laser sideband spectrometer which promises to revolutionize high resolution spectroscopy at submillimeter and far-infrared wavelengths, while the HOC+ molecular ion was synthesized in a novel glow discharge cell that increases ion abundances by roughly two orders of magnitude as compared with those produced by previously reported methods. Studies of several ions produced in the new discharge cell have provided a theory of the mechanism responsible for the ion enhancement. Sixty-five transitions of CN in its first four vibrational states have been observed, allowing a detailed examination of vibrational and electronic effects in this astrophysically important free radical. The investigation of HCO is the first extensive zero-field analysis of the formyl radical, and is one of the very few millimeter and submillimeter laboratory studies of a non-linear free radical performed to date.
", "date": "1986", "date_type": "degree", "id_number": "CaltechETD:etd-12092003-145807", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-12092003-145807", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-12-12", "doi": "10.7907/0F73-PJ76", "divisions": { "items": [ "div_chem" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" }, { "id": "Pickett-Herbert-M", "name": { "family": "Pickett", "given": "Herbert M." } } ] }, "thesis_committee": { "items": [ { "email": "mckoy@caltech.edu", "id": "McKoy-B-V", "name": { "family": "McKoy", "given": "Basil Vincent" }, "role": "chair" }, { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "member" }, { "id": "Pickett-H-M", "name": { "family": "Pickett", "given": "Herbert M." }, "role": "member" }, { "email": "wag@caltech.edu", "id": "Goddard-W-A-III", "name": { "family": "Goddard", "given": "William A., III" }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-12-09", "thesis_defense_date": "1985-07-02", "thesis_approved_date": "2003-12-12", "review_status": "approved", "option_major": { "items": [ "chemistry" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1986", "author_list": "Blake, Geoffrey A." }, { "id": "/id/eprint/3434", "eprint_id": 3434, "rev_number": 21, "documents": [ { "id": "/id/document/5969", "doc_id": 5969, "rev_number": 3, "files": [ { "id": "/id/file/35553", "fileid": 35553, "datasetid": "document", "objectid": 5969, "filename": "Hough_dh_1986.pdf", "mime_type": "application/pdf", "filesize": 5668667, "mtime": "2012-12-26 02:59:53", "url": "/3434/1/Hough_dh_1986.pdf" } ], "eprint_id": 3434, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Hough_dh_1986.pdf", "language": "en", "security": "public", "license": "other", "main": "Hough_dh_1986.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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accessible to very-long-baseline interferometry (VLSI). The purpose of defining the sample in this way is to facilitate tests of physical models proposed to explain both the compact and extended structures in extragalactic radio sources. Statistical studies of the properties of these objects on the >~ kiloparsec scale are consistent with the assumption of random orientations and the simple relativistic beaming theory.
\r\n\r\nThe central components of six double-lobed quasars have been mapped at high resolution and high sensitivity with VLBI. Each object exhibits a double or extended structure on the the ~parsec scale. This structure can be interpreted as a \"core-jet,\" the same morphology found in the dominant cores of powerful flat-spectrum sources, thus indicating a relation between the two classes of compact radio source. The presumed VLBI jets are all fairly well aligned with >~kiloparsec-scale, one-sided jets. The fact that the VLBI and large-scale jets always lie on the same side of the compact core suggests the same cause for the asymmetric structure on both scales.
\r\n\r\nThe central components of 3C245 and 3C263 have been mapped at three epochs. We find superluminal expansion in 3C263 with an apparent velocity of ~1.5c, and argue that there is evidence that 3C245 will also be found to be superluminal. These results are consistent with the simple beaming theory. It is thus clear that we will be able to measure component motion in many of these objects, which will permit us to distinguish among alternative theories of parsec-scale structure and motion.
\r\n\r\nThe future study of these compact central components will benefit greatly from the increased resolution afforded by both higher frequency, ground-based VLBI and VLBI using a radio telescope in Earth orbit.
\r\n", "date": "1986", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-091002", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-091002", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" }, { "agency": "NSF" }, { "agency": "Max-Planck-Gesellschaft" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-16", "doi": "10.7907/8P47-SM58", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "chair" }, { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1986-03-31", "thesis_approved_date": "2008-09-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1986", "author_list": "Hough, David Hans" }, { "id": "/id/eprint/3447", "eprint_id": 3447, "rev_number": 12, "documents": [ { "id": "/id/document/5982", "doc_id": 5982, "rev_number": 3, "files": [ { "id": "/id/file/35650", "fileid": 35650, "datasetid": "document", "objectid": 5982, "filename": "Rich_rm_1986.pdf", "mime_type": "application/pdf", "filesize": 20880490, "mtime": "2012-12-26 02:59:58", "url": "/3447/1/Rich_rm_1986.pdf" } ], "eprint_id": 3447, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Rich_rm_1986.pdf", "language": "en", "security": "public", "license": "other", "main": "Rich_rm_1986.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22522" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22522" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22522" } ] } }, { "id": "/id/document/22522", "doc_id": 22522, "rev_number": 3, "files": [ { "id": "/id/file/35648", "fileid": 35648, "datasetid": "document", "objectid": 22522, "filename": "preview.png", "mime_type": "image/png", "hash": "3b03c0151a9fdc733f885b1eb179d13f", "hash_type": "MD5", "filesize": 9636, "mtime": "2012-12-26 02:59:58", "url": "/3447/2/preview.png" } ], "eprint_id": 3447, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5982" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5982" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5982" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/47", "datestamp": "2008-09-18", "lastmod": "2021-04-16 22:30:43", "status_changed": "2009-09-25 02:58:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rich-Robert-Michael", "name": { "family": "Rich", "given": "Robert Michael" }, "show_email": "NO" } ] }, "title": "Abundances and Kinematics of K Giants in the Galactic Nuclear Bulge", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Spectroscopy and photometry has been obtained for 100 K giants in Baade's Window at l = 1\u00b0, b = -4\u00b0. For a galactocentric distance 7.5 kpc the line of sight passes 522 pc below the nucleus. The abundance distribution of the nuclear bulge K giants has been derived relative to 45 stars of known abundance. The abundances run from -1 to nearly +1 dex, with a peak at 0.3 dex, or twice the solar abundance. Of the 88 stars with derived abundances, 22% exceeded the abundance of the most metal rich local K giants; 50% exceeded the solar abundance, and 10% were metal poor (< -0.6 dex).
\r\n\r\nRadial velocities have been measured for 53 nuclear bulge K giants which also have derived abundances. Their velocity dispersion is 104 km/sec. The mean velocity is -19 \u00b1 14 km/sec; within 1\u03c3 of the solar II velocity of -10 km/sec. When this sample is divided into 3 subsets based on the abundances, the subset of 21 stars > 0.3 dex has \u03c3 = 92 \u00b1 14 km/sec and the metal poor subset of 16 stars < -0.3 dex has \u03c3 = 126 \u00b1 22 km/sec. An intermediate set of 16 stars has \u03c3 = 97 \u00b1 17 km/sec. The most metal rich stars may have a bulk velocity of -38 \u00b1 14 km/sec, 1\u03c3 less than the -19 km/sec of the metal poor stars.
\r\n\r\nThe abundance distribution function is found to be fit very well by the simple model of chemical evolution with complete gas consumption.
\r\n\r\nThe smaller velocity dispersion for the metal rich stars can be interpreted as supporting a steep power law for their spatial distribution \u03c1 ~ r-7. The metal rich stars may belong to a special central component of the Galaxy, which cuts off completely at 1kpc.
\r\n\r\nNo evidence was found that either the metal rich or metal poor stars follow the galactic rotation curve; hence neither population appears to be rotation supported.
\r\n\r\nOptical and infrared photometry is presented for nuclear bulge K giants. The colors of these stars are shown to be too hot for their derived metal abundances.
\r\n\r\nAnalysis of color-magnitude diagrams in bulge fields at -4\u00b0 (Baade's Window) and -8\u00b0 shows that there cannot be a 1 Gyr old population of main sequence stars in the galactic bulge. A turnoff population is detected at -8\u00b0, and comparison with isochrones indicates that the population is older than 5 Gyr. For the first time, there is a clear indication of a horizontal branch, or \"globular cluster feature\" in the luminosity function of the galactic bulge.
\r\n", "date": "1986", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-152942", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-152942", "related_url": { "items": [ { "description": "Article adapted for Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/161484" }, { "description": "Article adapted for Appendix 1.", "type": "doi", "url": "https://doi.org/10.1086/113654" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-18", "doi": "10.7907/zyq4-ta43", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "chair" }, { "email": "esp@tapir.caltech.edu", "id": "Phinney-E-S", "name": { "family": "Phinney", "given": "E. Sterl" }, "role": "member" }, { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1986-04-17", "thesis_approved_date": "2008-09-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1986", "author_list": "Rich, Robert Michael" }, { "id": "/id/eprint/3406", "eprint_id": 3406, "rev_number": 13, "documents": [ { "id": "/id/document/5941", "doc_id": 5941, "rev_number": 3, "files": [ { "id": "/id/file/35342", "fileid": 35342, "datasetid": "document", "objectid": 5941, "filename": "Biretta_ja_1986.pdf", "mime_type": "application/pdf", "filesize": 5046156, "mtime": "2012-12-26 02:59:42", "url": "/3406/1/Biretta_ja_1986.pdf" } ], "eprint_id": 3406, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Biretta_ja_1986.pdf", "language": "en", "security": "public", "license": "other", "main": "Biretta_ja_1986.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22481" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22481" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22481" } ] } }, { "id": "/id/document/22481", "doc_id": 22481, "rev_number": 3, "files": [ { "id": "/id/file/35340", "fileid": 35340, "datasetid": "document", "objectid": 22481, "filename": "preview.png", "mime_type": "image/png", "hash": "9776d666048e8af5af5a8d41a1df19a3", "hash_type": "MD5", "filesize": 8082, "mtime": "2012-12-26 02:59:42", "url": "/3406/2/preview.png" } ], "eprint_id": 3406, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5941" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5941" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5941" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/06", "datestamp": "2008-09-17", "lastmod": "2021-04-19 22:28:26", "status_changed": "2009-09-25 02:57:56", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Biretta-John-Anthony", "name": { "family": "Biretta", "given": "John Anthony" }, "show_email": "NO" } ] }, "title": "Investigations of Radio Jets in M87, 3C273, and 3C345", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "We present observational studies of extra-galactic radio jets in M87, 3C273, and 3C345.
\r\n\r\nObservations of the M87 jet were made at 15 GHz with 0.12\" resolution. All of the knots are clearly resolved both along and across the jet. Most of the knots are found to be smooth in appearance with no evidence of shocklike discontinuities. The brightest knot and the innermost knot are exceptions to this. The brightest knot (knot A) seems consistent with a shock caused by unsteady flow in the jet. Models for this feature are discussed. Combining our data with X-ray data suggests that the jet is neither freely expanding, thermally confined, nor ram pressure confined. The jet may, however, be magnetically confined.
\r\n\r\nWe present 10.7 GHz VLBI observations of 3C273 with high north-south resolution. A strong, non-monotonic curvature is found in the jet at projected radii \u2264 5 pc. It is unlikely that this curvature can be caused by precession. Measurements of the core size show that bulk relativistic motion in the core is not required for consistency with the observed x-ray flux.
\r\n\r\nFor 3C345 we present a systematic analysis of VLBI observations at 2.3, 5.0, 10.7, 22.2, and 89 GHz. Epochs are from 1979.25 through 1984.11. A newly ejected superluminal component (C4) is observed to accelerate, change position angle, undergo a large flux outburst, and have a flat spectrum. Older components C2 and C3 have different speeds, different position angles, and show little or no acceleration. The spectrum of C3 steepens as its flux decays. There are spectral index gradients such that both C4 and C3 are farther from the \"core\" at higher frequencies. The moving components define an opening angle of ~27\u00b0 and also show direct evidence for expansion. The counter-jet to jet flux ratio is extremely small, -0.007\u00b10.007.
\r\n\r\nThese data for 3C345 are interpreted in terms of simple models involving spherical components or shocks in a relativistic jet. All of the emission regions show evidence for bulk relativistic motion with \u03b4 > 3. The particle energies and pressures dominate those of the magnetic fields, unless \u03b4 \u2265 20. If the emission regions consist of an electron-proton plasma, then the density of thermal electrons is much less than the density of relativistic electrons. The fluxes decay with time much more rapidly than the synchrotron half-life, but much more slowly than predicted by adiabatic expansion. An attractive model for the observed kinematics identifies the emitting regions as shocks in an apparently broad and curved jet; a curvature of \u2265 3\u00b0 and \u03b3 \u2265 10 is required.
\r\n", "date": "1986", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-084712", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-084712", "related_url": { "items": [ { "description": "Article adapted for Chapter I.", "type": "doi", "url": "https://doi.org/10.1086/184144" }, { "description": "Article adapted for Chapter II.", "type": "doi", "url": "https://doi.org/10.1086/184462" }, { "description": "Article adapted for Chapter III.", "type": "doi", "url": "https://doi.org/10.1038/306042a0" }, { "description": "Article adapted for Chapter IV.", "type": "doi", "url": "https://doi.org/10.1086/164481" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-17", "doi": "10.7907/dsst-qp22", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1985-06-06", "thesis_approved_date": "2008-09-17", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1986", "author_list": "Biretta, John Anthony" }, { "id": "/id/eprint/3395", "eprint_id": 3395, "rev_number": 20, "documents": [ { "id": "/id/document/5925", "doc_id": 5925, "rev_number": 3, "files": [ { "id": "/id/file/35247", "fileid": 35247, "datasetid": "document", "objectid": 5925, "filename": "Fillmore_ja_1985.pdf", "mime_type": "application/pdf", "filesize": 3975765, "mtime": "2012-12-26 02:59:36", "url": "/3395/1/Fillmore_ja_1985.pdf" } ], "eprint_id": 3395, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Fillmore_ja_1985.pdf", "language": "en", "security": "public", "license": "other", "main": "Fillmore_ja_1985.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22465" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22465" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22465" } ] } }, { "id": "/id/document/22465", "doc_id": 22465, "rev_number": 3, "files": [ { "id": "/id/file/35245", "fileid": 35245, "datasetid": "document", "objectid": 22465, "filename": "preview.png", "mime_type": "image/png", "hash": "143367dc6cf063478c1b2ba44e062dfb", "hash_type": "MD5", "filesize": 8713, "mtime": "2012-12-26 02:59:35", "url": "/3395/2/preview.png" } ], "eprint_id": 3395, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5925" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5925" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5925" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/95", "datestamp": "2008-09-12", "lastmod": "2021-04-16 22:11:34", "status_changed": "2009-09-25 02:57:45", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fillmore-James-Arthur", "name": { "family": "Fillmore", "given": "James Arthur" }, "show_email": "NO" } ] }, "title": "A Study on the Formation and Dynamics of Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "The first half of this thesis is a study on the growth of perturbations in the early universe which might lead to galaxies, clusters of galaxies, or regions void of galaxies.
\r\n\r\nThe growth of self-similar perturbations in an Einstein-deSitter universe with cold, collisionless particles is investigated. Three classes of solutions are obtained; one each with planar, cylindrical, and spherical symmetry. The solutions follow the development of structure in both the linear and nonlinear regimes.
\r\n\r\nSelf-similar spherical voids which develop from initially underdense regions are also investigated. The character of each solution depends upon the initial density deficit. Steep perturbations result in voids bounded by overdense shells with sharp edges.
\r\n\r\nThe second half of this thesis details solutions of steady-state axisymmetric models of elliptical and disk galaxies, and considers which observable properties can be used as diagnostics of the kinematic configuration of the spheroidal component of these systems.
\r\n\r\nTwo component mass models are fitted to surface brightness measurements and used to fit kinematic models to the velocity data. The models with constant mass-to-light ratios and isotropic velocity dispersions adequately fit the inner regions of spiral galaxies with three caveats:
\r\n\r\n(i) Several galaxies show significant differences between the two sides of the major axis in both their rotation rate and velocity dispersion. While the differences might be caused by non-axisymmetric potentials, variations in the line-of-sight extinction are a more likely cause.
\r\n\r\n(ii) The inner segment (R \u2264 1 kpc) of the emission line (gas) rotation curve falls below the predicted circular velocity derived from the stellar velocities. We rule out a variation in the mass-to-light ratio as a cause for this discrepancy because M/L would have to significantly decrease at small radii; this trend is opposite to typical expectations of M/L. Significant emission from gas produced by stellar mass loss, particularly planetary nebulae, which is not yet settled into the disk might explain this observation.
\r\n\r\n(iii) Some of the bulges are flatter than one would expect from their rotation rate assuming isotropic random motions, but this additional flattening could be caused by the disk potential.
\r\n\r\nSelf-consistent solutions of the stellar hydrodynamic equations for systems with isodensity surfaces which are concentric oblate spheroids and have constant mass-to-light ratios are presented. Various kinematic configurations are constructed to develop observational diagnostics which can distinguish these configurations. Because the inclination and true flattening of each elliptical is indeterminable, several kinematically distinct configurations are indistinguishable. Observations can uniquely characterize only those galaxies which lie at certain kinematic extremes.
\r\n", "date": "1985", "date_type": "degree", "id_number": "CaltechETD:etd-09082008-150750", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082008-150750", "related_url": { "items": [ { "description": "Article adapted for Chapter One.", "type": "doi", "url": "https://doi.org/10.1086/162070" }, { "description": "Article adapted for Chapter Two.", "type": "doi", "url": "https://doi.org/10.1086/162071" }, { "description": "Article adapted for Chapter Three.", "type": "doi", "url": "https://doi.org/10.1086/163984" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "ARCS Foundation" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/b70x-qk59", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-08", "thesis_defense_date": "1985-05-09", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1985", "author_list": "Fillmore, James Arthur" }, { "id": "/id/eprint/10414", "eprint_id": 10414, "rev_number": 32, "documents": [ { "id": "/id/document/82468", "doc_id": 82468, "rev_number": 3, "files": [ { "id": "/id/file/233072", "fileid": 233072, "datasetid": "document", "objectid": 82468, "filename": "Schumaker_BL_1985.pdf", "mime_type": "application/pdf", "hash": "3f691de10a5a8598f3b7565791f4e6a6", "hash_type": "MD5", "filesize": 82746632, "mtime": "2017-09-06 22:18:31", "url": "/10414/8/Schumaker_BL_1985.pdf" } ], "eprint_id": 10414, "pos": 8, "placement": 8, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Schumaker_BL_1985.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/82468" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/01/04/14", "datestamp": "2017-09-06 22:33:03", "lastmod": "2021-04-16 23:25:25", "status_changed": "2017-09-06 22:33:03", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schumaker-Bonny-Laura", "name": { "family": "Schumaker", "given": "Bonny Laura" }, "show_email": "NO" } ] }, "title": "Theoretical Investigations in Nonlinear Quantum Optics, Theory of Measurement, and Pulsations of General Relativistic Models of Neutron Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis is a collection of six papers. The first four constitute the heart of the thesis; they are concerned with quantum mechanical properties of certain harmonic-oscillator states. The first paper is a discourse on single-mode and two-mode Gaussian pure states (GPS), states produced when harmonic oscillators in their ground states are exposed to potentials that are linear or quadratic in oscillator position and moment um variables (creation and annihilation operators). The second and third papers develop a formalism for analyzing two-photon devices (e.g., parametric amplifiers and phase-conjugate mirrors), in which photons in the ouput modes arise from two-photon transitions, i.e., are created or destroyed two at a time. The states produced by such devices are single-mode and two-mode \"squeezed states\", special kinds of GPS whose low-noise properties make them attractive for applications in such fields as optical communications and gravitational wave detection. The fourth paper is an analysis of the noise in homodyne detection, a phase-sensitive detection scheme in which the special properties of (single-mode) squeezed states are revealed as an improved signal-to-noise ratio relative to that obtained with coherent states (the states produced, e.g., by a laser).
\r\n\r\nThe fifth and sixth papers deal with problems of a different nature from that of the previous papers. The fifth paper considers the validity of the \"standard quantum limit\" (SQL) for measurements which monitor the posi\u00adtion of a free mass. It shows specifically that when the pre-measurement wave functions of the free mass and the measuring apparatus(es) are Gaus\u00adsian (in the general sense, which includes so-called \"contractive states\"), measurements described by linear couplings to the position or to both the position and momentum are limited by the SQL. The sixth paper develops the mathematical theory of torsional (toroidal) oscillations in fully general relativistic, nonrotating, spherical stellar models, and of the gravitational waves they emit.
", "date": "1985", "date_type": "degree", "id_number": "CaltechTHESIS:09062017-132307035", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09062017-132307035", "related_url": { "items": [ { "description": "Article adapted for Part One: 2.", "type": "doi", "url": "https://doi.org/10.1103/physreva.31.3068" }, { "description": "Article adapted for Part One: 3.", "type": "doi", "url": "https://doi.org/10.1103/physreva.31.3093" }, { "description": "Article adapted for Part One: 4.", "type": "doi", "url": "https://doi.org/10.1364/ol.9.000189" }, { "description": "Article adapted for Part Three.", "type": "doi", "url": "https://doi.org/10.1093/mnras/203.2.457" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-09-06 22:33:03", "doi": "10.7907/fwvz-7t26", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "id": "Whitcomb-S-E", "name": { "family": "Whitcomb", "given": "Stanley E." }, "role": "member" }, { "id": "Caves-C", "name": { "family": "Caves", "given": "Carlton" }, "role": "member" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1985-05-15", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1985", "author_list": "Schumaker, Bonny Laura" }, { "id": "/id/eprint/3328", "eprint_id": 3328, "rev_number": 14, "documents": [ { "id": "/id/document/5848", "doc_id": 5848, "rev_number": 3, "files": [ { "id": "/id/file/34706", "fileid": 34706, "datasetid": "document", "objectid": 5848, "filename": "Sahai_r_1985.pdf", "mime_type": "application/pdf", "filesize": 3296227, "mtime": "2012-12-26 02:59:06", "url": "/3328/1/Sahai_r_1985.pdf" } ], "eprint_id": 3328, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Sahai_r_1985.pdf", "language": "en", "security": "public", "license": "other", "main": "Sahai_r_1985.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22389" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22389" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22389" } ] } }, { "id": "/id/document/22389", "doc_id": 22389, "rev_number": 3, "files": [ { "id": "/id/file/34704", "fileid": 34704, "datasetid": "document", "objectid": 22389, "filename": "preview.png", "mime_type": "image/png", "hash": "3478b57fb332e2707f5d3df137ab0b01", "hash_type": "MD5", "filesize": 9132, "mtime": "2012-12-26 02:59:06", "url": "/3328/2/preview.png" } ], "eprint_id": 3328, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5848" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5848" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5848" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/28", "datestamp": "2008-09-10", "lastmod": "2021-04-16 23:11:07", "status_changed": "2009-09-25 02:56:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sahai-Raghvendra", "name": { "family": "Sahai", "given": "Raghvendra" }, "show_email": "NO" } ] }, "title": "Circumstellar Shells of Late-Type Stars -- A Study at Millimeter and Infrared Wavelenghts", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "This thesis describes an investigation of the physical conditions and molecular abundances in mass-loss envelopes around late-type stars based on millimeter and near infrared spectroscopy, concentrating on the high mass loss, carbon-rich star IRC +10216.
\r\n\r\nThe first part of this thesis is a multi-transition study of the rotational spectrum of SiS from the IRC +10216 envelope. The observational results are described in Chapter 2. A general numerical model to calculate the excitation and radiative transfer for rotation and vibration-rotation lines in circumstellar envelopes is developed in Chapter 3.
\r\n\r\nApplying this model to fit the observed SiS lines from IRC +10216 (Chapter 4), we find that the undissociated abundance [SiS]/[H2] in the shielded inner regions of the circumstellar shell is ~2.4 x 10-7, roughly a factor of 100 smaller than that predicted previously by chemical models. The SiS density falls steeply with radius, reaching one-half the undissociated abundance at r = 9 x 1016 cms. We show that a) Si, not S depletion is responsible for the low SiS abundance, and b) most of the available Si has probably been used up in forming SiC grains in the cool IRC +10216 atmosphere.
\r\n\r\nVariations in the 13 \u00b5m infrared flux over the 644 day light-cycle of IRC +10216 produce observable changes in some of the SiS lines. Sharp cusps in the J = 5-4 line wings, observed with the Onsala 20 m antenna, are explained in terms of weak maser emission at maximum light. The model predicts a different shape for this line at minimum light, in excellent agreement with a recent Onsala observation. Line coincidences, involving 13 \u00b5m transitions of HCN and C2H2 (not considered in the model), may be responsible for poor fits to some of the SiS rotational spectrum.
\r\n\r\nA sensitive search for SiS J = 7-6 and J = 6-5 lines in other carbon-rich, oxygen-rich, and S-type circumstellar shells was also conducted (Chapter 2). Three new SiS sources, CIT 6, CRL 2688 and IRC +20370, all of which are carbon-rich were detected, in agreement with the chemical equilibrium models predicting SiS to be significantly more abundant in a carbon-rich environment than in an oxygen-rich environment.
\r\n\r\nThe second part of the thesis (Chapters 5 and 6) deals with the investigation of physical conditions in the inner (r ~ 2\") envelope of IRC +10216 -- a scale size that has never been observed previously. We have devised a new observational technique, employing an annular aperture (size 2 - 3.45\") to measure extended emission from resonant-scattered photons in the 4.6 \u00b5m CO vibration-rotation band from IRC +10216. In addition to the expected emission up to the expansion velocity of the envelope, both CO and 13CO show evidence of high velocity features in the blue wing of the line, beyond the 15 km s-1 expansion velocity (Chapter 5).
\r\n\r\nIn order to derive physical quantities from the many P and R branch lines present in the infrared spectra, we develop an analytical model to calculate the excitation of these lines due to radiative pumping by thermal emission from circumstellar dust (Chapter 6). The lines are optically thick, and trapping of line radiation has been included. The model emission intensity is found to vary in a simple manner with radius, velocity, J value of the lower state, and the kinetic temperature (which we expect characterises the populations of the V = 0 rotational levels). Our model shows the V = 1 rotational level populations to be in equilibrium with the kinetic temperature despite being excited by infrared radiation.
\r\n\r\nWe derive the following results for the IRC +10216 inner envelope:
\r\n\r\ni) The kinetic temperature at radius r = 2\" is ~ 244 K, roughly twice the extrapolation of the Kwan and Hill (1977) thermodynamic model. This measurement forces revision of analyses of infrared absorption lines in which the radial information was derived assuming a temperature profile (known a priori).
\r\n\r\nii) The gas density in the inner regions of the envelope is characterised by a minimum mass loss rate of
\r\n\r\n[Equation; see abstract in scanned thesis for details].
\r\n", "date": "1985", "date_type": "degree", "id_number": "CaltechETD:etd-09042008-105047", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09042008-105047", "related_url": { "items": [ { "description": "Article adapted for Chapters 2 and 4.", "type": "doi", "url": "https://doi.org/10.1086/162394" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/yfv7-n741", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "member" }, { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "member" }, { "id": "Wannier-P-G", "name": { "family": "Wannier", "given": "Peter G." }, "role": "member" }, { "email": "nzs@astro.caltech.edu", "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-04", "thesis_defense_date": "1984-09-25", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"userid": 87, "dir": "disk0/00/00/85/53", "datestamp": "2014-07-18 14:29:03", "lastmod": "2022-11-09 19:20:06", "status_changed": "2014-07-18 14:29:03", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brown-Elliott-R", "name": { "family": "Brown", "given": "Elliott R." }, "show_email": "NO" } ] }, "title": "Investigation of Bulk Indium Antimonide as Heterodyne Detector for the Submillimeter Wavelength Region", "ispublished": "unpub", "full_text_status": "public", "keywords": "Applied Physics, Indium antimonide ", "abstract": "Bulk n-InSb is investigated at a heterodyne detector for the submillimeter wavelength region. Two modes of operation are investigated: (1) the Rollin or hot electron bolometer mode (zero magnetic field), and (2) the Putley mode (quantizing magnetic field). The highlight of the thesis work is the pioneering demonstration or the Putley mode mixer at several frequencies. For example, a double-sideband system noise temperature of about 510K was obtained using a 812 GHz methanol laser for the local oscillator. This performance is at least a factor or 10 more sensitive than any other performance reported to date at the same frequency. In addition, the Putley mode mixer achieved system noise temperatures of 250K at 492 GHz and 350K at 625 GHz. The 492 GHz performance is about 50% better and the 625 GHz is about 100% better than previous best performances established by the Rollin-mode mixer. To achieve these results, it was necessary to design a totally new ultra-low noise, room-temperature preamp to handle the higher source impedance imposed by the Putley mode operation. This preamp has considerably less input capacitance than comparably noisy, ambient designs.
\r\n\r\nIn addition to advancing receiver technology, this thesis also presents several novel results regarding the physics of n-InSb at low temperatures. A Fourier transform spectrometer was constructed and used to measure the submillimeter wave absorption coefficient of relatively pure material at liquid helium temperatures and in zero magnetic field. Below 4.2K, the absorption coefficient was found to decrease with frequency much faster than predicted by Drudian theory. Much better agreement with experiment was obtained using a quantum theory based on inverse-Bremmstrahlung in a solid. Also the noise of the Rollin-mode detector at 4.2K was accurately measured and compared with theory. The power spectrum is found to be well fit by a recent theory of non-equilibrium noise due to Mather. Surprisingly, when biased for optimum detector performance, high purity InSb cooled to liquid helium temperatures generates less noise than that predicted by simple non-equilibrium Johnson noise theory alone. This explains in part the excellent performance of the Rollin-mode detector in the millimeter wavelength region.
\r\n\r\nAgain using the Fourier transform spectrometer, spectra are obtained of the responsivity and direct detection NEP as a function of magnetic field in the range 20-110 cm-1. The results show a discernable peak in the detector response at the conduction electron cyclotron resonance frequency for magnetic fields as low as 3 KG at bath temperatures of 2.0K. The spectra also display the well-known peak due to the cyclotron resonance of electrons bound to impurity states. The magnitude of responsivity at both peaks is roughly constant with magnet1c field and is comparable to the low frequency Rollin-mode response. The NEP at the peaks is found to be much better than previous values at the same frequency and comparable to the best long wavelength results previously reported. For example, a value NEP = 4.5 x 10-13W/Hz1/2 is measured at 4.2K, 6 KG and 40 cm-1. Study of the responsivity under conditions of impact ionization showed a dramatic disappearance of the impurity electron resonance while the conduction electron resonance remained constant. This observation offers the first concrete evidence that the mobility of an electron in the N = 0 and N = 1 Landau levels is different. Finally, these direct detection experiments indicate that the excellent heterodyne performance achieved at 812 GHz should be attainable up to frequencies of at least 1200 GHz.
", "date": "1985", "date_type": "degree", "id_number": "CaltechTHESIS:07172014-130847340", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:07172014-130847340", "related_url": { "items": [ { "description": "Article adapted for part of thesis.", "type": "doi", "url": "https://doi.org/10.1063/1.332867" }, { "description": "Article adapted for part of thesis.", "type": "doi", "url": "https://doi.org/10.1063/1.334344" }, { "description": "Article adapted for part of thesis.", "type": "doi", "url": "https://doi.org/10.1063/1.335989" }, { "description": "Article adapted for part of thesis.", "type": "doi", "url": "https://doi.org/10.1049/el:19850296" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2014-07-18 14:29:03", "doi": "10.7907/wm40-4k69", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "email": "ayariv@caltech.edu", "id": "Yariv-A", "name": { "family": "Yariv", "given": "Amnon" }, "role": "member" }, { "email": "rutledge@caltech.edu", "id": "Rutledge-D-B", "name": { "family": "Rutledge", "given": "David B." }, "role": "member" }, { "email": "pbellan@caltech.edu", "id": "Bellan-P-M", "name": { "family": "Bellan", "given": "Paul Murray" }, "role": "member" }, { "email": "wlj@caltech.edu", "id": "Johnson-W-L", "name": { "family": "Johnson", "given": "William Lewis" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1985-05-06", "review_status": "approved", "option_major": { "items": [ "appliedphys" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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"userid": 87, "dir": "disk0/00/01/04/08", "datestamp": "2017-09-01 19:35:43", "lastmod": "2021-04-16 23:08:26", "status_changed": "2017-09-01 19:35:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Suen-Wai-Mo", "name": { "family": "Suen", "given": "Wai Mo" }, "show_email": "NO" } ] }, "title": "Dynamical Electromagnetic Fields Near Black Holes and Multipole Moments of Stationary, General Relativistic Systems", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This dissertation contains two works; one of the behavior of dynamical electromagnetic fields in the stationary spacetime generated by a black hole, and the other on the structure of a general stationary vacuum spacetime itself.
\r\n\r\nThe study of electromagnetic field is carried out in terms of the \"membrane formalism\" for black holes; and it is part of a series of papers with the aim of developing that formalism into a complete, self-consistent description of electromagnetic and gravitational fields in a black hole background. Various model problems are presented as aids in understanding the interactions of electromagnetic fields with a black hole, and special attention is paid to the concept of the \"stretched horizon\" which is vital for the membrane formalism.
\r\n\r\nThe second work develops a multipole moment formalism for a general stationary system in general relativity. The multipole moments are defined in terms of a general formal series solution of the stationary Einstein equation, in analogy to multipole moments in the Newtonian theory of gravity. These relativistic moments exhibit many desirable properties and are shown to be useful in studying the interactions between a gravitating body and an external gravitational field. A model calculation applying the formalism to a black hole interacting with an external multipole field shows that the interaction can be understood in terms of \"elastic moduli\" of the black-hole horizon.
", "date": "1985", "date_type": "degree", "id_number": "CaltechTHESIS:09012017-090944275", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09012017-090944275", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST82-14126" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-09-01 19:35:43", "doi": "10.7907/xayq-7806", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "jhs@theory.caltech.edu", "id": "Schwarz-J-H", "name": { "family": "Schwarz", "given": "John H." }, "role": "member" }, { "email": "wise@theory.caltech.edu", "id": "Wise-M-B", "name": { "family": "Wise", "given": "Mark B." }, "role": "member" }, { "id": "Cowan-E-W", "name": { "family": "Cowan", "given": "Eugene W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1985-05-21", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1985", "author_list": "Suen, Wai Mo" }, { "id": "/id/eprint/3405", "eprint_id": 3405, "rev_number": 15, "documents": [ { "id": "/id/document/5940", "doc_id": 5940, "rev_number": 3, "files": [ { "id": "/id/file/35335", "fileid": 35335, "datasetid": "document", "objectid": 5940, "filename": "Filippenko_av_1984.pdf", "mime_type": "application/pdf", "filesize": 9870292, "mtime": "2012-12-26 02:59:42", "url": "/3405/1/Filippenko_av_1984.pdf" } ], "eprint_id": 3405, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Filippenko_av_1984.pdf", "language": "en", "security": "public", "license": "other", "main": "Filippenko_av_1984.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22480" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22480" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22480" } ] } }, { "id": "/id/document/22480", "doc_id": 22480, "rev_number": 3, "files": [ { "id": "/id/file/35333", "fileid": 35333, "datasetid": "document", "objectid": 22480, "filename": "preview.png", "mime_type": "image/png", "hash": "98a290d98718a3ddf3d03714ef5f8022", "hash_type": "MD5", "filesize": 8428, "mtime": "2012-12-26 02:59:42", "url": "/3405/2/preview.png" } ], "eprint_id": 3405, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5940" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5940" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5940" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/05", "datestamp": "2008-09-17", "lastmod": "2021-07-22 17:39:43", "status_changed": "2009-09-25 02:57:54", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Filippenko-Alexei-Vladimir", "name": { "family": "Filippenko", "given": "Alexei Vladimir" }, "orcid": "0000-0003-3460-0103", "show_email": "NO" } ] }, "title": "Physical Conditions in Low-Luminosity Active Galactic Nuclei", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Physical conditions in the nuclei of emission-line galaxies are investigated by analyzing their continua and optical emission lines.
\r\n\r\nThe strength and shape of the nonstellar continuum is derived for nine Seyfert galaxies. As in QSOs, it is described by a power law with slope ~ -1.1, and in the most luminous objects it flattens at blue and UV wavelengths. Even at minimum brightness it has no short-wavelength cutoff near 1 \u03bcm, eliminating the possibility that the near-infrared flux is dominated by thermal emission from hot dust grains.
\r\n\r\nA detailed analysis at optical and X-ray energies demonstrates that gas in the nucleus of NGC 7213 is photoionized by nonstellar radiation, even though it also exhibits the spectral characteristics of galaxies thought to be heated by shocks. After careful removal of the strong stellar component, it is shown how these \"shock\" features are actually more consistent with photoionization. The key is a large range of densities (~ 103-107cm-3) in the narrow-line clouds, and a fairly low ionization parameter.
\r\n\r\nSimilar studies of three additional galaxies confirm these results and strengthen the hypothesis that gas in LINERs (\"low ionization nuclear emission-line regions\") is photoionized rather than shock-heated. A tight correlation is found between the width of forbidden lines and their critical density. Moreover, much of the ionizing radiation is probably produced by a hot (T ~ 104-105 K) accretion disk.
\r\n\r\nA sensitive survey indicates that ~ 30-40% of LINERS exhibit weak, broad H\u03b1 emission. The emission-line intensity ratios are consistent with photoionization by a nonstellar continuum, indicating the presence of activity similar to (but much milder than) that of QSOs in a significant fraction of all nearby galaxies.
\r\n\r\nRelative intensities of emission lines in the narrow-line X-ray galaxy NGC 7314 are typical of type 2 Seyferts, but their widths (FWHM ~ 120-150 km s-1) are remarkably small. Thus, nonstellar radiation need not be associated with rapid motions among the narrow-line clouds. The profile of the broad H\u03b1 emission suggests that gas flows ballistically away from the nucleus. Dust, which heavily reddens radiation from broad-line clouds, is probably located within or near the clouds themselves.
\r\n", "date": "1984", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-083654", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-083654", "related_url": { "items": [ { "description": "Article adapted for Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/161549" }, { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/162521" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1086/162522" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1086/162909" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "https://doi.org/10.1086/191012" }, { "description": "Article adapted for Appendix 1.", "type": "doi", "url": "https://doi.org/10.1086/131052" }, { "description": "Article adapted for Appendix 2.", "type": "doi", "url": "https://doi.org/10.1086/131372" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Hertz Foundation" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department", "Caltech Distinguished Alumni Award" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-17", "doi": "10.7907/34v9-vc35", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "chair" }, { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "member" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1984-05-18", "thesis_approved_date": "2008-09-17", "thesis_awards": "Caltech Distinguished Alumni Award, 2017", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1984", "author_list": "Filippenko, Alexei Vladimir" }, { "id": "/id/eprint/10385", "eprint_id": 10385, "rev_number": 30, "documents": [ { "id": "/id/document/82158", "doc_id": 82158, "rev_number": 3, "files": [ { "id": "/id/file/231987", "fileid": 231987, "datasetid": "document", "objectid": 82158, "filename": "Redmount_ih_1984.pdf", "mime_type": "application/pdf", "hash": "da198e61a646238a7ee94f0dd0fa3ea9", "hash_type": "MD5", "filesize": 43405588, "mtime": "2017-08-23 18:03:27", "url": "/10385/2/Redmount_ih_1984.pdf" } ], "eprint_id": 10385, "pos": 2, "placement": 2, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Redmount_ih_1984.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": 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"content": "archival" }, { "id": "/id/document/133854", "doc_id": 133854, "rev_number": 1, "files": [ { "id": "/id/file/379299", "fileid": 379299, "datasetid": "document", "objectid": 133854, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "413f090f5eea4997dad943977bd84b74", "hash_type": "MD5", "filesize": 22260, "mtime": "2021-06-24 20:15:44", "url": "/10385/9/indexcodes.txt" } ], "eprint_id": 10385, "pos": 9, "placement": 9, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/82158" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/82158" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/82158" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/01/03/85", "datestamp": "2017-08-25 15:35:59", "lastmod": "2021-04-16 23:08:59", "status_changed": "2017-08-25 15:35:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Redmount-Ian-H", "name": { "family": "Redmount", "given": "Ian H." }, "show_email": "NO" } ] }, "title": "Topics in Black-Hole Physics: Geometric Constraints on Noncollapsing, Gravitating Systems and Tidal Distortions of a Schwarzschild Black Hole", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This dissertation consists of two studies on the general-relativistic theory of black holes. The first work concerns the fundamental issue of black-hole forma\u00adtion: in it I seek geometric constraints on gravitating matter systems, in the special case of axial symmetry, which determine whether or not those systems undergo gravitational collapse to form black holes. The second project deals with mechanical behavior of a black hole: specifically, I study the tidal deforma\u00adtion of a static black hole by the gravitational fields of external bodies.
\r\n\r\nIn the first paper I approach the problem of geometric constraints deter\u00admining gravitational collapse or non-collapse through the initial-value formalism of general relativity. I construct initial-value data representing noncollapsing, nonsingular, axisymmetric matter systems and examine the constraints imposed on this construction by the initial-value equation derived from the Ein\u00adstein field equations. The construction consists of a nonsingular, momentarily static interior geometry with nonnegative mass-energy density, matched smoothly to a static, vacuum exterior geometry (described by a Weyl solution of the Einstein field equations) at a boundary surface. The initial-value equation is found to impose restrictions on the choice of the boundary surface for such a system. Two such constraints are obtained here, appropriate to spherical and toroidal interior-region topologies. These constraints are studied by applying them to simple examples of Weyl exterior geometries. The \"hoop conjecture\" for the general geometric-constraints problem states that a system must collapse to a black hole unless its circumference in some direction exceeds a lower bound of the order of the system's mass. The examples examined here show, however, that the constraints derived in this study are not generally correlated with any simple measure of system size, and thus that they do not embody the hoop conjecture.
\r\n\r\nThe second paper examines the tidal distortion of a Schwarzschild black hole by bodies (\"moons\") suspended above the horizon on \"ropes.\" A solution of the Einstein field equations is constructed describing this configuration, using the Weyl formalism for axisymmetric, static, vacuum geometries. The intrinsic geometry of the tidally deformed black-hole horizon is obtained from this solu\u00adtion; I construct embedding diagrams to represent the shape of the horizon and the tidal bulges raised on it for both weak and strong perturbations. The rela\u00adtions among the masses of the hole and moons, the binding energy of the sys\u00adtem, and the rope density and tension are calculated from the solution and shown to be mutually consistent. Also, the Riemann curvature tensor represent\u00ading the tidal fields near the horizon is calculated. This solution is found to agree with a previous calculation by Hartle of black-hole tides, in the limit of perturb\u00ading moons far from the horizon. In the opposite case of moons very near the horizon, this solution approaches the static limit of the distorted horizon in Rindler space calculated by Suen and Price. The results of this study thus sup\u00adport the use of the Rindler approximation to Schwarzschild spacetime in calcu\u00adlating static black-hole tides, and its extension to dynamical situations.
", "date": "1984", "date_type": "degree", "id_number": "CaltechTHESIS:08232017-105535039", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08232017-105535039", "related_url": { "items": [ { "description": "Article adapted for Part One.", "type": "doi", "url": "https://doi.org/10.1103/physrevd.27.699" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Robert Andrews Millikan Fellowship" }, { "agency": "Caltech" }, { "agency": "J. S. Fluor Graduate Fellowship" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-25 15:35:59", "doi": "10.7907/mp3n-4r06", "alt_title": { "items": [ "Geometric Constraints on Noncollapsing, Gravitating Systems", "Tidal Distortions of a Schwarzschild Black Hole" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "scf@theory.caltech.edu", "id": "Frautschi-S-C", "name": { "family": "Frautschi", "given": "Steven C." }, "role": "chair" }, { "id": "Price-Richard-H", "name": { "family": "Price", "given": "Richard H." }, "role": "member" }, { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "member" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1983-09-23", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1984", "author_list": "Redmount, Ian H." }, { "id": "/id/eprint/3404", "eprint_id": 3404, "rev_number": 15, "documents": [ { "id": "/id/document/5939", "doc_id": 5939, "rev_number": 3, "files": [ { "id": "/id/file/35328", "fileid": 35328, "datasetid": "document", "objectid": 5939, "filename": "Lichten_sm_1984.pdf", "mime_type": "application/pdf", "filesize": 5636116, "mtime": "2012-12-26 02:59:41", "url": "/3404/1/Lichten_sm_1984.pdf" } ], "eprint_id": 3404, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Lichten_sm_1984.pdf", "language": "en", "security": "public", "license": "other", "main": "Lichten_sm_1984.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22479" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22479" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22479" } ] } }, { "id": "/id/document/22479", "doc_id": 22479, "rev_number": 3, "files": [ { "id": "/id/file/35326", "fileid": 35326, "datasetid": "document", "objectid": 22479, "filename": "preview.png", "mime_type": "image/png", "hash": "13e86c27e8945a8c89db5fbf26bd819d", "hash_type": "MD5", "filesize": 7107, "mtime": "2012-12-26 02:59:41", "url": "/3404/2/preview.png" } ], "eprint_id": 3404, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5939" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5939" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5939" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/04", "datestamp": "2008-09-12", "lastmod": "2021-04-16 23:33:01", "status_changed": "2009-09-25 02:57:53", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lichten-Stephen-Morris", "name": { "family": "Lichten", "given": "Stephen Morris" }, "show_email": "NO" } ] }, "title": "Turbulence and Mass Motion in Galactic Molecular Clouds", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "The main subject of this thesis is the origin and maintenance of supersonic gas motions in dense molecular clouds.
\r\n\r\nIn Chapters 1 and 2, we interpret and model millimeter wavelength CO line profiles whose broad wings and self-reversals provide clues about the nature of the observed supersonic motions. Broad molecular line wings provide evidence for high-velocity bipolar gas flows powered by strong stellar winds. The self-reversed CO line profiles are due in part to radiative transfer effects in molecular clouds which, in some cases, are expanding or contracting; Monte Carlo simulations of radiative transfer, however, demonstrate that cloud fragmentation may be responsible for some observed properties of the line profiles. The detection of broad-wing sources in quiescent, dark nebulae, shows that energetic outflows are common in a wide range of molecular clouds.
\r\n\r\nIn Chapter 3, our high resolution maps of molecular and atomic line emission across molecular cloud edges show that these clouds are embedded in warm H I halos which appear in emission against the galactic H I background. We also find that molecular cloud internal motions may be correlated with the H I halo temperature; however, the halo masses are much less than those of the molecular clouds and exert only a limited influence on internal cloud kinematics.
\r\n\r\nThe statistical and autocorrelation analyses of Chapters 4 and 5 show that molecular clouds are clumpy and contain hundreds of turbulent fragments whose relative velocities are supersonic, but whose internal velocity dispersions are not. Shock dissipation processes, clump collisions, and gas compression have major roles in molecular cloud kinematics. Our observations indicate that turbulent energy is supplied at small scales, as opposed to the dissipationless energy transfer from large to small scales which is known to occur in incompressible fluids with high Reynolds numbers. Energetic outflows from embedded young stars may break apart, fragment, and compress portions of molecular clouds, and may be capable of originating and sustaining the supersonic turbulence. Additional observational and theoretical studies of cloud clumpiness and of the rate of energy transfer from stellar outflows to ambient molecular material, are required before this mechanism for cloud support can be evaluated.
\r\n", "date": "1984", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-083043", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-083043", "related_url": { "items": [ { "description": "Article adapted from Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/159661" }, { "description": "Article adapted from Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/183781" }, { "description": "Article adapted from Chapter 3.", "type": "doi", "url": "https://doi.org/10.1086/160995" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" }, { "agency": "Achievement Rewards for College Scientists Foundation" }, { "agency": "J. Gimbel Estate" } ] }, "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/wbm2-9x67", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Wannier-P-G", "name": { "family": "Wannier", "given": "Peter G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Wannier-P-G", "name": { "family": "Wannier", "given": "Peter G." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1983-08-05", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1984", "author_list": "Lichten, Stephen Morris" }, { "id": "/id/eprint/10410", "eprint_id": 10410, "rev_number": 33, "documents": [ { "id": "/id/document/82434", "doc_id": 82434, "rev_number": 3, "files": [ { "id": "/id/file/232946", "fileid": 232946, "datasetid": "document", "objectid": 82434, "filename": "Macdonald_DA_1984.pdf", "mime_type": "application/pdf", "hash": "5e1540294f6e10f0818b6eb7e68be682", "hash_type": "MD5", "filesize": 54919927, "mtime": "2017-09-05 23:16:13", "url": "/10410/8/Macdonald_DA_1984.pdf" } ], "eprint_id": 10410, "pos": 8, "placement": 8, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Macdonald_DA_1984.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/82434" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/01/04/10", "datestamp": "2017-09-06 20:23:03", "lastmod": "2021-04-16 23:13:38", "status_changed": "2017-09-06 20:23:03", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Macdonald-Douglas-Alan", "name": { "family": "Macdonald", "given": "Douglas Alan" }, "show_email": "NO" } ] }, "title": "Black-Hole Electrodynamics", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This dissertation considers several aspects of the structure and dynamics of electromagnetic fields around black holes. The four-dimensional, covariant laws of electrodynamics are reformulated in a 3 + 1 (space+time) language in which the key quantities are three-dimensional vectors lying in hypersurfaces of a constant global time t. This formulation is applied to the Blandford-Znajek model of power generation in quasars, which consists of a supermassive black hole surrounded by an accretion disk that holds a magnetic field on the hole, with the rotational energy and angular momentum of the hole and disk being extracted by electromagnetic torques. The 3 + 1 formalism allows the theory of stationary, axisymmetric black holes and their magnetospheres to be couched in an \"absolute-space/universal-time\" language very similar to the flat\u00ad spacetime theory of pulsar electrodynamics; and this similarity allows fiat-space pulsar concepts to be extended to curved-space black holes. The Blandford\u00ad-Znajek quasar model is reformulated in terms of a DC circuit-theory analysis, and action principles describing the overall structure of the magnetosphere and the field distribution on the horizon are developed. A general prescription for constructing global models of force-free magnetospheres is developed and this prescription is used to generate numerical models of black-hole magneto\u00adspheres for a variety of field configurations and black-hole angular velocities. The electromagnetic boundary conditions at the horizon of a black hole are described in terms of a recently developed \"membrane viewpoint\". The necess\u00adity and efficacy of using a \"stretched horizon\" in the membrane viewpoint is discussed, and is illustrated by two simple dynamical problems involving electromagnetic fields near black-hole horizons.
", "date": "1984", "date_type": "degree", "id_number": "CaltechTHESIS:09012017-133647841", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09012017-133647841", "related_url": { "items": [ { "description": "Article adapted for Chapter II.", "type": "doi", "url": "https://doi.org/10.1093/mnras/198.2.339" }, { "description": "Article adapted for Chapter III.", "type": "doi", "url": "https://doi.org/10.1093/mnras/198.2.345" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST79-22012" }, { "agency": "NSF", "grant_number": "AST82-14126" }, { "agency": "NSF", "grant_number": "PHY77-27084" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-09-06 20:23:03", "doi": "10.7907/vv78-at49", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "chair" }, { "id": "Cowan-E-W", "name": { "family": "Cowan", "given": "Eugene W." }, "role": "member" }, { "email": "wise@theory.caltech.edu", "id": "Wise-M-B", "name": { "family": "Wise", "given": "Mark B." }, "role": "member" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1983-11-07", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1984", "author_list": "Macdonald, Douglas Alan" }, { "id": "/id/eprint/3402", "eprint_id": 3402, "rev_number": 11, "documents": [ { "id": "/id/document/5937", "doc_id": 5937, "rev_number": 3, "files": [ { "id": "/id/file/35314", "fileid": 35314, "datasetid": "document", "objectid": 5937, "filename": "Saha_a_1984.pdf", "mime_type": "application/pdf", "filesize": 5351050, "mtime": "2012-12-26 02:59:41", "url": "/3402/1/Saha_a_1984.pdf" } ], "eprint_id": 3402, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Saha_a_1984.pdf", "language": "en", "security": "public", "license": "other", "main": "Saha_a_1984.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22477" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22477" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22477" } ] } }, { "id": "/id/document/22477", "doc_id": 22477, "rev_number": 3, "files": [ { "id": "/id/file/35312", "fileid": 35312, "datasetid": "document", "objectid": 22477, "filename": "preview.png", "mime_type": "image/png", "hash": "977e67f7f443333c0e1d46ea46e14bc3", "hash_type": "MD5", "filesize": 7736, "mtime": "2012-12-26 02:59:41", "url": "/3402/2/preview.png" } ], "eprint_id": 3402, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5937" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5937" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5937" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/02", "datestamp": "2008-09-12", "lastmod": "2021-04-19 22:33:50", "status_changed": "2009-09-25 02:57:52", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Saha-Abhijit", "name": { "family": "Saha", "given": "Abhijit" }, "show_email": "NO" } ] }, "title": "A Survey of Halo RR Lyrae Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "A survey of RR Lyrae stars has been conducted in selected regions of the Galactic halo, using the 48 inch Schmidt telescope at Palomar. 29 RR Lyrae stars were found in three fields (each is 42 square degrees) centered at 1 = 180\u00b0, b = 24\u00b0; 1 = 180\u00b0, b = 30\u00b0 and 1 = 110\u00b0, b = -30\u00b0. The faint limit for finding RR Lyraes is 19m.5 in B, and the faintest RR Lyrae stars that were found are at Galactocentric distances of over 40 kpc. The majority of the stars are 20 to 30 kpc from the Galactic center, and typically around 18m in B. Apart from a very few globular clusters, these stars are the most distant known probes of the outer halo.
\r\n\r\nPhotoelectric photometry done with the 60 inch telescope at Palomar has been used to obtain accurate light curves and ephemerides for all the survey RR Lyraes stars. Spectrophotometry at minimum light has been used to estimate reddening and interstellar extinction. Distances to the individual RR Lyrae stars have been derived using the information thus obtained.
\r\n\r\nThe space densities of RR Lyrae stars has been traced out to a Galactocentric distance R of 33 kpc. The data are combined with that obtained by others in the Galactic bulge and in the relatively nearby halo, which gives an overall picture of the run of space densities over a very wide range of R.
\r\n\r\nSpectra of many of these objects have been taken with the double spectrograph on the 200 inch telescope at Palomar. Chemical abundances and radial velocities have been derived from them. Center of mass velocities have typically been obtained to an accuracy of 35 km s-1.
\r\n\r\nThere is no discernible abundance gradient in the halo from 10 to 40 kpc, but there is a very wide range of abundances. Two RR Lyrae stars have been found which have metallicities that are unprecedentedly high ([Fe/H] ~ -0.5]) for this region of the halo. If the results are confirmed, this will imply that there is a sizeable population of moderately metal rich stars in the outer halo.
\r\n\r\nFrom the radial velocities, the systemic and random motions of the system of RR Lyrae stars in the distant halo have been studied. The velocity dispersion along the axis that points to the Galactic center is found to be 105 \u00b1 17 km s-1. The mass of the Galaxy within 25 kpc has been estimated at 3.9 (+3.4 or -2.2) x 1011M\u2609, assuming isotropic orbits and spherical potential at 25 kpc. This confirms that the Galactic mass continues to increase out to 25 kpc.
\r\n", "date": "1984", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-080231", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-080231", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/d56z-kf18", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "chair" }, { "id": "Preston-G-W", "name": { "family": "Preston", "given": "George W." }, "role": "member" }, { "id": "Moffet-A-T", "name": { "family": "Moffet", "given": "Alan Theodore" }, "role": "member" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1983-09-30", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1984", "author_list": "Saha, Abhijit" }, { "id": "/id/eprint/3409", "eprint_id": 3409, "rev_number": 14, "documents": [ { "id": "/id/document/5944", "doc_id": 5944, "rev_number": 3, "files": [ { "id": "/id/file/35364", "fileid": 35364, "datasetid": "document", "objectid": 5944, "filename": "Simon_rs_1983.pdf", "mime_type": "application/pdf", "filesize": 4341639, "mtime": "2012-12-26 02:59:43", "url": "/3409/1/Simon_rs_1983.pdf" } ], "eprint_id": 3409, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Simon_rs_1983.pdf", "language": "en", "security": "public", "license": "other", "main": "Simon_rs_1983.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22484" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22484" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22484" } ] } }, { "id": "/id/document/22484", "doc_id": 22484, "rev_number": 3, "files": [ { "id": "/id/file/35362", "fileid": 35362, "datasetid": "document", "objectid": 22484, "filename": "preview.png", "mime_type": "image/png", "hash": "11589449e719459298a4169c336c139b", "hash_type": "MD5", "filesize": 7575, "mtime": "2012-12-26 02:59:43", "url": "/3409/2/preview.png" } ], "eprint_id": 3409, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5944" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5944" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5944" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/09", "datestamp": "2008-09-17", "lastmod": "2021-11-05 22:42:17", "status_changed": "2009-09-25 02:57:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Simon-Richard-Stanley", "name": { "family": "Simon", "given": "Richard Stanley" }, "show_email": "NO" } ] }, "title": "Nuclear Structure of Quasars at 329 Megahertz", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "In the four chapters in this thesis are presented studies of compact quasars using Very Long Baseline Interferometry at 329 MHz.
\r\n\r\nThe first chapter presents hybrid maps of two quasars, 3C147 and 3C286, made at 329 MHz from VLBI observations taken in 1975 with a three station interferometer. The observations presented in the first chapter were used to make the first detailed maps of compact radio structure at this frequency. Both objects consist of an unresolved core; an extended, asymmetric jet; and an even larger, completely resolved halo. For 3C147 it is possible to decompose the spectrum into individual component spectra; at 329 MHz the core of 3C147 is found to be strongly self-absorbed. For both sources the spectral index decreases monotonically from core to jet to halo.
\r\n\r\nThe second chapter presents further observations of quasars at 329 MHz. These observations were taken with a seven-station interferometer and were used to produce high dynamic range maps of the quasars 3C48, 3C147, 3C309.1, 3C380, and 3C454.3. These maps, made with the most extensive low-frequency VLBI observations to date, are the first reliable, high dynamic range maps at this frequency, and reveal extremely complex source structure in four of these sources. All five of the objects are seen to have asymmetric structure that can be interpreted in the \"core-jet\" picture of compact extragalactic radio sources. The jets observed in these objects are not straight, but bent; three of these quasars have bends in their structure greater than 90\u00b0 on scales of 1 - 10 kpc.
\r\n\r\nChapter three deals with the analysis of the two maps of 3C147 presented in chapters 1 and 2. Comparison of those maps reveals that the core of 3C147 is a low-frequency variable radio source which has brightened by a factor of two in six years. In combination with X-ray observations this is used to demonstrate that bulk relativistic motion is taking place within the core and leads to the prediction that 3C147 is a member of the class of \"superluminal\" radio sources. It is also found that the inclination to the line of sight of the underlying bulk relativistic motion is less than 10\u00b0.
\r\n\r\nA self-consistent picture of 3C147 as a low-frequency variable is thus developed which is consistent with the available observations, yet does not require an extreme value of the total energy: the total energy of the core of 3C147 is found to be ~1054 ergs. Together with NRAO 140 there are now two extragalactic low-frequency variable radio sources in which bulk relativistic motion has been demonstrated. Thus it may well be that bulk relativistic motion is responsible for the required time-scales in most, if not all, low-frequency variables.
\r\n\r\nIn chapter four, the observations presented in chapter two of 3C48, 3C147, 3C309.1, 3C380 and 3C4S4.3 are analyzed using standard synchrotron emission theory in order to discover the physical conditions occurring in these objects. For 3C48, the suggestion in chapter 2 of this source as a \"core-jet\" source is seen to be reasonable with fields energy density and pressure all decreasing with increasing distance from the supposed core. For 3C48, the suggestion in chapter 2 of this source as a \"core-jet\" source is seen to be reasonable, with fields, energy density, and pressure all decreasing with increasing distance from the supposed core. The pressure in the jet in 3C48 is extremely large, implying that the jet cannot be confined by external gas pressure, unless the surrounding medium has extreme values of the temperature and density. In the case of 3C147 (which was analyzed extensively in chapter 3), the halfwidth of the observed jet implies that collimation of the jet is occurring; the jet in 3C147 is definitely not a \"free\" jet. For 3C309.1, the 329 MHz observations give an upper limit to the turnover frequency for synchrotron self-absorption significantly lower than that available up to now; this limit, in combination with Einstein X-ray observations of 3C309.1, implies that bulk relativistic motion is occurring within the core of 3C309.1. Thus, the core of 3C309.1 may be very similar to the core of 3C147, and is a candidate for being both a superluminal source and a low-frequency variable. For 3C380 and 3C454.3, the limited spectral information available allows broad limits to be put on their properties.
\r\n", "date": "1983", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-093723", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-093723", "related_url": { "items": [ { "description": "Article adapted for Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/157793" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1038/302487a0" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-17", "doi": "10.7907/zyfw-8c64", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "chair" }, { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "member" }, { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1982-11-04", "thesis_approved_date": "2008-09-17", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1983", "author_list": "Simon, Richard Stanley" }, { "id": "/id/eprint/3436", "eprint_id": 3436, "rev_number": 29, "documents": [ { "id": "/id/document/5971", "doc_id": 5971, "rev_number": 3, "files": [ { "id": "/id/file/35568", "fileid": 35568, "datasetid": "document", "objectid": 5971, "filename": "Malkan_ma_1983.pdf", "mime_type": "application/pdf", "filesize": 6482387, "mtime": "2012-12-26 02:59:54", "url": "/3436/1/Malkan_ma_1983.pdf" } ], "eprint_id": 3436, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Malkan_ma_1983.pdf", "language": "en", "security": "public", "license": "other", "main": "Malkan_ma_1983.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22511" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22511" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22511" } ] } }, { "id": "/id/document/22511", "doc_id": 22511, "rev_number": 3, "files": [ { "id": "/id/file/35566", "fileid": 35566, "datasetid": "document", "objectid": 22511, "filename": "preview.png", "mime_type": "image/png", "hash": "1906dcc6fd543b51d89865d9989e2da5", "hash_type": "MD5", "filesize": 6554, "mtime": "2012-12-26 02:59:54", "url": "/3436/2/preview.png" } ], "eprint_id": 3436, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5971" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5971" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5971" } ] } }, { "id": "/id/document/64068", "doc_id": 64068, "rev_number": 3, "files": [ { "id": "/id/file/179377", "fileid": 179377, "datasetid": "document", "objectid": 64068, "filename": "Malkan Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "352922cb649dc12629fb7fccfb04d7a2", "hash_type": "MD5", "filesize": 864, "mtime": "2016-03-02 16:03:16", "url": "/3436/3/Malkan Thesis Permission Form.txt" } ], "eprint_id": 3436, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "author ok 3/1/2016", "language": "en", "security": "internal", "license": "other", "main": "Malkan Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/36", "datestamp": "2008-09-18", "lastmod": "2021-11-05 23:02:22", "status_changed": "2009-09-25 02:58:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "malkan@astro.ucla.edu", "id": "Malkan-Matthew-Arnold", "name": { "family": "Malkan", "given": "Matthew Arnold" }, "show_email": "YES" } ] }, "title": "The Physical Nature of the Continuum in Active Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Quasar, accretion disk, black hole, emission line, Seyfert galaxy, reddening", "abstract": "We have measured the intrinsic nonstellar continuum from the nuclei of a wide range of active galaxies. We find little or no continuum reddening (from the 2175\u00c5 absorption bump) above that expected from the interstellar medium of the Milky Way. Nor do optical and ultraviolet emission from permitted Fe II lines alter the overall appearance of the energy distribution very much. After accounting for hydrogen recombination radiation, we find the continuum consists of a power law (fV\u221dV-1.1), closely related to the X-ray emission, and an optically thick thermal component. Some bright quasars produce as much or more thermal power as nonthermal. The thermal energy has an average characteristic temperature of 20-30,000 K. It is perfectly described by relativistic accretion disk models which include the gravitational redshifting and focusing of emerging light. These models are completely specified by two well-determined parameters: the mass of the central black hole and the accretion rate. The hole masses range from 0.2-0.5 billion M\u2609 in 3C 273 to 1-3 billion in the most luminous quasars, depending on the disk inclination and the angular momentum of the hole. All the bright quasars are shining at within a factor of two of their Eddington limits, while the Seyfert 1 galaxies are well below theirs.
\r\n\r\nUnlike most Seyfert 1 galaxies, those of type 2 have a large portion of their total power re-radiated in the infrared by warm dust grains. The intrinsic continuum in the Seyfert 2 galaxies may have a nonthermal power-law, but appears to lack the hot thermal component seen in quasars. The host galaxies around Seyfert nuclei of types 1 and 2, and those around low-redshift quasars are normal spirals of early to intermediate type.
\r\n\r\nWe calculated the level populations for the 0+ and S+ ions, to use the [0 II] (7320+7330)/(3726+3729) and [S II] (4069+4076)/(6716+6730) line ratios as reddening indicators (accurate to \u00b10.1 mag. in EB-V). Seyfert 2 galaxies are typically reddened by 0.2-0.5 mag. Most Seyfert 1 galaxies have less than half as much reddening. The H\u03b1/H\u03b2 ratio in the broad-line region is often much larger than the Case B value, and it is significantly larger than 2.86 in some narrow-line regions. The intrinsic Balmer continuum/H\u03b1 ratio in the narrow-line region is 1.4, consistent with the Case B prediction. But in the broad-line region it is two to three times larger, because of the effects of high electron density and optical depth.
", "date": "1983", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-091935", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-091935", "related_url": { "items": [ { "description": "Article adapted for Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/159701" }, { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/160981" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1086/161549" }, { "description": "Article adapted for Chapter 4.", "type": "doi", "url": "https://doi.org/10.1086/161968" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "https://doi.org/10.1086/160656" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "https://doi.org/10.1086/183934" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-18", "doi": "10.7907/Z85C-9706", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1983-05-23", "thesis_approved_date": "2008-09-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1983", "author_list": "Malkan, Matthew Arnold" }, { "id": "/id/eprint/3392", "eprint_id": 3392, "rev_number": 12, "documents": [ { "id": "/id/document/5922", "doc_id": 5922, "rev_number": 3, "files": [ { "id": "/id/file/35225", "fileid": 35225, "datasetid": "document", "objectid": 5922, "filename": "Pier_jr_1983.pdf", "mime_type": "application/pdf", "filesize": 3780820, "mtime": "2012-12-26 02:59:34", "url": "/3392/1/Pier_jr_1983.pdf" } ], "eprint_id": 3392, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Pier_jr_1983.pdf", "language": "en", "security": "public", "license": "other", "main": "Pier_jr_1983.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22462" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22462" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22462" } ] } }, { "id": "/id/document/22462", "doc_id": 22462, "rev_number": 3, "files": [ { "id": "/id/file/35223", "fileid": 35223, "datasetid": "document", "objectid": 22462, "filename": "preview.png", "mime_type": "image/png", "hash": "0f28b2465636c8d11c22e10d29ed7fc1", "hash_type": "MD5", "filesize": 8381, "mtime": "2012-12-26 02:59:34", "url": "/3392/2/preview.png" } ], "eprint_id": 3392, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5922" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5922" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5922" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/92", "datestamp": "2008-09-12", "lastmod": "2021-04-16 22:21:22", "status_changed": "2009-09-25 02:57:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pier-Jeffrey-Ross", "name": { "family": "Pier", "given": "Jeffrey Ross" }, "show_email": "NO" } ] }, "title": "A Study of A- and B-Type Stars in the Southern Galactic Halo", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "A sample of over 200 stars of spectral types A and B has been selected for study. Drawn from the Preston and Shectman objective-prism survey of the southern galactic halo, the stars comprise a sample of halo objects selected without kinematic bias. Photoelectric UBV photometry has been obtained and the sample stars have apparent V magnitudes mostly in the range 13.5 \u2264 V \u2264 15.5. The (U-B)--(B-V) two-color diagram shows that the halo AB stars have colors similar to those of globular cluster blue horizontal-branch (BHB) stars.
\r\n\r\nReticon spectroscopy of the sample confirms the BHB status of the large majority of the sample. Interesting non-BHB stars found include a few high luminosity A stars, several stars of low metallicity and apparently normal main-sequence gravities which may be field Population II blue stragglers, and ten metallic-line stars. A few normal A stars have been found as far as 2 to 3 kpc from the plane, but none beyond that distance. It is suggested that the metal-rich early-type population found by other authors belongs to a population of old disk stars with a scale height of over 1 kpc.
\r\n\r\nInterstellar Ca II K lines are found in many of the high-velocity stars. The interstellar components arise from low-velocity material associated with the disk.
\r\n\r\nThe solar motion of the halo AB stars is -236 \u00b1 39 km s-1 and the velocity ellipsoid is elongated towards the galactic center throughout the halo. By adding a list of halo objects drawn from other sources and solving for the solar motion a lower limit of -208 \u00b1 20 km s-1 is set for the circular velocity at the solar radius. The solar motion solution is found to be metallicity-dependent. Anisotropy in the velocity ellipsoid is strongly indicated for the combined halo objects. The presence of this global anisotropy removes one of the arguments favoring a flattened halo. Since the gravitational potential of the disk increases the z component of velocity it is seen that at very early times in the history of the Galaxy the velocities were highly anisotropic (predominantly radial).
\r\n", "date": "1983", "date_type": "degree", "id_number": "CaltechETD:etd-09082008-142312", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082008-142312", "related_url": { "items": [ { "description": "Article adapted for Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/113242" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "United States Department of Veterans Affairs" } ] }, "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/s939-dc28", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "chair" }, { "id": "Mould-J-R", "name": { "family": "Mould", "given": "Jeremy R." }, "role": "member" }, { "id": "Preston-G-W", "name": { "family": "Preston", "given": "George W." }, "role": "member" }, { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-08", "thesis_defense_date": "1982-10-18", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1983", "author_list": "Pier, Jeffrey Ross" }, { "id": "/id/eprint/3391", "eprint_id": 3391, "rev_number": 14, "documents": [ { "id": "/id/document/5921", "doc_id": 5921, "rev_number": 3, "files": [ { "id": "/id/file/35220", "fileid": 35220, "datasetid": "document", "objectid": 5921, "filename": "Horne_kd_1983.pdf", "mime_type": "application/pdf", "filesize": 2838683, "mtime": "2012-12-26 02:59:34", "url": "/3391/1/Horne_kd_1983.pdf" } ], "eprint_id": 3391, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Horne_kd_1983.pdf", "language": "en", "security": "public", "license": "other", "main": "Horne_kd_1983.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/93405" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/93405" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/93405" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/91", "datestamp": "2008-09-12", "lastmod": "2021-11-05 23:02:05", "status_changed": "2009-09-25 02:57:42", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kdh1@st-andrews.ac.uk", "id": "Horne-Keith-Douglas", "name": { "family": "Horne", "given": "Keith Douglas" }, "show_email": "NO" } ] }, "title": "Eclipse Mapping of Accretion Disks in Cataclysmic Binaries", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Surface brightness distributions for accretion disks in eclipsing cataclysmic binaries may be reconstructed from observed eclipse light curves by use maximum entropy imaging methods. Three-color eclipse photometry of six eclipsing cataclysmic binaries provides the basis for an observational study of the local and global structure of their accretion disks. Observations from several eclipse cycles are averaged to form mean eclipse profiles with diminished contamination by flickering. Flickering is shown to be widely distributed over the face of the accretion disks in RW Tri and LX Ser. Accretion disk maps are derived which give satisfying fits to the observed eclipse profiles and which are maximally symmetric about the center of the disk. Disk maps for nova DQ Her and for four nova-like systems show broad intensity distributions with bright spots, associated with the gas streams that feed the disks, in evidence at a radii comparable to the disk tidal radius. The HT Cas disk is smaller and is dominated by a compact source at its center. Analysis of disk intensity maps at U, B and R show that the brighter parts of the accretion disks are optically-thick thermal radiators with temperatures which decrease with radius. The angular scale of each disk is fixed by a method analogous to cluster main sequence fitting. Distance estimates are derived which are free of assumptions about the global structure of the disks, but which depend on currently uncertain dyamical parameters of the binaries. The temperature in the disk is observed to fall much more slowly with radius than the R-3/4 law predicted by a steady-state mass-conserving viscous accretion disk model. Apparently, much of the visible light from the disk is produced by reprocessing of hard radiation from the center of the disk. Upper limits are found for the mass transfer rates which are one to two orders of magnitude smaller than the canonical mass transfer rate for novae and nova-like systems and which thus are in better agreement with mass transfer driven by gravitational radiation alone. Mass transfer rates have previously been systematically overestimated by the neglect of reprocessing. The accretion disk in HT Cas is shown to be optically thin in the Paschen continuum. The compact bright source at the center of its disk is a composite of light from the photosphere of the white dwarf and of free-free emission from hot gas in the accretion boundary layer.
\r\n", "date": "1983", "date_type": "degree", "id_number": "CaltechETD:etd-09082008-140704", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082008-140704", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/5E49-4N30", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "chair" }, { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-08", "thesis_defense_date": "1983-01-07", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/104814" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/104814" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/104814" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/90", "datestamp": "2008-09-12", "lastmod": "2020-07-17 00:05:15", "status_changed": "2009-09-25 02:57:42", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "kirk.borne@gmail.com", "id": "Borne-Kirk-Daniel", "name": { "family": "Borne", "given": "Kirk Daniel" }, "orcid": "0000-0001-5608-255X", "show_email": "YES" } ] }, "title": "The Structure and Evolution of Interacting Binary Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy, Galaxies, Mergers, Galaxy Evolution, Colliding Galaxies, Numerical Simulations, Merging Galaxies", "abstract": "A numerical code has been constructed for the study of the evolution of interacting binary galaxies. This \"multiple three-body\" algorithm (MTBA) essentially involves N concurrent three-body integrations; it is the sum of the interactions of the perturber with each of the N particles comprising the primary \"galaxy\" that determines the binary orbital evolution. MTBA incorporates a violent relaxation phase that allows the particles to redistribute themselves in the gravitational field of the perturber prior to the full binary orbital evolution calculation. This redistribution is important for systems with an initially strong tidal potential; their predicted merger times are 50-100% larger than previously estimated. Tabulated merger times for both circular and elliptical orbits demonstrate that typical close binary galaxies will merge in about twice their initial binary orbital periods, roughly 109 years. This timescale depends strongly on the binary separation, weakly on its mass ratio, and less on initial galaxy rotation than has heretofore been suggested.
\r\n\r\nA specific interacting binary simulation is described in detail in the first paper. Surface brightness maps, structural parameters, and rotation properties are described at various times during the evolution, followed by a discussion of the properties of the merger remnant. Many of the results reported here are consistent with those obtained from the larger, more expensive N-body simulations.
\r\n\r\nFor the second paper, MTBA is altered so that each \"galaxy\" is represented by a configuration of test particles. Simulated tidal interactions between these \"galaxies\" are matched to the measured properties of real binaries in an effort to determine the physical state of each observed pair. The catalog of isolated galaxy pairs prepared by Karachentsev has been culled for its E-E constituents. CCD pictures and long-slit spectroscopic observations have been obtained at KPNO for the most photometrically distorted of these systems. Such pairs very likely represent strongly interacting, physically associated, binary elliptical galaxies. Radial variations of rotation velocity and velocity dispersion are extracted from the spectroscopic data for each of the two galaxies in a given pair. The combined spectroscopic and photometric data for that binary can be reproduced by an appropriate projection of a particular numerical simulation of the system. Some constraints can be placed on the masses of the galaxies, their internal dynamical configurations, and the properties of their relative orbit, including the three-dimensional orientation of the pair. Detailed results are presented for two pairs, K99 and K564. NGC 1587, the brighter component of K99, has the highest rotation rate known for an E2 galaxy, with a value vrot/\u03c3 = 0.6.
", "date": "1983", "date_type": "degree", "id_number": "CaltechETD:etd-09082008-132748", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082008-132748", "related_url": { "items": [ { "description": "Article adapted for Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/162709" }, { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/166453" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/8PH6-6R18", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Gunn-J-E", "name": { "family": "Gunn", "given": "James E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "chair" }, { "id": "Gunn-James-E", "name": { "family": "Gunn", "given": "James E." }, "role": "member" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-08", "thesis_defense_date": "1982-06-16", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1983", "author_list": "Borne, Kirk Daniel" }, { "id": "/id/eprint/3389", "eprint_id": 3389, "rev_number": 16, "documents": [ { "id": "/id/document/5919", "doc_id": 5919, "rev_number": 3, "files": [ { "id": "/id/file/35206", "fileid": 35206, "datasetid": "document", "objectid": 5919, "filename": "Berriman_g_1983.pdf", "mime_type": "application/pdf", "filesize": 4475021, "mtime": "2012-12-26 02:59:33", "url": "/3389/1/Berriman_g_1983.pdf" } ], "eprint_id": 3389, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Berriman_g_1983.pdf", "language": "en", "security": "internal", "license": "other", "main": "Berriman_g_1983.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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A particular requirement of these techniques is that they do not rely on a model of the poorly understood discs. They can be applied not only to Cataclysmic Variable Stars, but also to other interacting systems containing a red star, such as symbiotic stars.
\r\n\r\nAnalysis of the visible to infrared colours of fourteen largely uneclipsing systems, based on flux ratio diagrams, shows that the red dwarfs and the opaque gas in the disc supply most of the infrared light, but the contributions of each vary widely from system to system, with more light coming from the red dwarfs in the longer period systems than in the shorter period ones. For nearly all the systems studied, upper limits can be found to the fluxes of the red dwarfs that are approximately independent of spectral type and of the conditions in the accretion discs.
\r\n\r\nIn highly inclined systems, measurements of the amplitudes of the tidally induced ellipsoidal variations of the red dwarfs provide a more precise measure of the proportion of light coming from the red dwarf. A technique to simulate the light curves of tidally distorted red dwarfs successfully accounts for the infrared light curves of U Geminorum, a system in which the red dwarf supplies nearly all the infrared light.
\r\n\r\nCompleting the Thesis is a visible and infrared study of the eclipsing dwarf nova OY Carina in quiescence. This system has been studied because in the visible, the red dwarf is seen to eclipse the white dwarf. Analysis of these eclipses, based on the assumption that the red dwarf fills its Roche Lobe, allows the determination of several fundamental properties of the system: the inclination of the system is 73.5\u00b0 to 81\u00b0, the mass of the white dwarf lies in the broad range 0.4-1.4 M\u2299 and the red dwarf lies either on or slightly below the Main Sequence mass radius relation. The principal source of uncertainty in the analysis is that the semi-amplitude of the radial velocity variations of the white dwarf is poorly known. The infrared light curves show an eclipse of the disc and, half a cycle later, a secondary minimum produced by the ellipsoidal variations of the red dwarf and its eclipse by the disc. The depth of this minimum and the colours of the system imply that the red dwarf supplies approximately one-half of the uneclipsed light of the system and that it eclipses more than three-fifths of the light of the disc. The latter result requires that the K magnitude of the red dwarf lies in the range 14.2 to 14.7. The distance to the system, as deduced from these limits and an estimate of the surface brightness of the red dwarf lies in the range 100 to 300pc. The infrared light of the disc comes largely from optically thin emission; the opaque gas occupying most of the disc does not supply much of infrared light because the disc is atypically small and more highly inclined compared with other systems.
", "date": "1983", "date_type": "degree", "id_number": "CaltechETD:etd-09082008-130459", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082008-130459", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1093/mnras/204.4.1105" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/psse-c523", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" }, { "id": "Persson-Eric", "name": { "family": "Persson", "given": "Eric" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-08", "thesis_defense_date": "1983-02-07", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1983", "author_list": "Berriman, Graham" }, { "id": "/id/eprint/945", "eprint_id": 945, "rev_number": 26, "documents": [ { "id": "/id/document/1447", "doc_id": 1447, "rev_number": 3, "files": [ { "id": "/id/file/9041", "fileid": 9041, "datasetid": "document", "objectid": 1447, "filename": "Gursel_y_1983.pdf", "mime_type": "application/pdf", "filesize": 5608089, "mtime": "2012-12-26 02:33:53", "url": "/945/1/Gursel_y_1983.pdf" } ], "eprint_id": 945, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Gursel_y_1983.pdf", "language": "en", "security": "internal", "license": "other", "main": "Gursel_y_1983.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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Part I deals with the question of stability of a spherically symmetric, charged black hole against scalar, electromagnetic, and gravitational perturbations. It consists of two papers written in collaboration with Igor D. NoVikov, Vernon D. Sandberg and A. A. Starobinsky. In these papers we describe the dynamical evolution of these perturbations on the interior of a Reissner-Nordstrom black hole. The instability of the hole's Cauchy horizon is discussed in detail in terms of the energy densities of the test fields as measured by a freely falling observer approaching the Cauchy horizon. We conclude that the Cauchy horizon of the analytically extended Reissner-Nordstrom solution is highly unstable and not a physical feature of a realistic gravitational collapse. Part II of this dissertation addresses two problems closely connected with muitipole structure of stationary, asymptotically flat spacetimes. It consists of two papers written in collaboration with Kip S. Thorne despite the fact that his name does not appear on one of them. The first one (Paper III in this thesis) shows the equivalence of the moments defined by Kip S. Thorne and the moments defined by Robert Geroch and Richard Hansen. The second (Paper IV in this thesis) proves a conjecture by Kip S. Thorne: In the limit of \"slow\" motion, general relativistic gravity produces no changes whatsoever in the classical Euler equations of rigid body motion. We prove this conjecture by giving an algorithm for generating rigidly rotating solutions of Einstein's equations from nonrotating, static solutions.
\r\n", "date": "1983", "date_type": "degree", "id_number": "CaltechETD:etd-03132009-081222", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03132009-081222", "related_url": { "items": [ { "description": "Article adapted for Part I, Paper I.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.19.413" }, { "description": "Article adapted for Part I, Paper II.", "type": "doi", "url": "https://doi.org/10.1103/PhysRevD.20.1260" }, { "description": "Article adapted for Part II, Paper III.", "type": "doi", "url": "https://doi.org/10.1007/BF01031881" }, { "description": "Article adapted for Part II, Paper IV.", "type": "doi", "url": "https://doi.org/10.1093/mnras/205.3.809" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST76-80801 A01" }, { "agency": "NSF", "grant_number": "AST76-80801 A02" }, { "agency": "NSF", "grant_number": "AST79-22012" }, { "agency": "NSF", "grant_number": "PHY77-27084" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-03-13", "doi": "10.7907/e9t6-dr05", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "email": "scf@theory.caltech.edu", "id": "Frautschi-S-C", "name": { "family": "Frautschi", "given": "Steven C." }, "role": "member" }, { "id": "Whitcomb-S-E", "name": { "family": "Whitcomb", "given": "Stanley E." }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-03-13", "thesis_defense_date": "1982-07-12", "thesis_approved_date": "2009-03-13", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1983", "author_list": "G\u00fcrsel, Halis Yekta" }, { "id": "/id/eprint/10391", "eprint_id": 10391, "rev_number": 28, "documents": [ { "id": "/id/document/82226", "doc_id": 82226, "rev_number": 4, "files": [ { "id": "/id/file/232268", "fileid": 232268, "datasetid": "document", "objectid": 82226, "filename": "Flammang_RA_1982.pdf", "mime_type": "application/pdf", "hash": "68e490df33005677c2c0ef4ddd369b87", "hash_type": "MD5", "filesize": 35513873, "mtime": "2017-08-28 21:03:48", "url": "/10391/1/Flammang_RA_1982.pdf" } ], "eprint_id": 10391, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Flammang_RA_1982.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/82226" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/01/03/91", "datestamp": "2017-08-28 21:34:44", "lastmod": "2021-04-16 23:08:56", "status_changed": "2017-08-28 21:34:44", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Flammang-Richard-Alan", "name": { "family": "Flammang", "given": "Richard Alan" }, "show_email": "NO" } ] }, "title": "Stationary Spherical Optically Thick Accretion into Black Holes", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "As its title indicates, this thesis treats the problem of stationary, spherical, optically thick accretion into black holes. By the phrase \"optically thick\" it is meant that (1) radiative energy transport can be adequately described by the diffusion approximation and (2) the photons are everywhere in local energy equilibrium (LTE) with the accreting gas particles.
\r\n\r\nIn Chapter 1, a general set of equations governing time-independent spherical accretion into black holes is formulated. The equations are fully general relativistic and are applicable to optically thick regions, optically thin regions, and the transition regions which join them. The radiation is treated using frequency-integrated moments. The full, infinite series of moment equations is given, together with the limiting forms the equations take in the optically thick regime.
\r\n\r\nIn Chapter 2, we present the mathematical theory of stationary spherical optically thick accretion. We analyze the integral curves of the differential equations describing the problem. We find a one-parameter family of critical points, where the inflow velocity equals the isothermal sound speed. Physical solutions must pass through one of these critical points. We obtain a complete set of boundary conditions which the solution must satisfy at the horizon of the black hole, and show that these, plus the requirement that the solution pass through a critical point, determine a unique solution to the problem. This analysis leads to a generalization of the well-known Bondi critical point constraint, which arises in the adiabatic accretion problem and which is effective at the point where the inflow velocity equals the adiabatic sound speed. We show that this point can be regarded as a \"diffused critical point\" in our problem. The analysis also yields a simple expression for the diffusive luminosity at radial infinity. Finally, we find a satisfying explanation for the rather peculiar critical point structure of this problem in an analysis of the characteristics and subcharacteristics present in the problem and in a \"hierarchical\" analysis of the waves which propagate along them.
\r\n\r\nIn Chapter 3, we apply the theory of optically thick accretion developed in Chapter 2 to a wide range of physically different accretion regimes. Numerical solutions are presented and their physical properties are discussed. For solutions in which radiation pressure PR dominates gas pressure PG, but in which gas energy density (including its rest-mass) \u03c1G dominates radiation energy density \u03c1R, we pay particular attention to the adabaticity of the flow. Our quantitative results in this regime agree very well with Begelman's (1978) theory. We find the dimensionless number which governs the importance of heat diffusion in our problem and show that it reduces to the idea of \"trapping of photons\" and to the P\u00e9clet number in the appropriate limits. We find that solutions with PR > PG and \u03c1R > \u03c1G are always essentially adiabatic, owing in part to a relativistic suppression of heat flux which becomes important in this regime. The diffusive luminosity at infinity for these solutions is the Eddington limit of the black hole; with the adiabatic accretion rate, \"efficiencies\" of up to order unity are possible. We give preliminary consideration to the question of the stability of our solutions against convection and conclude that the Schwarzschild criterion is applicable, even for our non-static accretion flows. We show that solutions with PR > PG are everywhere stable against convection. On the other hand, solutions which start out at radial infinity with PG > PR are unstable to convection (if the adiabatic index of the gas \u03b3G exceeds 17/12) from radial infinity down to the point where PR ~ PG and the radiation-gas mixture has attained an adiabatic index of 17/12. The diffusive luminosity at infinity for these solutions is reduced from the Eddington limit of the black hole by the factor (\u03b3G - 1)4PR\u221e/\u03b3GPG\u221e; it is further reduced by the ratio of the electron scattering opacity to the actual opacity at infinity, if this differs from unity. In most cases, energy diffusion has a negligible effect on the accretion rate of these solutions.
", "date": "1982", "date_type": "degree", "id_number": "CaltechTHESIS:08252017-133002176", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08252017-133002176", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Schlumberger Foundation" }, { "agency": "Danforth Foundation" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-28 21:34:44", "doi": "10.7907/t73p-2e81", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Whitcomb-S-E", "name": { "family": "Whitcomb", "given": "Stanley E." }, "role": "member" }, { "email": "bsimon@caltech.edu", "id": "Simon-B-M", "name": { "family": "Simon", "given": "Barry M." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1982-01-04", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. 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The clusters are distributed fairly uniformly in Abell richness class. Seventy-five new measurements of cluster redshifts are presented (previously published redshifts were used for the nine other clusters). The selection criteria resulted in a strong redshift-richness correlation in the sample. Poor clusters (richness classes 0 and 1) have redshifts ~0.09, while the richest clusters have redshifts roughly as twice as large.
\r\n\r\nDirect imaging of the core of each cluster was affected using a CCD area photometer. The wavelength response of the CCD is so different from that of previous photometric devices that a new photometric system is required. The reductions employ photon based k-corrections (instead of energy based ones) and galactic absorption determined by the neutral hydrogen column density.
\r\n\r\nThe luminosity of the brightest cluster galaxy (G1) within an aperture of 16 kpc radius is shown to be a good standard candle. Previous aperture measurements of 135 first-ranked cluster galaxies are placed on the CCD photometric system. Nearly 200 Gl's with redshifts less than 0.3 have been measured, and they effectively determine the luminosity of giant ellipticals at the present epoch. Their aperture luminosity dispersion is 0.34 mag, which can be reduced to slightly under 0.3 mag by removing richness and morphological trends. The richness correction is reasonably well established at 0.10 magnitudes per Abell richness class, with the rich clusters having brighter galaxies. The trend of luminosity with Bautz-Morgan type matches those of previous investigations, ~0.12 mag per subclass, with BM I clusters having brightest cluster galaxies which are 0.3 mag brighter than the average Gl.
\r\n\r\nAperture magnitudes were also determined for the second and third ranked cluster galaxies (G2 and G3), which are defined as the next two brightest galaxies within 250 kpc of Gl. The limiting radius was adopted because of the relatively small area covered by the detector. The dispersion in the aperture luminosity for G2 is 0.55 mag; for G3 the dispersion is 0.65 mag. On average G2 is 0.8 mag and G3 1.3 mag fainter than Gl. The luminosity dependence of G2 and G3 on Abell richness class is roughly the same as that for Gl, except for the richest clusters where G2 and G3 are much brighter than expected. There is no significant BM-luminosity correlation for either G2 or G3 in this sample. The observed colors for the brightest three cluster galaxies indicate that no color evolution has taken place since redshifts of 0.25 (~four billion years).
\r\n\r\nThe radius surface brightness profiles inside 16 kpc for Gl, G2, and G3 are fit fairly well by either a de Vaucouleurs model or a modified Hubble law. At 16 kpc the surface brightness for G1 falls off like a power law with an index of -1.6 to -1.8. For first-ranked galaxies the mean effective radius is 28 kpc and the mean core radius is 2.1 kpc. These scale lengths are three and five times the values for G2 and G3, respectively. The strong correlation of Gl's structure with its absolute magnitude and with cluster morphology are confirmed. The average aperture correction factor (\u03b1) for first-ranked cluster galaxies is 0.7; this reduces the sensitivity of the Hubble diagram to qo by 35%.
\r\n\r\nNearly half of the brightest cluster galaxies have multiple nuclei, roughly five times the number expected from projection effects. The multiple systems are, on average, ~0.13 magnitudes brighter than the single systems. An evolutionary correction to qo of ~+1.5 is required if the multiple systems are interpreted as mergers induced by dynamical friction. The merger process, however, can be calibrated from the \u03b1-luminosity relations; this allows corrections to be applied to each galaxy individually.
\r\n\r\nThere is a strong effective radius-surface brightness relation for brightest cluster galaxies. The surface brightness at the effective radius I(Re), determines the effective radius (Re) to ~25%. The observed effective radii (determined from fits to the inner 16 kpc) range from ~4 kpc to over 100 kpc. The outer regions (> 30 kpc) of galaxies with extended envelopes do not match the de Vaucouleurs profile found by fitting the inner regions. An angular diameter test based on the effective radii is impractical due to the large intrinsic scatter; a test using the surface brightness corrected effective radii conveys the same information as the standard redshift-magnitude test. The effective radius-surface brightness relation explains the small dispersion in the aperture magnitudes of Gl, and predicts that the total luminosities of brightest cluster galaxies grow as the 0.7 power of the scale length. If the mass-to-light ratio in ellipticals is constant, the luminosity-scale length correlation is incompatible with the Faber-Jackson relation. Application of the Re-I(Re) relation to the brightest galaxies in Virgo (NGC 4472 and NGC 4486) yields a null result (no infall) for the distortion of the local Hubble flow. Infall velocities of 250 km s-1 are excluded at the 2\u03c3 level. The second and third ranked galaxies follow a similar Re-I(Re) relation. The exponent in the luminosity scale length relation for G2 is about 10% smaller than that for Gl. For G3 the luminosity increases as the square root of the scale length.
\r\n\r\nData of sufficient quality to allow construction of luminosity functions were obtained for 60 of the 84 clusters. The limited size of the field required that the luminosity functions be determined inside a given metric radius (250 kpc). The observed luminosity functions were fit to Schechter functions using maximum likelihood techniques. The brightest cluster galaxy cannot be drawn from a universal luminosity function. It is impossible to reconcile the small total luminosity-richness correlation with the relatively large (0.6 mag) dispersion in their total luminosities. The first- ranked galaxies are also about one magnitude too bright to be drawn from a Schechter function. Excluding Gl from the luminosity function results in satisfactory Schechter function fits to the rest of the cluster members. The power-law slope at low luminosities is ~-1, but is not well determined. The observations find a mean M* in close agreement with other investigations. The observed dispersion of M* about the mean as a function of cluster richness is similar to that predicted from numerical simulations.
\r\n\r\nCluster richness is defined as the total luminosity found by integrating over all luminosities the best fitting Schechter function determined from galaxies within 250 kpc of the brightest cluster galaxy. This definition correlates well but not perfectly with Abell richness class. Richness (actually central density) varies by nearly a factor of 40 from the poorest to the richest clusters in this sample,and in several poor clusters the brightest galaxy outshines the rest of the core. The total luminosity of G1 is weakly correlated with richness (at the same level as with Abell richness class). The luminosities of G2 and G3, however, exhibit a strong positive relationship with cluster richness.
\r\n\r\nSurface photometry of ~2000 cluster members indicates that they may form the basis for a very powerful angular diameter (or luminosity) test for the deceleration parameter, but uncertainties in the seeing corrections and object selection effects must first be resolved.
\r\n\r\nThe evidence for dynamical evolution, while admittedly circumstantial, is nevertheless persuasive. The strong structure-luminosity relation and the frequency of multiple systems are strong arguments in favor of galactic cannibalism. A detailed spectroscopic and photometric study of a brightest cluster galaxy composed of nine nuclei, V Zw 311, indicates that dynamical friction can radically alter a galaxy in a time scale of only a billion years. The lack of strong luminosity-richness correlation is the most often advanced objection to the merger picture, but dynamical studies of rich systems are required before their capture rates can be calculated.
", "date": "1982", "date_type": "degree", "id_number": "CaltechETD:etd-09172008-091944", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09172008-091944", "related_url": { "items": [ { "description": "Article adapted for Chapter I.", "type": "doi", "url": "https://doi.org/10.1086/160602" }, { "description": "Article adapted for Chapter II.", "type": "doi", "url": "https://doi.org/10.1086/160973" }, { "description": "Article adapted for Chapter IV.", "type": "doi", "url": "https://doi.org/10.1086/160475" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-05", "doi": "10.7907/tsbt-dz83", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" }, { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "id": "Gunn-James-E", "name": { "family": "Gunn", "given": "James E." }, "role": "chair" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" }, { "id": "Moffet-A-T", "name": { "family": "Moffet", "given": "Alan Theodore" }, "role": "member" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" }, { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-17", "thesis_defense_date": "1982-04-13", "thesis_approved_date": "2008-11-05", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1982", "author_list": "Schneider, Donald P." }, { "id": "/id/eprint/3320", "eprint_id": 3320, "rev_number": 17, "documents": [ { "id": "/id/document/5840", "doc_id": 5840, "rev_number": 3, "files": [ { "id": "/id/file/34647", "fileid": 34647, "datasetid": "document", "objectid": 5840, "filename": "Redman_ro_1982.pdf", "mime_type": "application/pdf", "filesize": 2174878, "mtime": "2012-12-26 02:59:03", "url": "/3320/1/Redman_ro_1982.pdf" } ], "eprint_id": 3320, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Redman_ro_1982.pdf", "language": "en", "security": "internal", "license": "other", "main": "Redman_ro_1982.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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The clouds are shown to be roughly bar-shaped with their long axes normally aligned within thirty degrees of the axis of the spiral arm in which the cloud is embedded. The long axis is typically three times longer than the two shorter axes, although all axial ratios from one to five appear to be present. These results appear to be independent of cloud size over the range from 15 parsecs to 175 parsecs for the maximum apparent cloud dimension.
\r\n\r\nIn Part II, the size distribution of the CO clouds is measured. Most of the mass of molecular gas in the galaxy resides in the largest clouds, with semimajor axes slightly larger than 100 pc long. The largest cloud sizes appear to be about the same over the entire molecular disk. These very large clouds must have been formed full sized from the intercloud gas, since they cannot have been assembled from smaller clouds. In deriving this distribution a simple and effective technique was developed to resolve the kinematic distance ambiguity.
\r\n\r\nThe concentration of the mass of molecular gas into the largest clouds, and the alignment of the clouds along the spiral arms, both indicate that the clouds are very young. They must be formed directly from the intercloud medium, probably behind a spiral arm shock wave, and cannot grow over long periods of time from smaller clouds. The mechanism forming the clouds from the intercloud gas must have a prefered scale length. Examples of such mechanisms are the Parker magnetic instability, or the collapse of a slowly accumulating dust lane. Similarly, the clouds must be dispersed rapidly at the ends of their lives.
\r\n", "date": "1982", "date_type": "degree", "id_number": "CaltechETD:etd-09032008-131405", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09032008-131405", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" }, { "agency": "National Research Council of Canada" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-08", "doi": "10.7907/p0pn-sw91", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Wannier-P-G", "name": { "family": "Wannier", "given": "Peter G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "tgp@submm.caltech.edu", "id": "Phillips-T-G", "name": { "family": "Phillips", "given": "Thomas G." }, "role": "chair" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "email": "mxs@astro.caltech.edu", "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "member" }, { "id": "Wannier-P-G", "name": { "family": "Wannier", "given": "Peter G." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-03", "thesis_defense_date": "1981-11-03", "thesis_approved_date": "2008-09-08", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1982", "author_list": "Redman, Russell Ormond" }, { "id": "/id/eprint/3317", "eprint_id": 3317, "rev_number": 25, "documents": [ { "id": "/id/document/5837", "doc_id": 5837, "rev_number": 3, "files": [ { "id": "/id/file/34624", "fileid": 34624, "datasetid": "document", "objectid": 5837, "filename": "Linfield_rp_1981.pdf", "mime_type": "application/pdf", "filesize": 1811172, "mtime": "2012-12-26 02:59:02", "url": "/3317/1/Linfield_rp_1981.pdf" } ], "eprint_id": 3317, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Linfield_rp_1981.pdf", "language": "en", "security": "internal", "license": "other", "main": "Linfield_rp_1981.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { 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\r\n\r\nIn the first, VLBI maps are presented of the nuclear cores of four radio galaxies which have large symmetric radio lobes: 3C 111, 3C 390.3, Cyg A, and 0055+30. Each source contains a nuclear jet having a scale of 1 pc, but no counterjets are seen. The jets in 3C 111 and 0055+30 point directly at the outer radio lobes, but in 3C 390.3 and Cyg A the jets are pointed from 4 to 6 degrees away from the lobes.
\r\n\r\nThe implications of the maps and models of these sources are considered in the second study. It is concluded that in all four cases, the observed asymmetry reflects an intrinsic asymmetry on a msec scale. The minimum pressure in the four jets is calculated, and it is concluded that the jet in Cyg A is very unlikely to be confined by gas pressure.
\r\n\r\nIn the third study, an attempt is made to explain the structure of compact radio sources with a precession-like motion or a relativistic jet. It is found that the curvature of these sources can be readily explained in this way. In addition, the knots which are often revealed by VLBI observations arise naturally in such a model. The main problem with the model is that it cannot by itself explain the arcsecond structure of asymmetric radio sources.
", "date": "1981", "date_type": "degree", "id_number": "CaltechETD:etd-09022008-153247", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09022008-153247", "related_url": { "items": [ { "description": "Article adapted for Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/158720" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/5cg5-0d24", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "chair" }, { "id": "Kellerman-Kenneth-I", "name": { "family": "Kellerman", "given": "Kenneth I." }, "role": "member" }, { "id": "Young-Peter-J", "name": { "family": "Young", "given": "Peter J." }, "role": "member" }, { "email": "acr@astro.caltech.edu", "id": "Readhead-A-C-S", "name": { "family": "Readhead", "given": "Anthony C. S." }, "orcid": "0000-0001-9152-961X", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-02", "thesis_defense_date": "1981-04-28", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1981", "author_list": "Linfield, Roger Paul" }, { "id": "/id/eprint/3340", "eprint_id": 3340, "rev_number": 19, "documents": [ { "id": "/id/document/5861", "doc_id": 5861, "rev_number": 4, "files": [ { "id": "/id/file/34800", "fileid": 34800, "datasetid": "document", "objectid": 5861, "filename": "Yee_hck_1981.pdf", "mime_type": "application/pdf", "filesize": 4879864, "mtime": "2012-12-26 02:59:12", "url": "/3340/1/Yee_hck_1981.pdf" } ], "eprint_id": 3340, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Yee_hck_1981.pdf", "language": "en", "security": "internal", "license": "other", "main": "Yee_hck_1981.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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\r\n\r\nMultichannel scans of 3CR radio galaxies are decomposed by using a two-component model -- an elliptical galaxy and a power-law nonthermal component. It is found that there is a strong correlation between the luminosity of the power-law component and the strength of the Balmer emission-lines. In most cases, by extrapolating to the Lyman continuum, the power-law models derived provide enough ionizing radiation to account for the Balmer line strengths.
\r\n\r\nExtending the study of radio galaxies to include Seyfert galaxies and quasars, it is found that there is a strong continuity between broad-line AGN's and quasars in terms of similarities in the correlations between line luminosities and nonthermal continuum luminosity. There is a tight correlation between H\u03b2 and nonthermal luminosity for all objects, suggesting that the Balmer lines arise from recombination after photoionization by the central continuum, and that parameters such as the overall spectral index and the covering factor are similar. Relative to the nonthermal continuum, the forbidden lines of the broad-line objects are approximately one order of magnitude weaker than those of the narrow-line objects. This is consistent with the view that forbidden lines are suppressed in the dense broad-line region of the broad-line objects.
\r\n\r\nNext, a study of the variability of absolute optical energy distribution and emission-lines of the N-galaxies 3C 382 and 3C 390.3 is made. By assuming that the nuclear component retains its spectral shape despite the variation, consistent decomposition of the spectrum into its nuclear and ellitipcial galaxy component can be made. Within each object, the narrow forbidden lines have remained constant, but the broad Balmer lines vary with the luminosity of the central component (LNT) as a power-law: L\u0393NT with \u0393 < 0.5. This relation can be explained by having two components of broad-line gas clouds \u2014 one having a time-scale for variability of a few months, the other, years. Variability of Balmer line profiles in these two objects are also discussed.
\r\n\r\nLastly, a preliminary study of surface photometry of Markarian Seyfert galaxies are presented. It is found that the properties of the underlying galaxies such as scale-length and surface brightness of the disk, color, and total brightness, do not depart systematically from those of luminous normal spiral galaxies. In addition, along with the results from the study of radio galaxies, it is found that there is no correlation between the luminosity of nuclear component and the brightness of the host-galaxy.
", "date": "1981", "date_type": "degree", "id_number": "CaltechETD:etd-09052008-110748", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09052008-110748", "related_url": { "items": [ { "description": "Article adapted for Chapter 1.", "type": "doi", "url": "https://doi.org/10.1086/156657" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/5AKF-YS51", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "bts@irastro.caltech.edu", "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. Thomas" }, "role": "member" }, { "id": "Young-Peter-J", "name": { "family": "Young", "given": "Peter J." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-05", "thesis_defense_date": "1980-10-30", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1981", "author_list": "Yee, Howard Kwong Chew" }, { "id": "/id/eprint/3388", "eprint_id": 3388, "rev_number": 15, "documents": [ { "id": "/id/document/5918", "doc_id": 5918, "rev_number": 3, "files": [ { "id": "/id/file/35199", "fileid": 35199, "datasetid": "document", "objectid": 5918, "filename": "Wade_ra_1981.pdf", "mime_type": "application/pdf", "filesize": 4259963, "mtime": "2012-12-26 02:59:33", "url": "/3388/1/Wade_ra_1981.pdf" } ], "eprint_id": 3388, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Wade_ra_1981.pdf", "language": "en", "security": "internal", "license": "other", "main": "Wade_ra_1981.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/107887" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/107887" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/88", "datestamp": "2008-09-12", "lastmod": "2021-04-16 23:32:19", "status_changed": "2009-09-25 02:57:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wade-Richard-Alan", "name": { "family": "Wade", "given": "Richard Alan" }, "show_email": "NO" } ] }, "title": "Spectroscopy and Spectrophotometry of Cataclysmic Variable Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Distances and luminosities of individual cataclysmic variable stars (as opposed to statistical properties of the group as a whole) can best be acquired by studying the secondary stars of these short-period binary systems. Since the secondary stars are of late spectral type, observations in the near infrared are especially useful.
\r\n\r\nSpectrophotometry of the dwarf nova U Geminorum has been carried out from 0.3\u00b5 to 1\u00b5 using the Hale 5m telescope. The energy distribution can be interpreted as the sum of fluxes from an M4.5 or M5 star and a source giving a flat continuum. The M companion, referred to as U Gem B, is less dense than a main-sequence star of the same color index. The absolute spectrophotometry allows a distance modulus of 4.4 \u00b1 0.8 mag to be derived for U Geminorum. The absolute visual magnitude of the quiescent system is about Mv = 10.3.
\r\n\r\nThe Na I infrared doublet in the spectrum of U Geminorum has been observed at high resolution around the orbit. The velocity semi-amplitude of U Gem B is 283 \u00b1 15 km s-1, and spectroscopic conjunction occurs before mid-eclipse of the bright spot. These results, combined with previous analysis of the emission-line velocity variations, have been used to deduce M1 = 1.01 \u00b1 0.25 and M2 = 0.36 \u00b1 0.10 (solar units) for the masses of the component stars. U Gem B is too cool and probably too large, compared to a zero-age main-sequence star of the same mass.
\r\n\r\nA spectrophotometric survey of about 30 cataclysmic variable stars has been carried out from 0.3\u00b5 to 1\u00b5. Old novae, nova-like variables, and erupting dwarf novae are characterized by spectral energy distributions which are flat (f\u03bd = constant) or rising toward shorter wavelengths. These objects have Balmer jumps in absorption or else no Balmer jump at all. No trace of a red stellar spectrum is evident in these stars, except for the nova-like system RW Tri. Quiescent dwarf novae show emission Balmer jumps and emission lines of the Balmer series and He I. Some quiescent dwarf novae show no trace of the spectrum of the secondary star, while others show the secondary star with various degrees of observability.
\r\n\r\nThese spectral energy distributions are analyzed to determine the spectral types of the secondary stars and the fraction of light contributed by the primary stars and their accretion disks. The analysis makes use of flux-ratio diagrams to eliminate those spectral decompositions which result in physically implausible energy distributions for the accretion disks. The Balmer jump is especially useful in eliminating unphysical distributions. Refined estimates of spectral type and fractional light contribution are made in favorable cases, using an interactive computer program. It is argued that the secondary stars in cataclysmic variable systems should be expected to deviate from the normal main-sequence relations among mass, radius, spectral type, and luminosity. The results of the analysis support previous workers' estimates of the absolute visual magnitudes of cataclysmic variable stars; the spectral types assigned to the secondary stars of individual systems on the basis of this work are generally later than those assigned by previous workers.
", "date": "1981", "date_type": "degree", "id_number": "CaltechETD:etd-09082008-093158", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082008-093158", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/112450" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/83wt-0h57", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "chair" }, { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Young-Peter-J", "name": { "family": "Young", "given": "Peter J." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-08", "thesis_defense_date": "1980-10-23", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1981", "author_list": "Wade, Richard Alan" }, { "id": "/id/eprint/10394", "eprint_id": 10394, "rev_number": 49, "documents": [ { "id": "/id/document/82233", "doc_id": 82233, "rev_number": 3, "files": [ { "id": "/id/file/232287", "fileid": 232287, "datasetid": "document", "objectid": 82233, "filename": "Wisdom_jl_1981.pdf", "mime_type": "application/pdf", "hash": "5d60979cb4494c84eca98f0d6f47e8dc", "hash_type": "MD5", "filesize": 19568200, "mtime": "2017-08-28 22:00:19", "url": "/10394/1/Wisdom_jl_1981.pdf" } ], "eprint_id": 10394, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Wisdom_jl_1981.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 87, "dir": "disk0/00/01/03/94", "datestamp": "2017-08-28 22:22:27", "lastmod": "2020-04-16 16:13:34", "status_changed": "2017-08-28 22:22:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "wisdom@mit.edu", "id": "Wisdom-Jack-Leach", "name": { "family": "Wisdom", "given": "Jack Leach" }, "show_email": "YES" } ] }, "title": "1. The Origin of the Kirkwood Gaps: A Mapping for Asteroidal Monitor Near the 3/1 Commensurability. 2. The Resonance Overlap Criterion and the Onset of Stochastic Behavior in the Restricted Three-Body Problem", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "note": "Title listed in 1981 commencement program -- I. The Origin of the Kirkwood Gaps: A Mapping for Asteroidal Monitor Near the 3/1 Commensurability. II. The Resonance Overlap Criterion and the Onset of Stochastic Behavior in the Restricted Three-Body Problem -- varies from title listed in thesis file (PDF).", "abstract": "Paper 1:
\r\n\r\nA mapping of the phase space onto itself with the same low order resonance structure as the 3/1 commensurability in the planar elliptic three-body prob\u00adlem is derived. This mapping is approximately one thousand (1000) times faster than the usual method of numerically integrating the averaged equations of motion (as used by Schubart, Froeschl\u00e9 and Scholl in their studies of the asteroid belt). This mapping exhibits some very surprising behavior that might provide the key to the origin of the gaps. A test asteroid placed in the gap may evolve for a million years with low eccentricity (< 0.05) and then suddenly jump to large eccentricity (> 0.3) becoming a Mars crosser. The asteroid can then be removed by a close encounter with Mars. To test this hypothesis a dis\u00adtribution of 300 test asteroids in the neighborhood of the 3/1 commensurability was evolved for two million years. When the Mars crossers are removed the dis\u00adtribution of initial conditions displays a gap at the location of the 3/1 Kirkwood gap. While this is the first real demonstration of the formation of a gap, the gap is too narrow. The planar elliptic mapping is then extended to include the incli\u00adnations and the secular perturbations of Jupiter's orbit. The two million year evolution of the 300 test asteroids is repeated using the full mapping. The resulting gap is somewhat larger yet still too small. Finally the possibility that over longer times more asteroids will become Mars crossers is tested by studying the evolution of one test asteroid near the border of the gap for a much longer time. A jump in its eccentricity occurs after 18 million years indicating that indeed it may simply be a matter of time for the full width of the gap to open.
\r\n\r\nPaper 2:
\r\n\r\nThe resonance overlap criterion for the onset of stochastic behavior is applied to the planar circular-restricted three-body problem with small mass ratio (\u00b5). Its predictions for \u00b5 = 10-3, \u00b5 = 10-4 and \u00b5 = 10-5 are compared to the transitions in the numerically determined Kolmogorov-Sinai entropy and found to be in remarkably good agreement. In addition, an approximate scaling law for the onset of stochastic behavior is derived.
", "date": "1981", "date_type": "degree", "id_number": "CaltechTHESIS:08282017-145742321", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08282017-145742321", "related_url": { "items": [ { "description": "Article adapted for Paper 1.", "type": "doi", "url": "https://doi.org/10.1086/113132" }, { "description": "Article adapted for Paper 2.", "type": "doi", "url": "https://doi.org/10.1086/112778" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NGL 05-002-003 " }, { "agency": "NSF", "grant_number": "AST-8020005" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-28 22:22:27", "doi": "10.7907/s1r9-ff38", "alt_title": { "items": [ "I. The Origin of the Kirkwood Gaps: A Mapping for Asteroidal Monitor Near the 3/1 Commensurability. II. The Resonance Overlap Criterion and the Onset of Stochastic Behavior in the Restricted Three-Body Problem", "The Origin of the Kirkwood Gaps: A Mapping for Asteroidal Monitor Near the 3/1 Commensurability", "The Origin of the Kirkwood Gaps", "A Mapping for Asteroidal Monitor Near the 3/1 Commensurability", "The Resonance Overlap Criterion and the Onset of Stochastic Behavior in the Restricted Three-Body Problem" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" }, { "id": "Cohen-D-S", "name": { "family": "Cohen", "given": "Donald S." }, "role": "member" }, { "id": "Zachariasen-F", "name": { "family": "Zachariasen", "given": "Fredrik" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1981-05-15", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1981", "author_list": "Wisdom, Jack Leach" }, { "id": "/id/eprint/3432", "eprint_id": 3432, "rev_number": 8, "documents": [ { "id": "/id/document/5967", "doc_id": 5967, "rev_number": 3, "files": [ { "id": "/id/file/35539", "fileid": 35539, "datasetid": "document", "objectid": 5967, "filename": "Rabin_dm_1981.pdf", "mime_type": "application/pdf", "filesize": 8610043, "mtime": "2012-12-26 02:59:53", "url": "/3432/1/Rabin_dm_1981.pdf" } ], "eprint_id": 3432, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Rabin_dm_1981.pdf", "language": "en", "security": "public", "license": "other", "main": "Rabin_dm_1981.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22507" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22507" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22507" } ] } }, { "id": "/id/document/22507", "doc_id": 22507, "rev_number": 3, "files": [ { "id": "/id/file/35537", "fileid": 35537, "datasetid": "document", "objectid": 22507, "filename": "preview.png", "mime_type": "image/png", "hash": "d0bbdcd3ba8a49251b7e53646428516a", "hash_type": "MD5", "filesize": 9711, "mtime": "2012-12-26 02:59:52", "url": "/3432/2/preview.png" } ], "eprint_id": 3432, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5967" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5967" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5967" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/32", "datestamp": "2008-09-18", "lastmod": "2021-04-16 22:16:14", "status_changed": "2009-09-25 02:58:19", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rabin-D", "name": { "family": "Rabin", "given": "Douglas" }, "show_email": "NO" } ] }, "title": "Studies of stellar populations : star clusters in M31, the galaxy and the Magellanic clouds", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThis study focusses on medium resolution spectra of the integrated light of star clusters in our own Galaxy and in three nearby systems: M31 and the two Magellanic Clouds. Since only integrated properties will normally be observable for clusters in more distant galaxies, or for the galaxies themselves, it is important to develop quantitative techniques which relate features of the integrated light to physical characteristics such as age and chemical composition. Here, digital SIT spectra are analyzed both internally, as multivariate data sets, and externally, by comparison with evolutionary models of star clusters and with detailed observations of nearby clusters.\n\nFor 22 clusters in M31, direct comparison of the equivalent widths of various metallic features in the wavelength region [...]3800-5300 shows that they determine a one-dimensional sequence in cluster metallicity. However, a robust principal components analysis reveals that the Balmer lines ([...], [...], [...]) behave distinctively, both in the Galaxy and in M31. For galactic globular clusters, the independence of the hydrogen lines shows up as a poor correlation between the strength of the Balmer lines in the integrated spectrum and the observed distribution of stars along the horizontal branch. Synthesis models are used to evaluate possible explanations, none wholly satisfactory. Compared with spectra of standard stars, the M31 spectra provide a clue which may bear on the problem in both galaxies: all the Balmer lines are contaminated by metallic features, and this is advanced as the cause of the enhanced [...] strength in strong lined M31 clusters. In some cases the enhancement is seen directly.\n\nIt is speculatively suggested that the M31 clusters exhibit in integrated light a mild form of the \"hyperstrong line\" phenomenon ascribed to some stars and to the nuclei of some elliptical galaxies.\n\nBalmer lines are also central to the interpretation of the spectra of 17 \"red\" clusters in the Magellanic Clouds, but now as a manifestation of stars at the turnoff in the HR diagram and hence as direct indicators of age. In these spectra, the strength of the Ca II K line is well correlated with the strength of the G band, but the relation between K andAn automated system is created which scans photographic plates, locating, measuring, and identifying the objects on these plates. Four deep red sensitive plates from the Palomar 1.2 m. telescope are examined with this system. The objects classified as galaxies are divided into subcatalogs of different apparent magnitudes. The angular correlation function w(\u03b8) (a measure of how galaxies cluster) is computed for each subcatalog for galaxy separations between 18\" and 4'32\". This enables an analysis of the behavior of the angular correlation function with changing apparent magnitude.
\r\n\r\nThe slope of log correlation function versus log angle, for galaxies 16 < mr < 20.5, is measured to be -1.23 \u00b1 0.18, with a hint of higher negative slopes at fainter magnitudes. This is inconsistent at the 2\u03c3 level with the standard slope of -0.8, but may be possible if the slope is a function of magnitude or an effect of the smaller angular size (~ 1 arc. min.) used here.
\r\n\r\nThe slope of the log correlation function as a function of magnitude is most consistent with the slope of the log correlation function as a function of angle for bright galaxies being about -1.1, consistent with the above result.
\r\n\r\nIf this slope is -0.8, then moderate to strong correlation function evolution is favored. If the slope of the log correlation function versus angle is higher then less correlation function evolution is needed.
\r\n\r\nIf the slope is allowed to float to its preferred higher value, then amount of correlation function evolution cannot be distinguished.
\r\n\r\nNo luminosity or color evolution is included in the models, but the models have no trouble fitting the data without it.
", "date": "1981", "date_type": "degree", "id_number": "CaltechETD:etd-09052008-130643", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09052008-130643", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/112570" }, { "description": "Article adapted for Chapter 3.", "type": "doi", "url": "https://doi.org/10.1117/12.959807" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-11", "doi": "10.7907/179j-3364", "alt_title": { "items": [ "Use of an Automated Photographic Object Detection System to Analyze the Effect of Magnitude on the Angular Correlation Function of Galaxies" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "chair" }, { "id": "Gunn-James-E", "name": { "family": "Gunn", "given": "James E." }, "role": "member" }, { "id": "Young-Peter-J", "name": { "family": "Young", "given": "Peter J." }, "role": "member" }, { "id": "Lo-Kwok-Yung", "name": { "family": "Lo", "given": "Kwok-Yung" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-05", "thesis_defense_date": "1981-05-18", "thesis_approved_date": "2008-09-11", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1981", "author_list": "Sebok, William Lawrence" }, { "id": "/id/eprint/3330", "eprint_id": 3330, "rev_number": 8, "documents": [ { "id": "/id/document/5850", "doc_id": 5850, "rev_number": 3, "files": [ { "id": "/id/file/34720", "fileid": 34720, "datasetid": "document", "objectid": 5850, "filename": "Hoessel_jg_1980.pdf", "mime_type": "application/pdf", "filesize": 3524302, "mtime": "2012-12-26 02:59:08", "url": "/3330/1/Hoessel_jg_1980.pdf" } ], "eprint_id": 3330, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Hoessel_jg_1980.pdf", "language": "en", "security": "public", "license": "other", "main": "Hoessel_jg_1980.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22391" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22391" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22391" } ] } }, { "id": "/id/document/22391", "doc_id": 22391, "rev_number": 3, "files": [ { "id": "/id/file/34718", "fileid": 34718, "datasetid": "document", "objectid": 22391, "filename": "preview.png", "mime_type": "image/png", "hash": "09b08c77010febf7a778f0f492cb142f", "hash_type": "MD5", "filesize": 9480, "mtime": "2012-12-26 02:59:08", "url": "/3330/2/preview.png" } ], "eprint_id": 3330, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5850" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5850" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5850" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/30", "datestamp": "2008-09-11", "lastmod": "2021-04-16 23:06:04", "status_changed": "2009-09-25 02:56:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hoessel-J-G", "name": { "family": "Hoessel", "given": "John Greg" }, "show_email": "NO" } ] }, "title": "The photometric properties of brightest cluster galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nPhotometry of a large sample of first-ranked cluster galaxies, obtained with SIT and CCD area photometers, is discussed. The absolute photometric results anchor the bright end of the Hubble diagram; essentially the entire formal error for the method is now due to the distant clusters used. New determinations of the systematic trend of galaxy absolute magnitude with the cluster properties of richness and Bautz-Morgan type are derived.\n\nStructural properties of the galaxies are derived from the surface photometric observations. All the structure data support and are interpreted on the dynamical friction evolution model. Twenty-eight percent of the galaxies have multiple component nuclei; the short lifetimes of such systems provide the best available evidence that ongoing evolution actually occurs. Average magnitude and structure evolution rates are derived and used to estimate corrections to the value of q[subscript o] derived from the Hubble diagram. When combined with the expected rate of evolution of the stellar population in the galaxies and accounting for known selection effects in the sample, a true value near the formal value of q[subscript o] = -0.5 is indicated, suggesting an open universe.\n\nCorrelation of the absolute magnitudes with galaxy structure may be used to eliminate the magnitude dependence on cluster richness and Bautz-Morgan type, and remove the bias introduced into cluster samples by selection procedures. After removal of the trend due to differences in their volution the dispersion in the magnitudes of those brightest cluster galaxies is reduced to \u03c3 = 0[...]21 and the scatter in their core radii is \u03c3 = 22%.\n", "date": "1980", "date_type": "degree", "id_number": "CaltechETD:etd-09042008-141201", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09042008-141201", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-11", "doi": "10.7907/2nws-1w21", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Gunn-J-E", "name": { "family": "Gunn", "given": "James E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-04", "thesis_defense_date": "1979-11-08", "thesis_approved_date": "2008-09-11", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1980", "author_list": "Hoessel, John Greg" }, { "id": "/id/eprint/10058", "eprint_id": 10058, "rev_number": 22, "documents": [ { "id": "/id/document/76334", "doc_id": 76334, "rev_number": 3, "files": [ { "id": "/id/file/216179", "fileid": 216179, "datasetid": "document", "objectid": 76334, "filename": "Zimmermann_ME_1980.pdf", "mime_type": "application/pdf", "hash": "2d9bddb14d00fd21a96117934b41d889", "hash_type": "MD5", "filesize": 51291870, "mtime": "2017-02-17 22:47:11", "url": "/10058/1/Zimmermann_ME_1980.pdf" } ], "eprint_id": 10058, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Zimmermann_ME_1980.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/76334" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/01/00/58", "datestamp": "2017-02-18 00:06:30", "lastmod": "2022-11-09 19:20:08", "status_changed": "2017-02-18 00:06:30", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zimmermann-Mark-Edward", "name": { "family": "Zimmermann", "given": "Mark Edward" } } ] }, "title": "Studies on Gravitational Waves and Stars with Neutron Cores", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis reports on investigations in two major areas: astrophysics\r\nand relativity. It is divided into six independent chapters.
\r\n\r\nChapter I contains estimates of the astrophysically-likely amplitude\r\nof gravitational radiation emitted by the Crab and Vela pulsars. For\r\nmy analysis, I model the pulsars as rapidly-rotating, freely-precessing,\r\nrigid or elastic solid bodies. I find that the Crab is likely to produce\r\ngravitational waves at Earth with dimensionless amplitude 10-27\u00b12, and\r\nthat Vela is likely to give waves one or two orders of magnitude larger.
\r\n\r\nChapters II and III study the gravitational radiation produced by\r\nan idealized rotating and freely-precessing rigid body in the weak-field,\r\nslow-motion, small-stresses, quadrupole-moment formalism. Chapter II gives\r\nthe results for axisymmetric objects and for arbitrarily shaped objects\r\nundergoing small-angle precession. In that chapter, I also discuss the\r\napplication of my results to neutron stars in nature, and I describe in\r\ndetail how to analyze the incoming waves and extract information about\r\ntheir source. Chapter III extends the analysis of Chapter II to the\r\ngeneral case of an arbitrary rigid body undergoing large-angle precession.
\r\n\r\nChapter IV considers all astrophysically-reasonable sources of\r\ngravitational waves. Based on a minimal set of \"cherished beliefs\" about\r\nthe universe and about gravitation, I give general upper limits to the\r\nexpected intensity of gravitational radiation at the earth, at various\r\nfrequencies and from a variety of sources.
\r\n\r\nChapter V examines a \"natural\" coordinate system which might be set\r\nup by a rotating and accelerating observer. I expand the metric through\r\nsecond-order terms in distance from the origin of the coordinates; from\r\nthe metric, I derive the equations of motion for test particles. I\r\nidentify many forces and pseudoforces in the equations of motion, and\r\nI discuss how my results may be used to analyze some laboratory gravitational\r\nexperiments.
\r\n\r\nChapter VI of this thesis is a report on my results in studying nucleo-synthesis\r\nin stars with neutron-star cores. I was not able to generate\r\nany self-consistent models with a total mass of 16 M\u2299, core mass of 1 M\u2299,\r\n\r\nand core radius of 10 km; nuclear reactions fell short of producing the\r\nneeded luminosity by a factor of 25 or more. I describe in detail my\r\nmodeling procedures and the reasons for the failure of nucleosynthesis,\r\nand I point out extensions and modifications of my models which may be\r\nmore successful.
\r\n\r\n", "date": "1980", "date_type": "degree", "id_number": "CaltechTHESIS:02172017-144352834", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:02172017-144352834", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Schlumberger Corporation" }, { "agency": "State of California" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-02-18 00:06:30", "doi": "10.7907/n4hc-5489", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1979-12-10", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1980", "author_list": "Zimmermann, Mark Edward" }, { "id": "/id/eprint/3332", "eprint_id": 3332, "rev_number": 8, "documents": [ { "id": "/id/document/5852", "doc_id": 5852, "rev_number": 3, "files": [ { "id": "/id/file/34737", "fileid": 34737, "datasetid": "document", "objectid": 5852, "filename": "Kent_s_1980.pdf", "mime_type": "application/pdf", "filesize": 6479903, "mtime": "2012-12-26 02:59:08", "url": "/3332/1/Kent_s_1980.pdf" } ], "eprint_id": 3332, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Kent_s_1980.pdf", "language": "en", "security": "public", "license": "other", "main": "Kent_s_1980.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22393" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22393" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22393" } ] } }, { "id": "/id/document/22393", "doc_id": 22393, "rev_number": 3, "files": [ { "id": "/id/file/34735", "fileid": 34735, "datasetid": "document", "objectid": 22393, "filename": "preview.png", "mime_type": "image/png", "hash": "4f24d3affdc4be916a6d13283e63f530", "hash_type": "MD5", "filesize": 9389, "mtime": "2012-12-26 02:59:08", "url": "/3332/2/preview.png" } ], "eprint_id": 3332, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5852" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5852" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5852" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/32", "datestamp": "2008-09-11", "lastmod": "2021-04-16 23:00:23", "status_changed": "2009-09-25 02:56:51", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kent-S-M", "name": { "family": "Kent", "given": "Stephen Matthew" }, "show_email": "NO" } ] }, "title": "Interactions between galaxies and a hot medium in rich clusters", "ispublished": "unpub", "full_text_status": "public", "abstract": "The influence of a hot medium on the formation and evolution of galaxies in rich clusters is investigated. Part I begins with an observational study of the two peculiar systems of emission line filaments around the galaxy NGC1275 in the Perseus cluster. It is concluded that one system consists of condensations in an accretion flow from a surrounding medium onto an underlying elliptical galaxy while the second system arises in a superposed but unrelated spiral galaxy. Part II investigates the problem of whether SO galaxies can be formed by the ram pressure sweeping of spirals due to their motion through a hot intracluster medium. It is found that while the ram pressure may do considerable damage to spirals it is too weak by a large factor to produce the required numbers of S0's. In Part III observations of emission lines from spiral galaxies in the x-ray cluster A1367 reveal that they are deficient in gas content relative to field galaxies and this deficiency is strongest for galaxies closest to the region of x-ray emission. This is taken as evidence that spirals can lose a significant fraction of their gas content by interaction with a hot medium and is therefore a manifestation of the considerable damage predicted in Part II. Finally in Part IV the systematic trends in morphological populations observed in clusters are explained as resulting from a truncation of disks in spirals and SO's during their formation due to cluster collapse. Remarkably good agreement is obtained between the predictions of this scenario and a number of observed properties of galaxies in clusters.\n", "date": "1980", "date_type": "degree", "id_number": "CaltechETD:etd-09042008-145134", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09042008-145134", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-11", "doi": "10.7907/msvj-7y70", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-04", "thesis_defense_date": "1979-11-29", "thesis_approved_date": "2008-09-11", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1980", "author_list": "Kent, Stephen Matthew" }, { "id": "/id/eprint/849", "eprint_id": 849, "rev_number": 27, "documents": [ { "id": "/id/document/1274", "doc_id": 1274, "rev_number": 3, "files": [ { "id": "/id/file/8000", "fileid": 8000, "datasetid": "document", "objectid": 1274, "filename": "Nicholson_pd_1979.pdf", "mime_type": "application/pdf", "filesize": 6541142, "mtime": "2012-12-26 02:32:55", "url": "/849/1/Nicholson_pd_1979.pdf" } ], "eprint_id": 849, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Nicholson_pd_1979.pdf", "language": "en", "security": "internal", "license": "other", "main": "Nicholson_pd_1979.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/106446" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/106446" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/08/49", "datestamp": "2006-03-03", "lastmod": "2020-04-16 17:05:22", "status_changed": "2009-09-25 01:47:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nicholson-Philip-David", "name": { "family": "Nicholson", "given": "Philip David" }, "orcid": "0000-0003-2275-4463", "show_email": "NO" } ] }, "title": "1. Tidal Synchronization of the Rotation of Early Main Sequence Stars in Close Binaries. 2. The Rings of Uranus: Results of the 1978 April 10 Occultation. 3. On the Resonance Theory of the Rings of Uranus", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science; Astronomy", "note": "Title listed in 1979 commencement program -- I. Tidal Synchronization of the Rotation of Early Main Sequence Stars in Close Binaries. II. The Rings of Uranus: Results of the 1978 April 10 Occultation. III. On the Resonance Theory of the Rings of Uranus -- differs from title listed in thesis file (PDF).", "abstract": "Part 1:
\r\n\r\nThe rotational synchronization of an early type main sequence star in a close binary system has been attributed to radiative damping of the dynamical component of the tide raised in the star by its companion (Zahn, 1975, 1977). An investigation of the dynamical tide is presented here, which includes the heretofore neglected effects of stellar rotation. Foremost among these effects is the splitting of the tidal response into a set of modes whose latitudinal structures are controlled by the solutions of Laplace's tidal equation.
\r\n\r\nAn approximate analytic expression is derived for the rate of tidal energy dissipation associated with each of these modes, which in turn determines the rate of synchronization of the star's rotation with its orbital motion. This analytic result is supported by a numerical analysis of the dynamical tide raised in a 5 M\u2299 star. Combination of analytic and numerical results yields synchronization timescales for stars in the mass range 2 M\u2299 - 10 M\u2299. These timescales are a factor of 10 shorter than those obtained by Zahn, and are in good agreement with the observational data concerning synchronism among early type stars in close binaries. It is suggested, however, that the final stages of synchronization are controlled by another mechanism: the slow stellar expansion which accompanies the later stages of main sequence evolution.
\r\n\r\nPart 2:
\r\n\r\nObservations of the 1978 April 10 stellar occultation by the rings of Uranus are presented. Nine rings were observed and their radii and widths are calculated. Rings \u03b7, \u03b3, and \u03b4 are found to be most likely circular and coplanar, in agreement with previous analyses; the remaining rings are either non-circular or slightly inclined. The width of the \u03f5 ring is a linear function of its radius from the center of Uranus, projected onto the satellites' orbital plane; this suggests that it forms one continuous non-circular ring. The optical depth profile of the \u03f5 ring has not changed significantly since 1977 March. A model of this ring which fits all available observations adequately is that of a uniformly precessing Keplerian ellipse coplanar with the satellites' orbits. This model permits predictions of the radius and width of the \u03f5 ring for future occultations. The precession rate is used to determine J2 for Uranus, on the assumption that precession is caused solely by the planetary oblateness and not by satellite-ring interactions.
\r\n\r\nPart 3:
\r\n\r\nA three-body resonance model proposed to account for the rings of Uranus is quantitatively analyzed and found to be unacceptable on several grounds. Calculation of the strengths of two-body and three-body resonances involving all known satellites of Uranus, and which fall in the neighborhood of the rings, reveals that the strongest resonances are the 4:1 and 5:1 resonances with Miranda, and the three-body resonances involving Miranda and Ariel. Resonances invoked by the proposed model are much weaker. Despite the fact that four of these relatively strong resonances approximately coincide with rings 5, \u03b1, \u03b3, and \u03f5, they are too weak to explain the observed widths of the rings. Finally, the simple ring model of densely packed particles librating about a resonance is shown to be secularly unstable.
", "date": "1979", "date_type": "degree", "id_number": "CaltechETD:etd-03032006-160754", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03032006-160754", "related_url": { "items": [ { "description": "Article adapted for Section 3.", "type": "doi", "url": "https://doi.org/10.1038/269783b0" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NGL 05-002-003 " }, { "agency": "NASA", "grant_number": "NGL 05-002-140" }, { "agency": "NASA", "grant_number": "NGL 05-002-207" }, { "agency": "NSF", "grant_number": "AST 76-22676" }, { "agency": "NSF", "grant_number": "AST 77-20516" }, { "agency": "NSF", "grant_number": "AST 76-24281" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-03-03", "doi": "10.7907/xtcv-p562", "alt_title": { "items": [ "Tidal Synchronization of the Rotation of Early Main Sequence Stars in Close Binaries", "The Rings of Uranus: Results of the 1978 April 10 Occultation", "The Rings of Uranus", "Results of the 1978 April 10 Occultation", "On the Resonance Theory of the Rings of Uranus", "I. Tidal Synchronization of the Rotation of Early Main Sequence Stars in Close Binaries. II. The Rings of Uranus: Results of the 1978 April 10 Occultation. III. On the Resonance Theory of the Rings of Uranus" ] }, "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-03-03", "thesis_defense_date": "1978-09-25", "thesis_approved_date": "2006-03-03", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1979", "author_list": "Nicholson, Philip David" }, { "id": "/id/eprint/3331", "eprint_id": 3331, "rev_number": 11, "documents": [ { "id": "/id/document/5851", "doc_id": 5851, "rev_number": 3, "files": [ { "id": "/id/file/34730", "fileid": 34730, "datasetid": "document", "objectid": 5851, "filename": "Cimerman_m_1980.pdf", "mime_type": "application/pdf", "filesize": 2558298, "mtime": "2012-12-26 02:59:08", "url": "/3331/1/Cimerman_m_1980.pdf" } ], "eprint_id": 3331, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Cimerman_m_1980.pdf", "language": "en", "security": "public", "license": "other", "main": "Cimerman_m_1980.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22392" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22392" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22392" } ] } }, { "id": "/id/document/22392", "doc_id": 22392, "rev_number": 3, "files": [ { "id": "/id/file/34728", "fileid": 34728, "datasetid": "document", "objectid": 22392, "filename": "preview.png", "mime_type": "image/png", "hash": "80b398d5dcd8821d92aadec7f9f037bb", "hash_type": "MD5", "filesize": 8699, "mtime": "2012-12-26 02:59:08", "url": "/3331/2/preview.png" } ], "eprint_id": 3331, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5851" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5851" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5851" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/31", "datestamp": "2008-09-11", "lastmod": "2021-04-16 23:06:26", "status_changed": "2009-09-25 02:56:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cimerman-M", "name": { "family": "Cimerman", "given": "Menachem" }, "show_email": "NO" } ] }, "title": "A study of hydroxyl masers in the circumstellar envelopes of long period variable stars", "ispublished": "unpub", "full_text_status": "public", "abstract": "The 18 cm wavelength maser radiation from long period variable (LPV) stars is emitted by hydroxyl (OH) molecules in the expanding circumstellar envelopes. The four possible transitions within the ground state of the OH molecule are divided into two groups: mainlines at 1665 and 1667 MHz and satellite lines at 1612 and 1720 MHz. Three of these lines are observed in maser radiation from LPV stars: the 1612 MHz line and the mainlines. The observed properties of the 1612 MHz radiation are easier to interpret than those of the mainlines due to the quantum mechanical symmetries of the OH molecule. This investigation tackles the problem of the OH mainline masers, first by radio observations of two LPV sources with unique OH properties, and then by a theoretical analysis.\n\nThe U Ori OH masers were monitored following the drastic events in these masers in early 1974. The events consisted of the sudden appearance of strong 1612 MHz radiation, coincident with the disappearance of the 1667 MHz radiation. They are interpreted in light of the monitored evolution of the 1612 MHz radiation, the decline in its output level, and the subsequent re-emergence of a 1667 MHz line. The conclusion is that the events are the outcome of a short-lived disturbance in the stellar photosphere, most likely a shock-wave, which affected the maser through radiative coupling between the photosphere and the OH molecules.\n\nObservations of the OH maser in W Hya are presented, which suggest an explanation of their unique polarization characteristics. The maser lines may be formed at a distance of ~ 10[superscript 14] cm from the stellar surface in the presence of a magnetic field of ~ 9 milligauss. This magnetic field is coupled to the ionized component of the outflowing circumstellar envelope. In the W Hya case the magnetic field is evident in the strong polarization, Zeeman pattern and differential magnetorotation. However, it may exist unnoticed in other OH sources, and contribute to the pumping mechanism.\n\nThe pumping of OH masers in late-type-variables by direct stellar radiation of 2.8\u03bc is studied. Two pumping schemes are suggested based on line coincidences between OH V=0-1 transitions and strong H[subscript 2]0 \u03c5[subscript 3] transitions. The water molecules perturb the stellar radiation by absorption, and thus cool the coinciding OH transition. It is demonstrated that this cooling is capable of producing strong OH masers in the circumstellar envelopes of late-type-variables. This model can account for the existence of mainline (\u0394F=0) OH masers, which is hard to explain otherwise.\n", "date": "1979", "date_type": "degree", "id_number": "CaltechETD:etd-09042008-141513", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09042008-141513", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-11", "doi": "10.7907/zsta-x423", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" }, { "id": "Wannier-P-G", "name": { "family": "Wannier", "given": "Peter G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "chair" }, { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Wannier-P-G", "name": { "family": "Wannier", "given": "Peter G." }, "role": "member" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "Nicholas Zabriskie" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-04", "thesis_defense_date": "1979-05-09", "thesis_approved_date": "2008-09-11", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1979", "author_list": "Cimerman, Menachem" }, { "id": "/id/eprint/9621", "eprint_id": 9621, "rev_number": 22, "documents": [ { "id": "/id/document/64324", "doc_id": 64324, "rev_number": 3, "files": [ { "id": "/id/file/180013", "fileid": 180013, "datasetid": "document", "objectid": 64324, "filename": "Caves_cm_1979.pdf", "mime_type": "application/pdf", "hash": "41dee6359fb717420fc6f9484dca488e", "hash_type": "MD5", "filesize": 99323420, "mtime": "2016-03-15 23:13:24", "url": "/9621/1/Caves_cm_1979.pdf" } ], "eprint_id": 9621, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Caves_cm_1979.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"disk0/00/00/96/21", "datestamp": "2016-03-16 20:18:17", "lastmod": "2022-11-09 19:20:08", "status_changed": "2016-03-16 20:18:17", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ccaves@unm.edu", "id": "Caves-Carlton-Morris", "name": { "family": "Caves", "given": "Carlton Morris" }, "show_email": "YES" } ] }, "title": "Theoretical investigations of experimental gravitation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This thesis has two basic themes: the investigation of new experiments\r\nwhich can be used to test relativistic gravity, and the investigation of new\r\ntechnologies and new experimental techniques which can be applied to make\r\ngravitational wave astronomy a reality.
\r\n\r\nAdvancing technology will soon make possible a new class of gravitation\r\nexperiments: pure laboratory experiments with laboratory sources of non-Newtonian\r\ngravity and laboratory detectors. The key advance in techno1ogy\r\nis the development of resonant sensing systems with very low levels of dissipation.\r\nChapter 1 considers three such systems (torque balances, dielectric\r\nmonocrystals, and superconducting microwave resonators), and it proposes\r\neight laboratory experiments which use these systems as detectors. For each\r\nexperiment it describes the dominant sources of noise and the technology\r\nrequired.
\r\n\r\nThe coupled electro-mechanical system consisting of a microwave cavity\r\nand its walls can serve as a gravitational radiation detector. A gravitational \r\nwave interacts with the walls, and the resulting motion induces\r\ntransitions from a highly excited cavity mode to a nearly unexcited mode.\r\nChapter 2 describes briefly a formalism for analyzing such a detector, and\r\nit proposes a particular design.
\r\n\r\nThe monitoring of a quantum mechanical harmonic oscillator on which a\r\nclassical force acts is important in a variety of high-precision experiments,\r\nsuch as the attempt to detect gravitational radiation. Chapter 3 reviews\r\nthe standard techniques for monitoring the oscillator; and it introduces a\r\nnew technique which, in principle, can determine the details of the force\r\nwith arbitrary accuracy, despite the quantum properties of the oscillator.
\r\n\r\nThe standard method for monitoring the oscillator is the \"amplitude-\r\nand-phase\" method (position or momentum transducer with output fed through\r\na linear amplifier). The accuracy obtainable by this method is limited by\r\nthe uncertainty principle. To do better requires a measurement of the type\r\nwhich Braginsky has called \"quantum nondemolition.\" A well-known quantum\r\nnondemolition technique is \"quantum counting,\" which can detect an arbitrarily\r\nweak force, but which cannot provide good accuracy in determining\r\nits precise time-dependence. Chapter 3 considers extensively a new type\r\nof quantum nondemolition measurement - a \"back-action-evading\" measurement\r\nof the real part X1 (or the imaginary part X2) of the oscillator's complex\r\namplitude. In principle X1 can be measured arbitrarily quickly and arbitrarily\r\naccurately, and a sequence of such measurements can lead to an\r\narbitrarily accurate monitoring of the classical force.
\r\n\r\nChapter 3 describes explicit gedanken experiments which demonstrate that\r\nX1 can be measured arbitrarily quickly and arbitrarily accurately, it considers\r\napproximate back-action-evading measurements, and it develops a theory\r\nof quantum nondemolition measurement for arbitrary quantum mechanical systems.
\r\n\r\nIn Rosen's \"bimetric\" theory of gravity the (local) speed of gravitational\r\nradiation vg is determined by the combined effects of cosmological\r\nboundary values and nearby concentrations of matter. It is possible for vg\r\nto be less than the speed of light. Chapter 4 shows that emission of gravitational\r\nradiation prevents particles of nonzero rest mass from exceeding the\r\nspeed of gravitational radiation. Observations of relativistic particles\r\nplace limits on vg and the cosmological boundary values today, and observations\r\nof synchrotron radiation from compact radio sources place limits on\r\nthe cosmological boundary values in the past.
", "date": "1979", "date_type": "degree", "id_number": "CaltechTHESIS:03152016-161054898", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03152016-161054898", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Feynman Fellowship" }, { "agency": "NASA" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2016-03-16 20:18:17", "doi": "10.7907/H3T8-FQ06", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" }, { "id": "Drever-R-W-P", "name": { "family": "Drever", "given": "Ronald W. P." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1979-05-08", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1979", "author_list": "Caves, Carlton Morris" }, { "id": "/id/eprint/3314", "eprint_id": 3314, "rev_number": 8, "documents": [ { "id": "/id/document/5834", "doc_id": 5834, "rev_number": 3, "files": [ { "id": "/id/file/34603", "fileid": 34603, "datasetid": "document", "objectid": 5834, "filename": "Young_pj_1979.pdf", "mime_type": "application/pdf", "filesize": 4342977, "mtime": "2012-12-26 02:59:01", "url": "/3314/1/Young_pj_1979.pdf" } ], "eprint_id": 3314, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Young_pj_1979.pdf", "language": "en", "security": "public", "license": "other", "main": "Young_pj_1979.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22375" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22375" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22375" } ] } }, { "id": "/id/document/22375", "doc_id": 22375, "rev_number": 3, "files": [ { "id": "/id/file/34601", "fileid": 34601, "datasetid": "document", "objectid": 22375, "filename": "preview.png", "mime_type": "image/png", "hash": "9589a5c59e7eacc1ec7be882355ae61e", "hash_type": "MD5", "filesize": 8540, "mtime": "2012-12-26 02:59:01", "url": "/3314/2/preview.png" } ], "eprint_id": 3314, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5834" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5834" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5834" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/14", "datestamp": "2008-09-09", "lastmod": "2021-04-16 23:10:55", "status_changed": "2009-09-25 02:56:38", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Young-P-J", "name": { "family": "Young", "given": "Peter John" }, "show_email": "NO" } ] }, "title": "Supermassive black holes in galactic nuclei", "ispublished": "unpub", "full_text_status": "public", "abstract": "The existence of supermassive black holes in galactic nuclei is investigated both theoretically and observationally. In addition the dynamics of flattened elliptical galaxies is examined observationally. Part I of the thesis deals with the theoretical distribution of a stellar population around a massive black hole in a galactic nucleus. Part II calculates the luminous energy output such a black hole could achieve by wreaking carnage among the stars in that nucleus. Part III is a photometric study of the radio galaxy M87 and concludes that this galaxy harbours some sort of massive object, if not a black hole. Part IV is a dynamical stud of the same galaxy M87 via spectroscopic measurements of the velocity dispersion as a function of radius. It comes to the same conclusion as in Part III. Part V is a study of the dynamics of the E5 galaxy NGC 4473 which is found to exhibit scant rotation.\n", "date": "1979", "date_type": "degree", "id_number": "CaltechETD:etd-09022008-144208", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09022008-144208", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/mcgd-jp70", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-02", "thesis_defense_date": "1978-07-10", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1979", "author_list": "Young, Peter John" }, { "id": "/id/eprint/3342", "eprint_id": 3342, "rev_number": 10, "documents": [ { "id": "/id/document/5863", "doc_id": 5863, "rev_number": 3, "files": [ { "id": "/id/file/34814", "fileid": 34814, "datasetid": "document", "objectid": 5863, "filename": "Romney_jdm_1979.pdf", "mime_type": "application/pdf", "filesize": 3258298, "mtime": "2012-12-26 02:59:13", "url": "/3342/1/Romney_jdm_1979.pdf" } ], "eprint_id": 3342, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Romney_jdm_1979.pdf", "language": "en", "security": "public", "license": "other", "main": "Romney_jdm_1979.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22403" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22403" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22403" } ] } }, { "id": "/id/document/22403", "doc_id": 22403, "rev_number": 3, "files": [ { "id": "/id/file/34812", "fileid": 34812, "datasetid": "document", "objectid": 22403, "filename": "preview.png", "mime_type": "image/png", "hash": "5d844b2edc16fa2c009ff93f368711b1", "hash_type": "MD5", "filesize": 9502, "mtime": "2012-12-26 02:59:13", "url": "/3342/2/preview.png" } ], "eprint_id": 3342, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5863" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5863" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5863" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/42", "datestamp": "2008-09-09", "lastmod": "2021-04-16 22:11:53", "status_changed": "2009-09-25 02:56:58", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Romney-J-D-M", "name": { "family": "Romney", "given": "Jonathan Daniel MacLeish" }, "show_email": "NO" } ] }, "title": "Fine-scale structure of the neutral hydrogen absorption in NGC1275", "ispublished": "unpub", "full_text_status": "public", "abstract": "The high-velocity 21-cm absorption feature in NGC1275 (=3C84) has been mapped at an angular resolution of a few milliarcseconds with an intercontinental very-long-baseline interferometer. The method of analysis makes use of both the absolute amplitude of the visibility function in the continuum, and the relative amplitude and phase between the line and continuum.\r\n\r\nFine-scale structure in the continuum is determined from the observations, and the 21-cm structure of 3C84 on angular scales covering almost six orders of magnitude is reviewed.\r\n\r\nThe HI absorption is found to arise in a cloud covering part of the intense, compact continuum nucleus. Although absorption is seen against the brightest part of the continuum structure, the cloud is displaced to the northeast from the nucleus, reaching optical depths of at least 0.83. The cloud is at least 5.6 pc in diameter, with a deduced volume density between 12 and 120 cm[superscript -3].\r\n\r\nTwo basic hypotheses which have been advanced to elucidate the 21-cm absorption and other high-velocity features in NGC1275 are discussed. The results of the present investigation strongly support the interpretation that all the high-velocity features arise in a superposed galaxy in the Perseus Cluster. The alternative model, in which the high-velocity gas is ejected from the active nucleus, is inconsistent with the structure observed in the HI absorption.\r\n", "date": "1979", "date_type": "degree", "id_number": "CaltechETD:etd-09052008-131956", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09052008-131956", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/ytaj-x179", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-05", "thesis_defense_date": "1978-06-21", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1979", "author_list": "Romney, Jonathan Daniel MacLeish" }, { "id": "/id/eprint/3412", "eprint_id": 3412, "rev_number": 9, "documents": [ { "id": "/id/document/5947", "doc_id": 5947, "rev_number": 3, "files": [ { "id": "/id/file/35386", "fileid": 35386, "datasetid": "document", "objectid": 5947, "filename": "LaBonte_bj_1979.pdf", "mime_type": "application/pdf", "filesize": 30562760, "mtime": "2012-12-26 02:59:44", "url": "/3412/1/LaBonte_bj_1979.pdf" } ], "eprint_id": 3412, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "LaBonte_bj_1979.pdf", "language": "en", "security": "public", "license": "other", "main": "LaBonte_bj_1979.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22487" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22487" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22487" } ] } }, { "id": "/id/document/22487", "doc_id": 22487, "rev_number": 3, "files": [ { "id": "/id/file/35384", "fileid": 35384, "datasetid": "document", "objectid": 22487, "filename": "preview.png", "mime_type": "image/png", "hash": "c7e0725becd48c1827e080bb407cf03d", "hash_type": "MD5", "filesize": 8857, "mtime": "2012-12-26 02:59:44", "url": "/3412/2/preview.png" } ], "eprint_id": 3412, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5947" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5947" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5947" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/12", "datestamp": "2008-09-17", "lastmod": "2021-04-19 22:28:36", "status_changed": "2009-09-25 02:58:02", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "LaBonte-Barry-James", "name": { "family": "LaBonte", "given": "Barry James" }, "show_email": "NO" } ] }, "title": "Studies of Chromospheric Activity Observed in H\u03b1 and D\u2083", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Several studies of chromospheric activity as observed in H\u03b1 and D3 have been made. These are: H\u03b1 Observations of the August 12, 1975 Type III-RS Bursts (Solar Physics, 50, 201, 1976); A Measurement of the Helium D3 Profile with a Birefringent Filter (Solar Physics, 53, 369, 1977); The Properties of Macrospicules Observed in H\u03b1 and D3 (Big Bear Solar Observatory Preprint No. 0171); Polar Flares with D3 Emission: November 15, 1974 (Big Bear Solar Observatory Preprint No. 0170); and Thick Target Models of Impulsive Chromospheric Flares (Big Bear Solar Observatory Preprint No. 0173).\r\n", "date": "1979", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-112830", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-112830", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-17", "doi": "10.7907/wv44-e526", "alt_title": { "items": [ "Studies of Chromospheric Activity Observed in Halpha and D3" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1978-06-23", "thesis_approved_date": "2008-09-17", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1979", "author_list": "LaBonte, Barry James" }, { "id": "/id/eprint/3377", "eprint_id": 3377, "rev_number": 14, "documents": [ { "id": "/id/document/5907", "doc_id": 5907, "rev_number": 4, "files": [ { "id": "/id/file/35117", "fileid": 35117, "datasetid": "document", "objectid": 5907, "filename": "Sargent_ai_1978.pdf", "mime_type": "application/pdf", "filesize": 4158368, "mtime": "2012-12-26 02:59:29", "url": "/3377/1/Sargent_ai_1978.pdf" } ], "eprint_id": 3377, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Scanned, no OCR. 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clouds. An extended (20 pc x 60 pc) molecular cloud was detected and mapped, and additional observations of 13CO and H2CO were made at selected positions. The total mass of the cloud is 5 x 103 M\u2609. A range of velocities is seen over the cloud complex. This is comparable with the stellar velocities in the association.
\r\n\r\nWithin the molecular cloud are found three regions in which different stages of star formation are identified. In one an embedded star may be present. Another appears to be collapsing on a time scale of ~3 x 105 years to form a new subgroup of the OB association. The mass of this region, 500 M\u2609, is sufficient to produce only the number of O and B stars typically found in association subgroups, suggesting that lower mass stars must form under different conditions. The third displays signs of enhanced density and is probably the precursor of a star forming region. All three regions are situated in that part of the molecular cloud which is closest to the association stars.
\r\n\r\nThe membership and ages of the subgroups of the Cepheus OB3 association have been re-examined, and their places of origin determined. Ages of 1-3 x 105 years and 5-7 x 105 years are found for younger and older subgroups respectively. Their birthplaces are not coincident but are situated at that end of the cloud where star formation still appears to be taking place. The younger subgroup appears to have formed closer to the active regions than did the older subgroup, so that there is a well-defined age sequence across the association which continues into the cloud.
\r\n\r\nThere is currently little direct interaction between the stars and the molecular cloud, although a few younger subgroup stars still lie close to or within the complex. The absence of primeval gas in the environs of the older subgroup is attributed to the unusually high velocity of separation between these stars and the cloud.
\r\n\r\nIt appears that the younger and still-forming subgroups of Cepheus OB3 are created in a different way from the older subgroup. However, the way in which star formation is initiated in this association remains uncertain.
\r\n", "date": "1978", "date_type": "degree", "id_number": "CaltechETD:etd-09082004-115311", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082004-115311", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department", "Caltech Distinguished Alumni Award" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-09-08", "doi": "10.7907/XZSK-2H71", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-09-08", "thesis_defense_date": "1977-10-14", "thesis_approved_date": "2004-09-08", "thesis_awards": "Caltech Distinguished Alumni Award, 2019", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1978", "author_list": "Sargent, Anneila Isabel" }, { "id": "/id/eprint/10406", "eprint_id": 10406, "rev_number": 22, "documents": [ { "id": "/id/document/82351", "doc_id": 82351, "rev_number": 4, "files": [ { "id": "/id/file/232656", "fileid": 232656, "datasetid": "document", "objectid": 82351, "filename": "De Logi_wk_1978.zip", "mime_type": "application/x-zip", "hash": "45e59299365fad783f77fb5921b29efe", "hash_type": "MD5", "filesize": 66315032, "mtime": "2017-08-31 22:02:38", "url": "/10406/1/De Logi_wk_1978.zip" } ], "eprint_id": 10406, "pos": 1, "placement": 1, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "De Logi_wk_1978.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": 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"userid": 87, "dir": "disk0/00/01/04/06", "datestamp": "2017-08-31 22:31:16", "lastmod": "2021-04-16 23:14:12", "status_changed": "2017-08-31 22:31:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "De-Logi-Walter-K", "name": { "family": "De Logi", "given": "Walter K." } } ] }, "title": "Electromagnetic Wave Generation and Propagation in Gravitational Fields", "ispublished": "unpub", "full_text_status": "public", "keywords": "Electrical Engineering", "abstract": "We use Feynman perturbation techniques to analyze some aspects\r\nof electromagnetic wave generation and propagation in weak gravitational\r\nfields.
\r\n\r\nIn the first part of this report we calculate differential \r\ncross sections d\u03c3/d\u03a9 for the scattering of plane electromagnetic\r\nwaves by weakly gravitating and rotating bodies in the long-wavelength \r\nlimit (wavelength of incident radiation >> radius of scatterer >> mass \r\nof scatterer). We find that the polarization of right (or left) \r\ncircularly polarized electromagnetic waves is unaffected by the \r\nscattering process (i.e., helicity is conserved), and that the two \r\nhelicity states of the photon are scattered differently by a rotating \r\nbody. This coupling between the photon helicity and the angular \r\nmomentum of the scatterer also leads to a partial polarization of \r\nunpolarized incident light.
\r\n\r\n\r\nFor the sake of comparison, we also compute the differential \r\ncross sections for the gravitational scattering of scalar and gravi\u00adtational \r\nwaves. For the latter there is neither helicity conservation \r\nnor helicity-dependent scattering; and the angular momentum has no \r\npolarizing effect on incident, unpolarized gravitational waves.
\r\n\r\nIn the second part of this report, we analyze the conversion \r\nof gravitational waves into electromagnetic waves (and vice versa) \r\nunder the \"catalytic\" action of a static electromagnetic background \r\nfield. Closed-form differential cross sections are presented for \r\nconversion in the Coulomb field of a point charge, electric and \r\nmagnetic dipole fields, and uniform electrostatic and magnetostatic \r\nfields. Using the model calculation of conversion in a Coulomb field, \r\nwe discuss the problems that we must face when calculating non-gauge\u00ad-invariant \r\ntransition amplitudes, as is frequently done in the litera\u00adture.
\r\n\r\n\r\nWe conclude this report by pointing out how charged-particle \r\nbeams may be used (in principle) as direction-sensitive gravitational\u00ad-wave detectors.
\r\n \r\n\r\n\r\n", "date": "1978", "date_type": "degree", "id_number": "CaltechTHESIS:08312017-150019175", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08312017-150019175", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-31 22:31:16", "doi": "10.7907/es3k-qv56", "divisions": { "items": [ "div_eng" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1978-03-28", "review_status": "approved", "option_major": { "items": [ "eleceng" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1978", "author_list": "De Logi, Walter K." }, { "id": "/id/eprint/3676", "eprint_id": 3676, "rev_number": 22, "documents": [ { "id": "/id/document/6278", "doc_id": 6278, "rev_number": 3, "files": [ { "id": "/id/file/37623", "fileid": 37623, "datasetid": "document", "objectid": 6278, "filename": "Alcock_c_1978.pdf", "mime_type": "application/pdf", "filesize": 3437991, "mtime": "2012-12-26 03:01:59", "url": "/3676/1/Alcock_c_1978.pdf" } ], "eprint_id": 3676, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Alcock_c_1978.pdf", "language": "en", "security": "internal", "license": "other", "main": "Alcock_c_1978.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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Small Angle Scattering of Radiation. II. Molecular Emission Lines Around Evolved Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy; Distance determination; Grains; Scattering; X-rays; X-ray bursts; Masers molecules; Circumstellar radiative transfer", "abstract": "This dissertation is in two Parts. Part I consists of a paper on the effect of small angle scattering on a pulse of radiation, and an analysis of the particular case of X-rays scattering off interstellar grains. Part II concerns the excitation of SiO emission lines around evolved stars. There are two papers, the first on 'thermal' emission lines and the second on maser emission lines. Each paper has its own abstract.
\r\n\r\nPart I: We have analyzed in detail the general problem of the propagation of a pulse of radiation through a uniform medium containing small angle scatterers. Simple expressions for the first moment of the arrival time delay and for the second and fourth moments of the arrival angle of the pulse photons are given, valid for any optical depth. Using the first two of these we find a simple method of distance determination. Joint and individual distribution functions for arrival time and angle are derived in the small and large optical depth limits. An exponential tail in the arrival time distribution is characteristic in both limits. The analysis has been applied to a burst of x-rays from a source near the galactic center propagating through the dust of the interstellar medium. The grains responsible for interstellar reddening can have very little observable effect. However, the observed lengths, energy dependence, and variability of the burst tails can be readily accounted for by a population of large ~3\u03bc grains. We derive useful constraints on the grain distribution from observations of the burst tails.
\r\n\r\nPart II (i): We have investigated the excitation of the microwave lines in the ground vibrational state of the SiO molecule in the expanding envelope of cool Mira-type stars. The rotational levels are excited when an SiO molecule absorbs an 8\u03bc photon and is left in the lowest excited vibrational state; the spontaneous decay of the excited vibrational state preferentially leaves the molecule with a higher rotational quantum number than it had before. In all of the cases investigated the majority of the microwave transitions were optically thick, and photon trapping causes the excitation temperature to increase with optical depth in such a way that the antenna temperature measured by a distant observer is proportional to the flux of SiO leaving the star, to the square root of the ambient 8\u03bc flux and inversely to the square of the asymptotic velocity. We have analysed the reported detection of J = 1 \u2192 2, v = 0 emission from three Miras and VY CMa, and find that the flux of SiO leaving the stars is very low. This indicates that either they are losing very little mass, or more probably that grain formation very effectively removes a large fraction of gaseous SiO molecules.
\r\n\r\nPart II (ii): We have investigated the excitation of the microwave lines in the excited vibrational states of the SiO molecules in the expanding envelopes of cool Mira-type stars. The excited vibrational states are populated principally by the absorption of 8\u03bc photons. The inversions occur when the gas temperature exceeds the excitation temperature of the vibrational levels, and upward vibrational collisions selectively populate higher rotational levels. The masers are all saturated. We discuss the line profiles, and show how the profile is determined by the velocity gradient and the ambient radiation field.
\r\n\r\nThe SiO abundance required for the masers is large. We discuss this in the light of our earlier calculation that the abundance is low in the outer envelope, and argue that grain formation is an efficient process.
\r\n", "date": "1978", "date_type": "degree", "id_number": "CaltechETD:etd-09212004-110141", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09212004-110141", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST76-80801" }, { "agency": "NSF", "grant_number": "MPS72-05045-A02" }, { "agency": "NSF", "grant_number": "AST73-04677-A03" } ] }, "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-09-21", "doi": "10.7907/9NC1-B853", "alt_title": { "items": [ "I. Small Angle Scattering of Radiation", "II. Molecular Emission Lines Around Evolved Stars", "Small Angle Scattering of Radiation", "Molecular Emission Lines Around Evolved Stars" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "id": "Garmire-G-P", "name": { "family": "Garmire", "given": "Gordon Paul" }, "role": "member" }, { "id": "Wannier-P-G", "name": { "family": "Wannier", "given": "Peter G." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-09-21", "thesis_defense_date": "1977-09-30", "thesis_approved_date": "2004-09-21", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1978", "author_list": "Alcock, Charles" }, { "id": "/id/eprint/3315", "eprint_id": 3315, "rev_number": 8, "documents": [ { "id": "/id/document/5835", "doc_id": 5835, "rev_number": 3, "files": [ { "id": "/id/file/34610", "fileid": 34610, "datasetid": "document", "objectid": 5835, "filename": "Elias_jh_1978.pdf", "mime_type": "application/pdf", "filesize": 5928834, "mtime": "2012-12-26 02:59:02", "url": "/3315/1/Elias_jh_1978.pdf" } ], "eprint_id": 3315, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Elias_jh_1978.pdf", "language": "en", "security": "public", "license": "other", "main": "Elias_jh_1978.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22376" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22376" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22376" } ] } }, { "id": "/id/document/22376", "doc_id": 22376, "rev_number": 3, "files": [ { "id": "/id/file/34608", "fileid": 34608, "datasetid": "document", "objectid": 22376, "filename": "preview.png", "mime_type": "image/png", "hash": "06f7e73ffae87ed254db9572c102476b", "hash_type": "MD5", "filesize": 7552, "mtime": "2012-12-26 02:59:02", "url": "/3315/2/preview.png" } ], "eprint_id": 3315, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5835" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5835" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5835" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/15", "datestamp": "2008-09-10", "lastmod": "2021-04-16 23:11:44", "status_changed": "2009-09-25 02:56:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Elias-J-H", "name": { "family": "Elias", "given": "Jonathan H." }, "show_email": "NO" } ] }, "title": "Infrared studies of two dark clouds", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThe IC5146 dark cloud complex has been surveyed in the infrared in order to identify and study associated young stellar objects. Most of the objects detected in the survey appear to be field stars, predominantly late-type giants. Three young objects were detected in the survey: The BO star BD+4[\u2026]3474, the Ae star BD+46[\u2026]3471, and a previously unidentified object which appears to be a heavily obscured FU Ori star. The properties of the last two objects are examined in detail, and an attempt is made to produce reasonable models for them. It is suggested that FU Ori stars are binaries, and some consequences of this model are described. Photometry of the brighter stars in the IC5146 cluster has been used to establish a distance to the cluster of 900 \u00b1 100 pc.\n\nA near-infrared survey has also been conducted of nearly 18 square degrees of the Ophiuchus dark cloud complex. Additional observations have been made of selected objects found in this survey and of the brighter objects found by Grasdalen et al. and by Vrba et al. in this region, in order to identify and study the young stars associated with the cloud. These observations show that very recent star formation has been largely restricted to a small region no more than a few parsecs in extent at the center of the dark cloud complex. Most of the young stars do not appear to be main sequence stars. At least three of these objects appear to be surrounded by infrared reflection nebulae. Many of the objects studied are background K and M giants which can be used to determine the near-infrared extinction due to the dark cloud.\n", "date": "1978", "date_type": "degree", "id_number": "CaltechETD:etd-09022008-145925", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09022008-145925", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/78t4-q193", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-02", "thesis_defense_date": "1978-02-03", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1978", "author_list": "Elias, Jonathan H." }, { "id": "/id/eprint/3746", "eprint_id": 3746, "rev_number": 7, "documents": [ { "id": "/id/document/6363", "doc_id": 6363, "rev_number": 2, "files": [ { "id": "/id/file/38199", "fileid": 38199, "datasetid": "document", "objectid": 6363, "filename": "Huchra_jp_1977.pdf", "mime_type": "application/pdf", "filesize": 4520214, "mtime": "2012-12-26 03:02:36", "url": "/3746/1/Huchra_jp_1977.pdf" } ], "eprint_id": 3746, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Huchra_jp_1977.pdf", "language": "en", "security": "public", "license": "other", "main": "Huchra_jp_1977.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22901" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22901" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22901" } ] } }, { "id": "/id/document/22901", "doc_id": 22901, "rev_number": 2, "files": [ { "id": "/id/file/38197", "fileid": 38197, "datasetid": "document", "objectid": 22901, "filename": "preview.png", "mime_type": "image/png", "hash": "e4afacb0adda489f9bfbf618ead2e46c", "hash_type": "MD5", "filesize": 9846, "mtime": "2012-12-26 03:02:36", "url": "/3746/2/preview.png" } ], "eprint_id": 3746, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6363" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6363" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6363" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/46", "datestamp": "2008-10-08", "lastmod": "2019-12-20 19:19:14", "status_changed": "2009-09-25 03:04:38", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Huchra-J-P", "name": { "family": "Huchra", "given": "John Peter" }, "show_email": "NO" } ] }, "title": "The nature of Markarian galaxies and studies of star formation in blue galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\n\nIntegrated UBV photometry is given for 197 non-Seyfert Markarian galaxies and is compared with existing photometry of field galaxies. The distributions of galaxy colors overlap by almost seventy-five percent, and the color-color relations are the same. The color-aperture relations derived from multi-aperture observations show that the Markarian galaxies generally get bluer towards their centers, unlike all but the latest types of field galaxies.\n\nThirteen binary galaxies with good radial velocity data are used to derive the mean minimum mass-to-light ratio for Markarian galaxies. It is the same as the mean minimum mass-to-light ratio for field binary galaxies.\n\nAll Markarian galaxies with m[subscript pg][...] 14.0 are morphologically classified in the modified Hubble sequence. The distibution of morphological types for Markarian galaxies is generally similar to that of field galaxies. The only significant difference is that the Markarian sample shows a factor of three excess of very late type galaxies. The Markarian galaxies are generally blue for their morphological type but fall within the distributions of colors for their field counterparts. The bluest types - Magellanic spirals and irregulars - extend 0.3 magnitude bluer in U-B than the bluest field galaxies.\n\nThe Markarian galaxy luminosity function is derived from the available data for all seven lists of objects. Markarian galaxies represent approximately one tenth of all galaxies with absolute magnitudes fainter than M[subscript pg] = -22 (H[subscript o] = 50 km sec[superscript -1] Mpc[superscript -1]). A crude estimate is made of the space density as a function of color for both Markarian and field galaxies. Markarian appears to be finding all galaxies with U-B < -0.3 plus a decreasing fraction of the redder galaxies.\n\nFor the Markarian galaxies with available data, there are strong correlations of the emission line strength, measured by H\u03b2 equivalent width, with color and absolute magnitude. There are also weaker correlations of the excitation parameter I([O III]\u03bb5007)/I(H\u03b2) with color.\n\nThe optical and radio data indicate that the non-Seyfert Markarian galaxies (85% of all Markarian objects) are not a new class of object but rather a subset of normal galaxies. Markarian selects the bluest galaxies and those galaxies which are blue for their morphological type.\n\nThe Markarian galaxy photometry and photometry of galaxies in the lists of Haro and Zwicky extend the observed galaxy two color distribution significantly bluewards. Existing evolutionary models of galaxy colors (Tinsley 1968, 1972; Searle, Sargent and Bagnuolo 1973) do not match the observed colors of these blue galaxies. Models of galaxies are constructed with a variety of star formation histories and initial mass functions. The models include the effects of emission by gas ionized by the hot stars in the galaxy.\n\nThree general classes of models were studied. 'Old' galaxies are systems that are more than 10[superscript 10] years old. 'Young' galaxies are systems that are less than one tenth that age. 'Composite' galaxies are 'old' galaxies, with properties similar to ordinary spirals and ellipticals, plus a burst of recent star formation. Powerlaw initial mass functions were used.\n\nIn order to fit the observed colors, 'old' galaxies must have high mass star enriched initial mass functions and nearly constant rates of star formation. 'Young' galaxies must have large amounts of internal reddening. If their initial mass function is the Salpeter function, they must be less than 10[superscript 8] years old. 'Composite' galaxies must have bursts of star formation that contribute approximately twenty to fifty percent of the V band light.\n\nComparison of model predictions with the observed metal abundance, color-magnitude distribution, and internal reddening lead us to conclude that 'composite' models best fit the observed properties. There is no compelling evidence for the existence of 'young' galaxies - objects only recently condensed out of the intergalactic medium.\n\nIn addition, comparison of model predictions with the observed H\u03b2 emission as a function of color in blue galaxies leads to the conclusion that some of these galaxies are forming stars with an initial mass function flatter than the Salpeter function.\n", "date": "1977", "date_type": "degree", "id_number": "CaltechETD:etd-09242008-110419", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09242008-110419", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-08", "doi": "10.7907/F34C-J170", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-24", "thesis_defense_date": "1976-07-14", "thesis_approved_date": "2008-10-08", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1977", "author_list": "Huchra, John Peter" }, { "id": "/id/eprint/10390", "eprint_id": 10390, "rev_number": 18, "documents": [ { "id": "/id/document/82190", "doc_id": 82190, "rev_number": 2, "files": [ { "id": "/id/file/232111", "fileid": 232111, "datasetid": "document", "objectid": 82190, "filename": "Kovacs jr._sj_1977.pdf", "mime_type": "application/pdf", "hash": "e2956569ced45e30a95c1a349b1b5d58", "hash_type": "MD5", "filesize": 33335438, "mtime": "2017-08-25 16:39:01", "url": "/10390/1/Kovacs jr._sj_1977.pdf" } ], "eprint_id": 10390, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Kovacs jr._sj_1977.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" 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"content": "final" }, { "id": "/id/document/133859", "doc_id": 133859, "rev_number": 1, "files": [ { "id": "/id/file/379304", "fileid": 379304, "datasetid": "document", "objectid": 133859, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "6472b3ed80c48d126703cfb2b9e97bfa", "hash_type": "MD5", "filesize": 35467, "mtime": "2021-06-24 20:16:06", "url": "/10390/8/indexcodes.txt" } ], "eprint_id": 10390, "pos": 8, "placement": 8, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/82190" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/82190" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/82190" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/01/03/90", "datestamp": "2017-08-25 20:23:08", "lastmod": "2020-03-10 23:39:09", "status_changed": "2017-08-25 20:23:08", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kov\u00e1cs-S\u00e1ndor-J\u00e1nos-Jr.", "name": { "family": "Kov\u00e1cs", "given": "S\u00e1ndor J\u00e1nos, Jr." } } ] }, "title": "The Generation of Gravitational Waves", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "This dissertation is written in three tracks. Track 1, (Pages ii-vi)\r\nis intended for those many many people who don't know any physics but who\r\ndo know how to read English and a bit of Hungarian perhaps.
\r\n\r\nTrack 2 is intended for those one hundred or so people in the whole\r\nworld who do know classical physics and have serious interests in, or\r\nare experts in relativity theory. Papers 1, 2 and 3 dealing with \r\nrelativity are entirely Track 2.
\r\n\r\nThe remaining paper is Track 3 and is for the benefit of even fewer\r\npeople who have a simultaneous interest in relativity and quantum field\r\ntheory.
\r\n\r\nI will not discuss the abstracts of the individual papers here -\r\nsince each paper is preceded by its own abstract. Suffice it to say that this\r\ndissertation is a collection of papers dealing with the theoretical\r\naspects of how gravitational waves may (or may not) be generated\r\nby gravitational bremsstrahlung, and in Paper 4 Walter and I try to\r\nshow that some classical relativity problems may be solved with much\r\ngreater ease via a quantum approach.
", "date": "1977", "date_type": "degree", "id_number": "CaltechTHESIS:08252017-093756825", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08252017-093756825", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NDEA Fellowship" }, { "agency": "NASA", "grant_number": "NGR 05-002-256" }, { "agency": "NSF", "grant_number": "MPS75-01398" }, { "agency": "NSF", "grant_number": "AST75-01398 A01" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-25 20:23:08", "doi": "10.7907/VHQW-W277", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1977-05-27", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1977", "author_list": "Kov\u00e1cs, S\u00e1ndor J\u00e1nos, Jr." }, { "id": "/id/eprint/3766", "eprint_id": 3766, "rev_number": 7, "documents": [ { "id": "/id/document/6404", "doc_id": 6404, "rev_number": 2, "files": [ { "id": "/id/file/38404", "fileid": 38404, "datasetid": "document", "objectid": 6404, "filename": "Green_rf_1977.pdf", "mime_type": "application/pdf", "filesize": 15798932, "mtime": "2012-12-26 03:02:50", "url": "/3766/1/Green_rf_1977.pdf" } ], "eprint_id": 3766, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Green_rf_1977.pdf", "language": "en", "security": "public", "license": "other", "main": "Green_rf_1977.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22936" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22936" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22936" } ] } }, { "id": "/id/document/22936", "doc_id": 22936, "rev_number": 2, "files": [ { "id": "/id/file/38402", "fileid": 38402, "datasetid": "document", "objectid": 22936, "filename": "preview.png", "mime_type": "image/png", "hash": "1478fc538b45f84276463b4cf3d81e7a", "hash_type": "MD5", "filesize": 9748, "mtime": "2012-12-26 03:02:50", "url": "/3766/2/preview.png" } ], "eprint_id": 3766, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6404" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6404" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6404" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/66", "datestamp": "2008-10-08", "lastmod": "2019-12-21 04:20:05", "status_changed": "2009-09-25 03:05:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Green-R-F", "name": { "family": "Green", "given": "Richard Frederick" }, "show_email": "NO" } ] }, "title": "A complete sample of white dwarfs, hot subdwarfs, and quasars", "ispublished": "unpub", "full_text_status": "public", "abstract": "An analysis is made of a complete sample of hot white dwarfs, identified spectroscopically from candidates selected for ultraviolet excess without regard to proper motion. The luminosity function and local space density of hot white dwarfs are derived, giving 1.43 \u00b1 .28 per 1000 cubic parsecs for M[subscript v] < 12.75. A model of the local rate of star formation is constructed, which, when combined with white dwarf cooling theory, satisfactorily reproduces the observed luminosity function. The predicted densities at fainter absolute magnitudes also agree with the observations although uncertainties in the data do not allow a determination of the change in star formation rate with time. The model predicts a range of scale heights for hot white dwarfs of 220 to 270 pc, and a total local density of degenerate stars of at least 20 per 1000 cubic parsecs. The assumption of a single population of DA white dwarfs with identical composition is not adequate to explain the observed color-color diagram.\n\nA breakdown by spectral type of the entire complete pie of ultraviolet excess objects shows that the hot white dwarfs comprise 70% of the faint blue stars to a mean limiting magnitude of B = 15.7. The mean local density of subdwarf B stars is found to be (1.4 \u00b1 .5) x 10[superscript -9] pc[superscript -3], representing only .0005 of the number of stars on the halo horizontal branch, and thereby explaining their near absence in globular clusters. The mean local density of subdwarf O stars of (3.4 \u00b1 1.2) x 10[superscript -9] pc[superscript-3] makes unlikely the possibility that these stars have any direct evolutionary connection with the observed Population I hot white dwarfs or planetary nebulae. The local space density of quasars is derived on the assumption of cosmological redshifts, and provides no contradiction to the hypothesis of a smooth transition between the phenomena of Seyfert galaxy nuclei and quasars. Both the space and surface densities are consistent with the luminosity function and density evolution laws found by Schmidt (1972); the statistical uncertainties in the present case are too great to determine the choice of density laws.\n\nThe validity of these statistical studies depends upon the objective selection of a sample within well-defined limits of magnitude and color. To that end, computer programs have been developed for use in collecting and processing data from a PDS scanning microdensitometer. The goal is to obtain fast and simple algorithms for handling an entire astronomical photograph with one-pass digitization. This capability is realized by a real-time detection scheme that provides a data compression of a factor of 100, and a processing program that produces a catalogue of magnitudes colors, and positions for up to 90,000 multicolor stellar images.\n", "date": "1977", "date_type": "degree", "id_number": "CaltechETD:etd-09252008-085810", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09252008-085810", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-08", "doi": "10.7907/8Q1N-ZW17", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-25", "thesis_defense_date": "1977-05-23", "thesis_approved_date": "2008-10-08", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1977", "author_list": "Green, Richard Frederick" }, { "id": "/id/eprint/3394", "eprint_id": 3394, "rev_number": 8, "documents": [ { "id": "/id/document/5924", "doc_id": 5924, "rev_number": 2, "files": [ { "id": "/id/file/35239", "fileid": 35239, "datasetid": "document", "objectid": 5924, "filename": "Melnick_j_1977.pdf", "mime_type": "application/pdf", "filesize": 5423141, "mtime": "2012-12-26 02:59:35", "url": "/3394/1/Melnick_j_1977.pdf" } ], "eprint_id": 3394, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Melnick_j_1977.pdf", "language": "en", "security": "public", "license": "other", "main": "Melnick_j_1977.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22464" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22464" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22464" } ] } }, { "id": "/id/document/22464", "doc_id": 22464, "rev_number": 2, "files": [ { "id": "/id/file/35237", "fileid": 35237, "datasetid": "document", "objectid": 22464, "filename": "preview.png", "mime_type": "image/png", "hash": "4a33450270a08ce9149f6b73f99060c8", "hash_type": "MD5", "filesize": 8678, "mtime": "2012-12-26 02:59:35", "url": "/3394/2/preview.png" } ], "eprint_id": 3394, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5924" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5924" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5924" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/94", "datestamp": "2008-09-12", "lastmod": "2019-12-20 19:32:51", "status_changed": "2009-09-25 02:57:44", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Melnick-J", "name": { "family": "Melnick", "given": "Jorge" }, "show_email": "NO" } ] }, "title": "The structure of giant extragalactic HII regions", "ispublished": "unpub", "full_text_status": "public", "abstract": "The existence of a close correlation between the linear diameters of giant HII regions in late type spiral and irregular galaxies and the width of their global H[subscript alpha] emission is demonstrated by means of line profiles obtained using interferometric techniques. The relation (diameter-line width) established in members of the local and M81 \u2014 NGC 2403 groups is applied to a redetermination of the distance to M101.\r\n\r\nWith the purpose of avoiding the difficulties involved in accurately determining linear diameters of giant HII regions, a correlation between H[subscript beta] luminosity and line profile width has been established. The dust distribution in giant HII regions, which is the factor limiting the possible application of the (H[subscript beta] luminosity-line width) relation to the determination of distances, is studied in considerable detail. It is found that most of the extinction affecting the nebular light comes from dust particles that are mixed with the ionized gas, and that the wavelength dependence of the dust absorption is similar to, but significantly different from Whitford's extinction law.\r\n\r\nA dynamical model for giant HII regions is constructed on the basis of a detailed study of the 30 Doradus nebula in the LMC. It is shown that giant HII regions can be regarded as aggregates or \"clusters\" of small HII regions surrounding the hundreds of 0-B stars which ionize the giant nebulae. The highly supersonic velocities observed in these giant HII complexes, therefore, are interpreted as reflecting the motions of the individual stars imbedded therein. It is also shown that galactic shear, amplified during the gravitational collapse of the interstellar cloud out of which the HII regions were formed, can account for at least part of the observed motions.\r\n", "date": "1977", "date_type": "degree", "id_number": "CaltechETD:etd-09082008-145630", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082008-145630", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/H0TV-1A14", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-08", "thesis_defense_date": "1976-11-08", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1977", "author_list": "Melnick, Jorge" }, { "id": "/id/eprint/7179", "eprint_id": 7179, "rev_number": 21, "documents": [ { "id": "/id/document/15163", "doc_id": 15163, "rev_number": 4, "files": [ { "id": "/id/file/99053", "fileid": 99053, "datasetid": "document", "objectid": 15163, "filename": "Page_dn_1976.pdf", "mime_type": "application/pdf", "filesize": 20086237, "mtime": "2012-12-26 04:44:41", "url": "/7179/1/Page_dn_1976.pdf" } ], "eprint_id": 7179, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Page_dn_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/28143" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/28143" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/28143" } ] } }, { "id": "/id/document/15165", "doc_id": 15165, "rev_number": 4, "files": [ { "id": "/id/file/207988", "fileid": 207988, "datasetid": "document", "objectid": 15165, "filename": "Page_dn_1976.zip", "mime_type": "application/zip", "filesize": 128538584, "mtime": "2016-08-22 21:24:12", "url": "/7179/2/Page_dn_1976.zip" } ], "eprint_id": 7179, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Page_dn_1976.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/28143", "doc_id": 28143, "rev_number": 2, "files": [ { "id": "/id/file/99051", "fileid": 99051, "datasetid": "document", "objectid": 28143, "filename": "preview.png", "mime_type": "image/png", "hash": "5141a8e5ee0050b83d7d4286342aa221", "hash_type": "MD5", "filesize": 56713, "mtime": "2012-12-26 04:44:41", "url": "/7179/3/preview.png" } ], "eprint_id": 7179, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15163" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/15163" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15163" } ] } }, { "id": "/id/document/127621", "doc_id": 127621, "rev_number": 1, "files": [ { "id": "/id/file/373057", "fileid": 373057, "datasetid": "document", "objectid": 127621, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "27f53d404d20f2d1251374e9bf82e3c4", "hash_type": "MD5", "filesize": 32822, "mtime": "2021-06-24 01:55:15", "url": "/7179/4/indexcodes.txt" } ], "eprint_id": 7179, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15163" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15163" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15163" } ] } } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/71/79", "datestamp": "2012-07-19 18:18:04", "lastmod": "2022-11-09 19:20:11", "status_changed": "2012-07-19 18:18:04", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Page-D-N", "name": { "family": "Page", "given": "Don Nelson" }, "show_email": "NO" } ] }, "title": "Accretion into and emission from black holes", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Analyses are given of various processes involving matter falling\r\ninto or coming out of black holes.
\r\n\r\nA significant amount of matter may fall into a black hole in a\r\ngalactic nucleus or in a binary system. There gas with relatively high\r\nangular momentum is expected to form an accretion disk flowing into the\r\nhole. In this thesis the conservation laws of rest mass, energy, and\r\nangular momentum are used to calculate the radial structure of such a\r\ndisk. The averaged torque in the disk and flux of radiation from the\r\ndisk are expressed as explicit, algebraic functions of radius.
\r\n\r\nMatter may be created and come out of the gravitational field of\r\na black hole in a quantum-mechanical process recently discovered by\r\nHawking. In this thesis the emission rates of massless particles by\r\nHawking's process are computed numerically. The resulting power spectra\r\nof neutrinos, photons, and gravitons emitted by a nonrotating hole are\r\ngiven. For rotating holes, the rates of emission of energy and angular\r\nmomentum are calculated for various values of the rotation parameter.\r\nThe evolution of a rotating hole is followed as energy and angular\r\nmomentum are given up to the emitted particles. It is found that angular\r\nmomentum is lost considerably faster than energy, so that a black\r\nhole spins down to a nearly nonrotating configuration before it loses a\r\nlarge fraction of its mass. The implications are discussed for the lifetimes and possible present configurations of primordial black\r\nholes (the only holes small enough for the emission to be significant\r\nwithin the present age of the universe.
\r\n\r\nAs an astrophysical application, a calculation is given of the\r\ngamma-ray spectrum today from the emission by an assumed distribution\r\nof primordial black holes during the history of the universe. Comparison\r\nwith the observed isotropic gamma-ray flux above about 100 MeV yields\r\nan upper limit of approximately 10^4 pc^(-3) for the average number density\r\nof holes around 5 x 10^(14)g. (This is the initial mass of a nonrotating\r\nblack hole that would just decay away in the age of the universe.) The\r\nprospects are discussed for observing the final, explosive decay of an\r\nindividual primordial black hole. Such an observation could test the\r\ncombined predictions of general relativity and quantum mechanics and\r\nalso could provide information about inhomogeneities in the early universe\r\nand about the nature of strong interactions at high temperatures.
\r\n", "date": "1976", "date_type": "degree", "id_number": "CaltechTHESIS:07192012-091529776", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:07192012-091529776", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_on": "2012-07-19 18:18:04", "doi": "10.7907/RAEC-8822", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" }, { "id": "Hawking-S-W", "name": { "family": "Hawking", "given": "Stephen W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1976-05-20", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Page, Don Nelson" }, { "id": "/id/eprint/3343", "eprint_id": 3343, "rev_number": 7, "documents": [ { "id": "/id/document/5864", "doc_id": 5864, "rev_number": 2, "files": [ { "id": "/id/file/34821", "fileid": 34821, "datasetid": "document", "objectid": 5864, "filename": "Williams_tb_1976.pdf", "mime_type": "application/pdf", "filesize": 5808909, "mtime": "2012-12-26 02:59:13", "url": "/3343/1/Williams_tb_1976.pdf" } ], "eprint_id": 3343, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Williams_tb_1976.pdf", "language": "en", "security": "public", "license": "other", "main": "Williams_tb_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22404" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22404" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22404" } ] } }, { "id": "/id/document/22404", "doc_id": 22404, "rev_number": 2, "files": [ { "id": "/id/file/34819", "fileid": 34819, "datasetid": "document", "objectid": 22404, "filename": "preview.png", "mime_type": "image/png", "hash": "df3ac94ae4ceab70ce52e57239913134", "hash_type": "MD5", "filesize": 9415, "mtime": "2012-12-26 02:59:13", "url": "/3343/2/preview.png" } ], "eprint_id": 3343, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5864" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5864" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5864" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/43", "datestamp": "2008-09-10", "lastmod": "2019-12-20 19:32:14", "status_changed": "2009-09-25 02:56:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Williams-T-B", "name": { "family": "Williams", "given": "Theodore Burton" }, "show_email": "NO" } ] }, "title": "Stellar populations and velocity dispersions of ten nearby galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nPrevious attempts to synthesize the stellar populations of galaxies using unconstrained best fit algorithms yield astrophysically unreasonable models. Numerical experiments are performed which indicate that this behavior is due to noise in the data. Best fit models, constrained or not, are insensitive to the actual galaxy stellar population.\n\nSpectra from 3800 [...] to 6800 [...] with resolution of 2 [...] have been obtained for 137 stars, 5 globular clusters, and the nuclear regions of 10 galaxies. Line indices measured for 74 absorption lines and bands are presented. A method for determining parametrized stellar population models is discussed, and is shown to be stable in the prescence of noise. Population models and error estimates are derived for the ten galaxies. Most of the models have significant contributions from M giant stars and from metal poor stars. Only two of the galaxies seem to contain stars with metal lines stronger than those of stars in the solar neighborhood. Three of the ellipticals show evidence of recent star formation, possibly due to infall of gas from nearby spirals. The galaxies studied here can be divided by morphological type into three distinct population groups; E0 - Sa, Sb, and Sc.\n\nVelocity dispersions have been derived for the nuclear regions of the galaxies. These dispersions are estimated by comparing broadened composite stellar spectra with the galaxy spectra. The composite spectra give systematically lower velocity dispersions than those estimated from fitting with single stars. Mass to light ratios are derived from the velocity dispersions. These mass to light ratios are low, and there are no systematic differences between the nuclei of spirals and ellipticals.\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-09052008-132346", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09052008-132346", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/85S6-PX78", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-05", "thesis_defense_date": "1975-10-20", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Williams, Theodore Burton" }, { "id": "/id/eprint/3231", "eprint_id": 3231, "rev_number": 27, "documents": [ { "id": "/id/document/5722", "doc_id": 5722, "rev_number": 4, "files": [ { "id": "/id/file/33885", "fileid": 33885, "datasetid": "document", "objectid": 5722, "filename": "Reid_mj_1975.pdf", "mime_type": "application/pdf", "filesize": 3948268, "mtime": "2012-12-26 02:58:17", "url": "/3231/1/Reid_mj_1975.pdf" } ], "eprint_id": 3231, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Reid_mj_1975.pdf", "language": "en", "security": "internal", "license": "other", "main": "Reid_mj_1975.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"datestamp": "2008-09-09", "lastmod": "2020-02-29 02:05:46", "status_changed": "2009-09-25 02:54:54", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "reid@cfa.harvard.edu", "id": "Reid-Mark-Jonathan", "name": { "family": "Reid", "given": "Mark Jonathan" }, "orcid": "0000-0001-7223-754X", "show_email": "YES" } ] }, "title": "The Structure of Hydroxyl Masers and Circumstellar Envelopes of Long Period Variable Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Long period variable stars", "abstract": "Long period variable stars with envelopes of circumstellar dust and gas often exhibit strong hydroxyl (OH) maser emission. This emission is characterized by two emission line complexes typically separated by 20 km/s. While the OH maser spectra suggest well defined dynamical properties of the circumstellar material, the crucial observations required to determine these properties have been lacking. This thesis is primarily concerned with determining the radial velocity of the central star and the spatial distribution of the maser emission in the circumstellar material.
\r\n\r\nThe radial velocity of the central star can be determined by a statistical analysis of spectral line velocities in an ensemble of stars. Such an analysis is presented in Chapter I for optical emission and absorption lines and for radio OH maser emission lines. The results indicate that, contrary to currently accepted theories, the optical absorption line velocities and the high velocity OH emission line velocities are red-shifted with respect to the stellar radial velocity. This argues against models of the OH emission which involve shock fronts or emission from the limb of a spherically expanding circumstellar shell.
\r\n\r\nThe spatial distribution of the maser emission can be determined from radio interferometric observations. Spectral-line very long baseline (VLB) interferometric observations of the OH maser emission in long period variable stars such as IRC+F10011, U Ori and R Aql are presented in Chapter II. The primary result of these observations is that the apparent sizes of the OH maser components in long period variable stars are greater than or about 5 x 1015 cm. These large apparent sizes argue strongly against either gravitational collapse or rotation as the dominant dynamical process in the circumstellar envelope. Analysis of data obtained on IRC+10011 and VY CMa (discussed in Chapter III) indicate that the two emission complexes probably are separated by distances less than, or comparable to, the extent of the emission in either complex. These and other findings suggest that OH emission from long period variable stars comes from a series of concentric, inhomogeneous, circumstellar shells expanding from the central star. The origin of these shells is probably a result of condensation of dust followed by radiative acceleration away from the star during the stellar light cycle.
\r\n\r\nA direct Fourier inversion of VLB data is presented in Chapter III for the 1612 MHz OH emission of VY CMa. This is the first attempt at such an analysis procedure for any VLB observations. This work demonstrates that Fourier inversion of spectral-line VLB data, even with very limited u-v coverage, is more efficient and less biased than direct model fitting for the resolution of complex source structures.
\r\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-08262008-113619", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08262008-113619", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "MPS 73-04677A02" }, { "agency": "NASA", "grant_number": "05-002-114" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/4EGT-TW53", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "duane.muhleman@gmail.com", "id": "Muhleman-D-O", "name": { "family": "Muhleman", "given": "Duane Owen" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "duane.muhleman@gmail.com", "id": "Muhleman-D-O", "name": { "family": "Muhleman", "given": "Duane Owen" }, "role": "member" }, { "email": "pmg@ias.edu", "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "member" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "member" }, { "id": "Preston-G-W", "name": { "family": "Preston", "given": "George W." }, "role": "member" }, { "email": "mhc@astro.caltech.edu", "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-26", "thesis_defense_date": "1975-10-10", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Reid, Mark Jonathan" }, { "id": "/id/eprint/3393", "eprint_id": 3393, "rev_number": 7, "documents": [ { "id": "/id/document/5923", "doc_id": 5923, "rev_number": 2, "files": [ { "id": "/id/file/35232", "fileid": 35232, "datasetid": "document", "objectid": 5923, "filename": "Bagnuolo_wg_1976.pdf", "mime_type": "application/pdf", "filesize": 4192245, "mtime": "2012-12-26 02:59:35", "url": "/3393/1/Bagnuolo_wg_1976.pdf" } ], "eprint_id": 3393, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Bagnuolo_wg_1976.pdf", "language": "en", "security": "public", "license": "other", "main": "Bagnuolo_wg_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22463" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22463" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22463" } ] } }, { "id": "/id/document/22463", "doc_id": 22463, "rev_number": 2, "files": [ { "id": "/id/file/35230", "fileid": 35230, "datasetid": "document", "objectid": 22463, "filename": "preview.png", "mime_type": "image/png", "hash": "076211b17a2d647e132451e7ed88fef9", "hash_type": "MD5", "filesize": 10318, "mtime": "2012-12-26 02:59:35", "url": "/3393/2/preview.png" } ], "eprint_id": 3393, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5923" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5923" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5923" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/93", "datestamp": "2008-09-12", "lastmod": "2019-12-20 19:53:02", "status_changed": "2009-09-25 02:57:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bagnuolo-W-G", "name": { "family": "Bagnuolo", "given": "William G." }, "show_email": "NO" } ] }, "title": "The stellar composition and evolution of irregular and other late-type galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "The stellar content and history of star formation of a number of Irregular and other late-type galaxies have been analyzed by means of 10-color photometery of the galaxies and a comparison of their colors to the calculated colors of a set of three-parameter models. The galaxy models are assumed to be composed of various amounts of \"clusters\" from 10[superscript 6] to 10[superscript 10] years old, the colors of which were calculated from stellar-evolutionary tracks and observations of 102 stars of all spectral types. The colors of the model clusters were checked by comparison to the colors of 46 clusters in the Magellanic Clouds.\n\nThe first chapter of the thesis gives the principal results of the work, the analysis of the galaxies; the second gives a description of the cluster models and comparison to the cluster observations; the third presents the colors of the 102 calibrating stars.\n\nIn the first chapter the colors from 79 observations of 46 different Irregular and other late-type galaxies (mostly Sc's) are given first. The construction of model cluster colors and their behavior as a function of time, t, are briefly discussed. A principal component analysis of the galaxy colors indicates that only three parameters could explain most of the variation in galaxy colors.\n\nAccordingly, a set of three-parameter models is adopted to explain their colors. The three parameters chosen govern the star formation history of the galaxies. The Limber initial mass formation function is assumed. Various two-color plots of some of the galaxy models were made. It is found that the loci of the models agree well with observations. Finally, fits to individual galaxies in the three parameters are made, as well as estimates of the \"uniqueness\" of the fits. The average difference between the best-fitting parameters of Irregulars and Sc's is interpreted to mean that Irregulars have both relatively more star formation in the recent past and an initial mass formation function enriched in massive stars compared to the Sc's. An irregular rate of star formation in the recent past (t <10[superscript 8] yr) is also indicated.\n\nThe second chapter describes the construction of cluster models and a comparison between the model colors and the colors of 46 clusters in the Magellanic Clouds. Cluster models are found to fit observations well in general. Furthermore, the observations permit estimates of n[subscript b]/n[subscript r], the ratio of blue to red supergiants, to be obtained for stars of 3 to 20 solar masses.\n\nThe third chapter gives a description of the observation of 102 stars of all luminosity classes and spectral types from O5 to M6. The behavior of the colors of stars of different luminosity classes as functions of assumed log T[subscript e] and spectral type are discussed.\n\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-09082008-143633", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09082008-143633", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/84BT-0F97", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-08", "thesis_defense_date": "1976-01-23", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Bagnuolo, William G." }, { "id": "/id/eprint/3415", "eprint_id": 3415, "rev_number": 7, "documents": [ { "id": "/id/document/5950", "doc_id": 5950, "rev_number": 2, "files": [ { "id": "/id/file/35408", "fileid": 35408, "datasetid": "document", "objectid": 5950, "filename": "Turner_el_1976.pdf", "mime_type": "application/pdf", "filesize": 4573334, "mtime": "2012-12-26 02:59:45", "url": "/3415/1/Turner_el_1976.pdf" } ], "eprint_id": 3415, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Turner_el_1976.pdf", "language": "en", "security": "public", "license": "other", "main": "Turner_el_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22490" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22490" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22490" } ] } }, { "id": "/id/document/22490", "doc_id": 22490, "rev_number": 2, "files": [ { "id": "/id/file/35406", "fileid": 35406, "datasetid": "document", "objectid": 22490, "filename": "preview.png", "mime_type": "image/png", "hash": "0e43f0b02a333f5257712d5f86ac51b1", "hash_type": "MD5", "filesize": 9203, "mtime": "2012-12-26 02:59:45", "url": "/3415/2/preview.png" } ], "eprint_id": 3415, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5950" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5950" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5950" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/15", "datestamp": "2008-09-18", "lastmod": "2019-12-21 04:53:01", "status_changed": "2009-09-25 02:58:07", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Turner-E-L", "name": { "family": "Turner", "given": "Edwin Lewis" }, "show_email": "NO" } ] }, "title": "Binary galaxies and groups of galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nUsing precisely defined identification criteria, a sample of 156 binary galaxy systems is selected from the Zwicky Catalog of Galaxies and Clusters of Galaxies. Data on their magnitudes, morphological types, radial velocities, angular separations, et cetera are presented. Accurate, new radial velocities for both components of 66 of the pairs have been measured. Substantial effort is directed towards establishing a sample of binary galaxies in which all sources of systematic bias and statistical error are well understood.\n\nWith particular attention to the removal of selection effects, extensive statistical and dynamical analyses of these data lead to several conclusions: The ratio of the mass-to-light ratio in early-type galaxies to that in late-types is 2.0[...]0.5. The distribution of spatial separations r between binary galaxies has an approximately r[...] dependence. A variety of dynamical models for binary galaxy systems are viable; however, they all require total mass-to-light ratios for spirals far larger than conventional (rotation curve) values. The most plausible interpretation of the binary galaxy data requires that spiral galaxies possess halos containing [...]10 times the disk mass and have total mass-to-light ratios [...]. It is shown that previous studies of binary galaxies have probably underestimated masses by a factor [...]10 primarily because selection biases (particularly those toward small projected separations) were ignored. There is some evidence against halos containing significant mass on scales very large compared to 100 kpc. Orbits of moderate eccentricity are more consistent with the present data than either purely circular or purely radial (probably excluded) ones.\n\nA catalog of small groups of galaxies is generated by identifying regions of the sky in which the surface number-density of galaxies is enhanced. The determinations of both group existence and membership are accomplished by well-defined procedures and are based entirely on the distribution of galaxies in the sky. A variety of data on the groups, their component galaxies, and those galaxies not assigned to groups (i.e. field galaxies) is presented. The generally small velocity dispersions of the groups validate the group identification algorithm.\n\nUsing the available data, statistical analyses of the galaxy luminosity function in groups, the group dynamics, and the multiplicity function are described. The luminosity function is shown to be similar to that in rich clusters, well fit by a Schechter function with [...] and [...], and useful for estimating group distances. The dynamical analysis indicated that the groups are bound and relaxed, and gives typical mass-to-light ratios of [...]. A crude estimate of the group multiplicity function (distribution of total group luminosities) suggests a power-law [...] for groups brighter than [...].\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-135416", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-135416", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-18", "doi": "10.7907/C4RG-BW87", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1975-10-13", "thesis_approved_date": "2008-09-18", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Turner, Edwin Lewis" }, { "id": "/id/eprint/3439", "eprint_id": 3439, "rev_number": 7, "documents": [ { "id": "/id/document/5974", "doc_id": 5974, "rev_number": 2, "files": [ { "id": "/id/file/35590", "fileid": 35590, "datasetid": "document", "objectid": 5974, "filename": "Kormendy_j_1976.pdf", "mime_type": "application/pdf", "filesize": 6235892, "mtime": "2012-12-26 02:59:55", "url": "/3439/1/Kormendy_j_1976.pdf" } ], "eprint_id": 3439, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Kormendy_j_1976.pdf", "language": "en", "security": "public", "license": "other", "main": "Kormendy_j_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22514" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22514" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22514" } ] } }, { "id": "/id/document/22514", "doc_id": 22514, "rev_number": 2, "files": [ { "id": "/id/file/35588", "fileid": 35588, "datasetid": "document", "objectid": 22514, "filename": "preview.png", "mime_type": "image/png", "hash": "6dc8ad1a6201683951f192ee0ddfebdc", "hash_type": "MD5", "filesize": 9259, "mtime": "2012-12-26 02:59:55", "url": "/3439/2/preview.png" } ], "eprint_id": 3439, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5974" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5974" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5974" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/39", "datestamp": "2008-09-17", "lastmod": "2019-12-21 04:15:59", "status_changed": "2009-09-25 02:58:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kormendy-J", "name": { "family": "Kormendy", "given": "John" }, "show_email": "NO" } ] }, "title": "Brightness distributions in compact and normal galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nA study is made of three problems on luminosity distributions in galaxies: the nature of red compact galaxies, the systematic properties of spheroids, and the effect of decomposing observed profiles into spheroid and disk components.\n\nPhotographic brightness profiles are measured and discussed for sixteen compact and four normal galaxies, with the following results.\n\n(i) Red compacts are qualitatively E and SO galaxies.\n\n(ii) Their central and mean surface brightnesses are generally normal. Only II Zw 67 and VII Zw 421 are noticeably compact.\n\n(iii) Profile components which Sandage, in the Hubble Atlas, called lenses occur with great frequency and strength. They are the \"large, nearly uniform brightness halos\" described by Zwicky. VII Zw 793 has an exceptionally strong lens, which must be a disk because it shows spiral structure.\n\n(iv) II Zw 67 and VII Zw 421 seem to be prototypes of a class of very luminous, early-type objects with dominant spheroid-like lenses, and spectra characteristic of metal-poor stars.\n\n(v) Lenses are a distinct and independent component in galaxy profiles. They seem to be morphologically intermediate between spheroids and disks.\n\nA systematic study of galaxy spheroids is made by fitting the de Vaucouleurs r[superscript 1/4]-law to the profiles of sixteen compact and nineteen normal galaxies. The results are as follows.\n\n(i) Ellipticals with massive neighbors have bright outer halos not possessed by more isolated objects. Possible tidal explanations are considered.\n\n(ii) The brightness and radius parameters are related by B[subscript oV]= 3.02 log r[subscript o] + 19.74 B mag arcsec[superscript -2] ([...]). Here r[subscript o] varies from 1.0 to 14.1 kpc, and B[subscript oV] from 19.8 to 23.3 B[...]. Brighter galaxies tend to have larger r[subscript o] and fainter [subscript oV'] with considerable scatter.\n\n(iii) Some compacts are truly compact in having abnormally small r[subscript o] and bright B[subscript oV] for their absolute magnitude; most are just intrinsically faint.\n\n(iv) The B[subscript oV](log r[subscript o]) relation can be used to determine distances. We show that the Virgo cluster is closer than its redshift distance by \u03b4(m-M) \u2264 0[...]07 \u00b1 0[...]23, a null result supporting the uniform Hubble flow advocated by Sandage and Tammann.\n\nDetailed comparisons are made of how profile models due to de Vaucouleurs, Hubble and King fit galaxies. We show that the above results are model independent.\n\nFinally, exponential disk parameters are derived for seven S0 compacts and for NGC 7457. The central disk brightness B(0)[subscript c] is generally normal, but is unusually faint in two objects. Scale lengths are ~ 7 kpc, at the long end of the distribution found in normal galaxies. Spheroids clearly contribute significantly to the disk parameters. We therefore decompose the profiles into their underlying components. The disks, actually lenses in these objects, are shown to have a (possibly complete) inner brightness cutoff, where they enter the dominant part of the spheroid. Parameters of the underlying distributions are poorly determined, because there is considerable freedom in their relative strength. However, spheroids, and the above results on spheroids, are little affected by decomposition. In contrast, disks become significantly fainter.\n\nMotivated by this, we use model galaxies to investigate the spheroid contribution to B(0)[subscript c] derived for a composite profile. Exponentials with B(0)[subscript c] = 20-25 B[...] are added to spheroids with a wide range of parameters. These reproduce very well the distribution of B(0)[subscript c] observed for normal galaxies. Thus the near universality of B(0)[superscript c] = 21.65 \u00b1 0.30 B[...], observed by Freeman for 28 of 36 galaxies, is largely due to the contribution of the spheroid. Real disks can be much fainter. Measurements of galaxies with no spheroid are found to be consistent with this conclusion.\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-09102008-104759", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102008-104759", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-17", "doi": "10.7907/YZFX-X226", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-10", "thesis_defense_date": "1976-04-09", "thesis_approved_date": "2008-09-17", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Kormendy, John" }, { "id": "/id/eprint/3316", "eprint_id": 3316, "rev_number": 7, "documents": [ { "id": "/id/document/5836", "doc_id": 5836, "rev_number": 2, "files": [ { "id": "/id/file/34617", "fileid": 34617, "datasetid": "document", "objectid": 5836, "filename": "Hickson_p_1976.pdf", "mime_type": "application/pdf", "filesize": 1952893, "mtime": "2012-12-26 02:59:02", "url": "/3316/1/Hickson_p_1976.pdf" } ], "eprint_id": 3316, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Hickson_p_1976.pdf", "language": "en", "security": "public", "license": "other", "main": "Hickson_p_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22377" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22377" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22377" } ] } }, { "id": "/id/document/22377", "doc_id": 22377, "rev_number": 2, "files": [ { "id": "/id/file/34615", "fileid": 34615, "datasetid": "document", "objectid": 22377, "filename": "preview.png", "mime_type": "image/png", "hash": "574e5597debbfef410ddee3a365ee7df", "hash_type": "MD5", "filesize": 9496, "mtime": "2012-12-26 02:59:02", "url": "/3316/2/preview.png" } ], "eprint_id": 3316, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5836" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5836" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5836" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/16", "datestamp": "2008-09-10", "lastmod": "2019-12-21 02:54:52", "status_changed": "2009-09-25 02:56:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hickson-P", "name": { "family": "Hickson", "given": "Paul" }, "show_email": "NO" } ] }, "title": "The structure of clusters of galaxies and the angular size-redshift test", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nAn angular size-redshift cosmological test is presented based on the projected separations between bright cluster galaxies as the size statistic. The method is applied to 95 clusters of galaxies with redshifts ranging from .02 to .46 yielding a value of the deceleration parameter before evolution of q[...] = -.9. After correcting for known evolutionary effects we obtain q[...] = -.8. The formal standard deviation in q[...] at these values is .2, which corresponds to an uncertainty of about .4 at q[...] = 0. It is argued that the selection criteria for the sample, and the observed behavior of the cluster size dispersion with redshift precludes the existence of any major selection or evolutionary effects in the data.\n\nStructure parameters are presented for a sample of 64 cosmologically near clusters, and correlated with Rood and Sastry type. New type classifications are presented for 23 clusters. Mean surface density profiles are determined for the various cluster types. It is found that many clusters are deficient in separations of one to two Mpc.\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-09022008-152652", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09022008-152652", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/6F00-K950", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Gunn-J-E", "name": { "family": "Gunn", "given": "James E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-02", "thesis_defense_date": "1976-03-16", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Hickson, Paul" }, { "id": "/id/eprint/3225", "eprint_id": 3225, "rev_number": 9, "documents": [ { "id": "/id/document/5716", "doc_id": 5716, "rev_number": 2, "files": [ { "id": "/id/file/33815", "fileid": 33815, "datasetid": "document", "objectid": 5716, "filename": "Willner_sp_1976.pdf", "mime_type": "application/pdf", "filesize": 1836451, "mtime": "2012-12-26 02:58:14", "url": "/3225/1/Willner_sp_1976.pdf" } ], "eprint_id": 3225, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Willner_sp_1976.pdf", "language": "en", "security": "public", "license": "other", "main": "Willner_sp_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22258" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22258" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22258" } ] } }, { "id": "/id/document/22258", "doc_id": 22258, "rev_number": 2, "files": [ { "id": "/id/file/33813", "fileid": 33813, "datasetid": "document", "objectid": 22258, "filename": "preview.png", "mime_type": "image/png", "hash": "27bb192c116c3762ee0c9c78d2a5b2dc", "hash_type": "MD5", "filesize": 7827, "mtime": "2012-12-26 02:58:14", "url": "/3225/2/preview.png" } ], "eprint_id": 3225, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5716" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5716" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5716" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/25", "datestamp": "2008-09-09", "lastmod": "2019-12-20 19:58:37", "status_changed": "2009-09-25 02:54:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Willner-S-P", "name": { "family": "Willner", "given": "Steven Paul" }, "show_email": "NO" } ] }, "title": "Compact infrared sources : NGC 7538 and the galactic center", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThree infrared and radio sources in NGC 7538 have been observed from 8 to 13 [...] with 1% spectral and 5\" spatial resolution. The very small southern source shows a deep silicate absorption feature at 9.7 [...] while the northern extended source shows little or no silicate absorption, but has a 12.8-[...] emission line from Ne II. The data imply that the compact source has a gas to dust ratio of 75 inside the ionized region. The extended source only 10\" away has a gas to dust ratio implied by the 10-[...] data alone of 3 x 10[...], but the true ratio must be much lower to account for published 20-[...] measurements.\n\nA revised 10-[...] map of the Galactic center with 2[...]3 resolution, broadband photometry of individual sources from 1.2 to 20 [...], and 8 to 13-[...] photometry of individual sources with 1% spectral resolution have been obtained. The principal conclusions of this study are: (1) The five sources with the bluest energy distributions between 1.6 and 3.5 [...] are stars or star clusters. The brightest has a luminosity of 10[...] L[...] while the other four have luminosities of about 10[...] L[...]. (2) There is extended emission from ionized gas and dust. (3) The density of ionized gas in the discrete 10-[...] sources is no higher than that in the extended source. (4) There is at least one compact source that is not associated with the others and has a different energy distribution. (5) Most of the extinction toward the sources observed is interstellar and is moderately uniform. The visual extinction is about 28 magnitudes, and the 9.7-[...] silicate extinction is about 3.7 magnitudes.\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-08252008-153611", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08252008-153611", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/YGRP-NJ17", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Becklin-E-E", "name": { "family": "Becklin", "given": "Eric E." }, "role": "advisor" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-25", "thesis_defense_date": "1976-01-29", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Willner, Steven Paul" }, { "id": "/id/eprint/3414", "eprint_id": 3414, "rev_number": 11, "documents": [ { "id": "/id/document/5949", "doc_id": 5949, "rev_number": 2, "files": [ { "id": "/id/file/35401", "fileid": 35401, "datasetid": "document", "objectid": 5949, "filename": "Turnrose_be_1976.pdf", "mime_type": "application/pdf", "filesize": 5675088, "mtime": "2012-12-26 02:59:45", "url": "/3414/1/Turnrose_be_1976.pdf" } ], "eprint_id": 3414, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Turnrose_be_1976.pdf", "language": "en", "security": "public", "license": "other", "main": "Turnrose_be_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22489" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22489" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22489" } ] } }, { "id": "/id/document/22489", "doc_id": 22489, "rev_number": 2, "files": [ { "id": "/id/file/35399", "fileid": 35399, "datasetid": "document", "objectid": 22489, "filename": "preview.png", "mime_type": "image/png", "hash": "97658a36ab37a05b82ec609bd1e60b01", "hash_type": "MD5", "filesize": 8974, "mtime": "2012-12-26 02:59:45", "url": "/3414/2/preview.png" } ], "eprint_id": 3414, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5949" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5949" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5949" } ] } }, { "id": "/id/document/45907", "doc_id": 45907, "rev_number": 3, "files": [ { "id": "/id/file/134551", "fileid": 134551, "datasetid": "document", "objectid": 45907, "filename": "Turnrose Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "14d648c0f929f85d30ede799fb61c895", "hash_type": "MD5", "filesize": 873, "mtime": "2014-02-11 21:09:27", "url": "/3414/3/Turnrose Thesis Permission Form.txt" } ], "eprint_id": 3414, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "author ok feb 2014", "language": "en", "security": "internal", "license": "other", "main": "Turnrose Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/14", "datestamp": "2008-09-17", "lastmod": "2019-12-21 04:52:25", "status_changed": "2009-09-25 02:58:05", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "turnrose@hotmail.com", "id": "Turnrose-B-E", "name": { "family": "Turnrose", "given": "Barry Edmund" }, "show_email": "YES" } ] }, "title": "The stellar content of the nuclear regions of Sc galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy ; Sc galaxies", "abstract": "The stellar content of the nuclear regions of seven nearby Sc galaxies has been determined by means of population syntheses utilizing narrow-band spectrophotometric observations covering the wavelength range 3300\u00c5-10400\u00c5. A linear-programming fitting technique is used in conjunction with simple models of star formation to provide physically consistent population models incorporating multiple generations of stars. Evidence is found for substantial intrinsic reddening in the nuclear regions studied. Upper main-sequence stars are significant contributors in most cases, and the lower main sequence contributes insignificantly in all cases. All available indicators are consistent with M-giant-star dominance at the longest wavelengths.
\r\n\r\nAbsolute measurements of the emission-line spectra of the nuclear regions are presented and discussed. The 0-B stars arising naturally in the population models are found to be just sufficient to provide the observed nuclear ionization in all cases but NGC 5194, which may be collisionally ionized. The observed stellar populations are largely consistent with simple evolutionary models of star formation using a \"local\" initial mass function and a variety of time dependences ranging from exponential decays with time constants ~3-6 billion years to constant rates. A possibly significant correlation between stellar content and dynamical properties among four of the program galaxies is pointed out.
\r\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-130914", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-130914", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-17", "doi": "10.7907/4HGY-GB71", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "chair" }, { "id": "Franklin-J-N", "name": { "family": "Franklin", "given": "Joel N." }, "role": "member" }, { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "member" }, { "id": "Toomre-A", "name": { "family": "Toomre", "given": "Alar" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1975-07-30", "thesis_approved_date": "2008-09-17", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Turnrose, Barry Edmund" }, { "id": "/id/eprint/3188", "eprint_id": 3188, "rev_number": 9, "documents": [ { "id": "/id/document/5652", "doc_id": 5652, "rev_number": 2, "files": [ { "id": "/id/file/33427", "fileid": 33427, "datasetid": "document", "objectid": 5652, "filename": "Pigg_jc_1976.pdf", "mime_type": "application/pdf", "filesize": 1944829, "mtime": "2012-12-26 02:57:49", "url": "/3188/1/Pigg_jc_1976.pdf" } ], "eprint_id": 3188, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Pigg_jc_1976.pdf", "language": "en", "security": "public", "license": "other", "main": "Pigg_jc_1976.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22195" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22195" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22195" } ] } }, { "id": "/id/document/22195", "doc_id": 22195, "rev_number": 2, "files": [ { "id": "/id/file/33425", "fileid": 33425, "datasetid": "document", "objectid": 22195, "filename": "preview.png", "mime_type": "image/png", "hash": "dfb36a58d7aea73e9b8b1c22964eeaf2", "hash_type": "MD5", "filesize": 9265, "mtime": "2012-12-26 02:57:49", "url": "/3188/2/preview.png" } ], "eprint_id": 3188, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5652" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5652" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5652" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/88", "datestamp": "2008-09-09", "lastmod": "2019-12-21 04:31:26", "status_changed": "2009-09-25 02:53:45", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pigg-J-C", "name": { "family": "Pigg", "given": "Jay Cee" }, "show_email": "NO" } ] }, "title": "A limit on the inhomogeneity of the cosmic microwave background radiation at an angular scale of 1.25 arcmin", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nAn observational upper limit to the inhomogeneity of the cosmic background radiation of [...]T/T [...] 7.4 x 10[...] on an angular scale of 1.25 arcmin was obtained at a wavelength of 2.0 cm. This and Pariiskii's (1973, Astron. Zh., 50, 453 [Sov. Astron., 17, 291]) limit of [...]T/T [...] 4.8 x 10[...] at 22 arcmin define the observational upper limit to [...]T/T for all scales 1\u00b0 or less. Constraints are placed on published models of galaxy formation and 1000-Mpc scale clustering. Hypotheses that fluctuations in the background radiation could be caused by random fluctuations in the number of protogalaxies in a given solid angle, and that reionization of the intergalactic medium could be associated with the collapse of protogalaxies are shown to be consistent with the observations. Any discrete source model for the origin of the radiation would require more than 100 times as many sources as there are galaxies.\r\n", "date": "1976", "date_type": "degree", "id_number": "CaltechETD:etd-08212008-135114", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08212008-135114", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/RJMF-HZ44", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Moffet-A-T", "name": { "family": "Moffet", "given": "Alan Theodore" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-21", "thesis_defense_date": "1976-05-27", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1976", "author_list": "Pigg, Jay Cee" }, { "id": "/id/eprint/3403", "eprint_id": 3403, "rev_number": 9, "documents": [ { "id": "/id/document/5938", "doc_id": 5938, "rev_number": 2, "files": [ { "id": "/id/file/35321", "fileid": 35321, "datasetid": "document", "objectid": 5938, "filename": "Chu_kw_1975.pdf", "mime_type": "application/pdf", "filesize": 8587686, "mtime": "2012-12-26 02:59:41", "url": "/3403/1/Chu_kw_1975.pdf" } ], "eprint_id": 3403, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Chu_kw_1975.pdf", "language": "en", "security": "public", "license": "other", "main": "Chu_kw_1975.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22478" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22478" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22478" } ] } }, { "id": "/id/document/22478", "doc_id": 22478, "rev_number": 2, "files": [ { "id": "/id/file/35319", "fileid": 35319, "datasetid": "document", "objectid": 22478, "filename": "preview.png", "mime_type": "image/png", "hash": "015daf42ea558f14aa52291e5c5a1860", "hash_type": "MD5", "filesize": 8523, "mtime": "2012-12-26 02:59:41", "url": "/3403/2/preview.png" } ], "eprint_id": 3403, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5938" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5938" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5938" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/03", "datestamp": "2008-09-12", "lastmod": "2019-12-21 04:40:24", "status_changed": "2009-09-25 02:57:53", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chu-K-W", "name": { "family": "Chu", "given": "Kwong Wah" }, "show_email": "NO" } ] }, "title": "HI observations of dust clouds", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nAperture synthesis observations of three dust clouds, L134, L1495 and L1517, were made at 21 cm. A 7 arc min diameter beam was synthesized, and the velocity resolution was 0.2 km/sec. In addition to interferometer observations, single dish measurements were carried out to provide large scale information. Two dust clouds, L134 and L1495, were detected in absorption against background 21 cm emission. In both cases the 21 cm absorption line is at a velocity coincident with molecular lines detected in the dust clouds. The hydrogen responsible for the absorption line has a spin temperature less than 2[...] K, and the columnar atomic hydrogen density through the dust clouds is between [...] and [...]. Based upon optical extinction and normal cosmic abundances, the expected hydrogen content is [...]. It is presumed that most of the hydrogen is in molecular form.\r\n\r\nL134 consists of two velocity components separated by 2 km/sec. Fragmentation of a larger cloud into two smaller components may explain the data, but more evidence is needed to draw any firm conclusion. Within an individual velocity component, no significant substructure was detected in L134 or L1495. The optical appearance of L1517 strongly suggests a fragmented structure, but this dust cloud was not detectable at 21 cm. L1517 may be sufficiently dense that the amount of residual atomic hydrogen is too small to detect, but this conjecture remains to be substantiated.\r\n", "date": "1975", "date_type": "degree", "id_number": "CaltechETD:etd-09092008-081132", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09092008-081132", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/FFYW-J027", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Rogstad-D-H", "name": { "family": "Rogstad", "given": "David Herbert" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-09", "thesis_defense_date": "1974-08-29", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1975", "author_list": "Chu, Kwong Wah" }, { "id": "/id/eprint/1316", "eprint_id": 1316, "rev_number": 14, "documents": [ { "id": "/id/document/2007", "doc_id": 2007, "rev_number": 3, "files": [ { "id": "/id/file/12540", "fileid": 12540, "datasetid": "document", "objectid": 2007, "filename": "Kirshner_rp_1975.pdf", "mime_type": "application/pdf", "filesize": 4773390, "mtime": "2012-12-26 02:37:11", "url": "/1316/1/Kirshner_rp_1975.pdf" } ], "eprint_id": 1316, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Kirshner_rp_1975.pdf", "language": "en", "security": "internal", "license": "other", "main": "Kirshner_rp_1975.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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\r\n\r\nThe Crab Nebula is shown to have a mass of ionized hydrogen in excess of 0.3 M\u2299, but no enrichment of oxygen, nitrogen, or sulfur. The Cygnus Loop is shown to emit [Fe XIV], indicating gas at 2 x 106 \u00b0K: this establishes the thermal nature of the x-ray emission, and casts doubt on the Loop's size and distance.
\r\n\r\nType II supernovae are shown to be consistent with a few solar masses of material at cosmic abundance. Their distances are found without reference to any other astronomical distance through a model of the expansion. Type I supernovae are shown to consist of about 1 solar mass of matter that may be 20 times enriched in iron, if the identification of [Fe II] lines at late stages is correct.
", "date": "1975", "date_type": "degree", "id_number": "CaltechETD:etd-04092004-111020", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04092004-111020", "related_url": { "items": [ { "description": "Article adapted for Chapter 2.", "type": "doi", "url": "https://doi.org/10.1086/153248" }, { "description": "Article adapted for Chapter 5.", "type": "doi", "url": "https://doi.org/10.1086/153527" }, { "description": "Article adapted for Chapter 6.", "type": "doi", "url": "https://doi.org/10.1086/181161" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Virginia Steele Scott Fund" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-04-14", "doi": "10.7907/YN9G-P338", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-04-09", "thesis_defense_date": "1974-07-26", "thesis_approved_date": "2004-04-14", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1975", "author_list": "Kirshner, Robert Paul" }, { "id": "/id/eprint/4281", "eprint_id": 4281, "rev_number": 10, "documents": [ { "id": "/id/document/7023", "doc_id": 7023, "rev_number": 2, "files": [ { "id": "/id/file/42708", "fileid": 42708, "datasetid": "document", "objectid": 7023, "filename": "Callahan_ps_1974.pdf", "mime_type": "application/pdf", "filesize": 5236699, "mtime": "2012-12-26 03:07:10", "url": "/4281/1/Callahan_ps_1974.pdf" } ], "eprint_id": 4281, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Callahan_ps_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Callahan_ps_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23552" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23552" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23552" } ] } }, { "id": "/id/document/23552", "doc_id": 23552, "rev_number": 2, "files": [ { "id": "/id/file/42706", "fileid": 42706, "datasetid": "document", "objectid": 23552, "filename": "preview.png", "mime_type": "image/png", "hash": "ac999a093dc7a15f7d6c57681e45e16a", "hash_type": "MD5", "filesize": 8242, "mtime": "2012-12-26 03:07:10", "url": "/4281/2/preview.png" } ], "eprint_id": 4281, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7023" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7023" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7023" } ] } }, { "id": "/id/document/124114", "doc_id": 124114, "rev_number": 1, "files": [ { "id": "/id/file/369544", "fileid": 369544, "datasetid": "document", "objectid": 124114, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "226c2d31b29dc9a4c61ffe58239cee0b", "hash_type": "MD5", "filesize": 18507, "mtime": "2021-06-23 23:19:07", "url": "/4281/3/indexcodes.txt" } ], "eprint_id": 4281, "pos": 3, "placement": 3, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "public", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7023" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7023" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/7023" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/81", "datestamp": "2005-11-01", "lastmod": "2020-03-10 19:07:32", "status_changed": "2009-09-25 03:15:25", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Callahan-P-S", "name": { "family": "Callahan", "given": "Philip Sidney" }, "show_email": "NO" } ] }, "title": "Observations of the solar-wind turbulence near the sun", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe solar-wind turbulence near the sun is investigated with data obtained near the superior conjunctions of Mariners 6, 7, and 9. The data are time histories of the change in the electron columnar content between the earth and spacecraft. The data were obtained with a group-phase technique which is sensitive only to the change in the columnar content. The measurement technique is discussed. The theory of power spectra is outlined. The relationship between the temporal power spectrum of the columnar content data and the comoving wave-number spectrum of the solar wind is derived. It is found that comoving spectrum is well represented by a power-law [...] of index [...]= 3.9 [...] 0.2. Comparison of the overall average spectral amplitude near the sun [...] to that near 1 a.u. shows that the turbulence declines with heliocentric distance as [...], ignoring time variations. In the region near the sun (0.07 [...] r [...] 0.22 a.u.) [...] declines more slowly. It is suggested that there is a region of enhanced turbulence near the sun. The Mariner 9 spectral amplitudes correlate with Zurich sunspot number. The data are used to investigate the relationship between McMath calcium plage regions and density enhancements intersecting the line of sight. The relationship of the present observations to theories of solar wind heating and to interplanetary scintillation observations is discussed.\r\n", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-10282005-130203", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10282005-130203", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-11-01", "doi": "10.7907/9ZFM-K287", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" }, { "id": "Whaling-W", "name": { "family": "Whaling", "given": "Ward" }, "role": "advisor" }, { "id": "Jokipii-J-R", "name": { "family": "Jokipii", "given": "J. Randolph" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-10-28", "thesis_defense_date": "1974-02-01", "thesis_approved_date": "2005-11-01", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Callahan, Philip Sidney" }, { "id": "/id/eprint/2168", "eprint_id": 2168, "rev_number": 7, "documents": [ { "id": "/id/document/3948", "doc_id": 3948, "rev_number": 2, "files": [ { "id": "/id/file/23096", "fileid": 23096, "datasetid": "document", "objectid": 3948, "filename": "Oemler_a_1974.pdf", "mime_type": "application/pdf", "filesize": 2497103, "mtime": "2012-12-26 02:47:41", "url": "/2168/1/Oemler_a_1974.pdf" } ], "eprint_id": 2168, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Oemler_a_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Oemler_a_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20583" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20583" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20583" } ] } }, { "id": "/id/document/20583", "doc_id": 20583, "rev_number": 2, "files": [ { "id": "/id/file/23094", "fileid": 23094, "datasetid": "document", "objectid": 20583, "filename": "preview.png", "mime_type": "image/png", "hash": "402118744500f77046877e92300008a8", "hash_type": "MD5", "filesize": 9041, "mtime": "2012-12-26 02:47:41", "url": "/2168/2/preview.png" } ], "eprint_id": 2168, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3948" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3948" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3948" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/21/68", "datestamp": "2008-05-27", "lastmod": "2019-12-21 02:59:54", "status_changed": "2009-09-25 02:28:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Oemler-A", "name": { "family": "Oemler", "given": "Augustus" }, "show_email": "NO" } ] }, "title": "The systematic properties of clusters of galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "Fifteen rich clusters of galaxies have been studied on photoelectrically calibrated photographic plates. These plates were measured using new automatic photometry techniques. Data in the literature have been supplemented by new observations to obtain velocity dispersions in nine of these clusters.\n\nClusters can be divided by their galaxy content into three types: spiral rich, spiral poor, and those dominated by a cD galaxy. The luminosity functions of the latter two types are very similar, and differ significantly from that of galaxies in spiral rich clusters. The surface brightness profiles of the spiral poor and cD clusters agree in severalrespects with numerical models of collapsed clusters by Aarseth, but the spiral poor clusters are too irregular and have too little central concentration to be collapsed. All of the clusters have a local minimum in their profiles which cannot be explained.\n\nSpiral rich clusters tend to be less dense than average and cD clusters more dense, but, in the mean, all clusters follow a constant density law independent of mass. The cD clusters and others with a high ratio of elliptical to spiral galaxies have mass to light ratios of about 225, while the mass to light ratio of spiral rich clusters is less than half of this value. The collapse times calculated using these mass-luminosity ratios confirm that spiral rich clusters are still collapsing while the others are close to equilibrium. The degree of mass segregation in the collapsed clusters is close to that predicted by the Aarseth models and requires that most of the cluster mass be in the galaxies themselves rather than in a cluster-wide medium.\n\nThe decrease of the number of spirals towards the center of the collapsed clusters supports the idea that SO galaxies are created by stripping the gas from spirals, and the spiral rich clusters can be expected to evolve into spiral poor clusters after collapse by this mechanism. The high proportion of elliptical galaxies in the cD clusters probably means that they are a distinct type of object, and not just a later evolutionary state of the spiral poor clusters.", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-05272008-091956", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05272008-091956", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-27", "doi": "10.7907/BT4A-JT75", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Gunn-J-E", "name": { "family": "Gunn", "given": "James E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-27", "thesis_defense_date": "1973-12-13", "thesis_approved_date": "2008-05-27", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Oemler, Augustus" }, { "id": "/id/eprint/1317", "eprint_id": 1317, "rev_number": 9, "documents": [ { "id": "/id/document/2008", "doc_id": 2008, "rev_number": 2, "files": [ { "id": "/id/file/12547", "fileid": 12547, "datasetid": "document", "objectid": 2008, "filename": "Lee_dl_1974.pdf", "mime_type": "application/pdf", "filesize": 6414915, "mtime": "2012-12-26 02:37:12", "url": "/1317/1/Lee_dl_1974.pdf" } ], "eprint_id": 1317, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Lee_dl_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Lee_dl_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18778" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18778" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18778" } ] } }, { "id": "/id/document/18778", "doc_id": 18778, "rev_number": 2, "files": [ { "id": "/id/file/12545", "fileid": 12545, "datasetid": "document", "objectid": 18778, "filename": "preview.png", "mime_type": "image/png", "hash": "32b05f5cc564686467bb2573758f927d", "hash_type": "MD5", "filesize": 9058, "mtime": "2012-12-26 02:37:12", "url": "/1317/2/preview.png" } ], "eprint_id": 1317, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2008" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2008" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2008" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/13/17", "datestamp": "2004-04-14", "lastmod": "2020-03-10 23:39:04", "status_changed": "2009-09-25 02:01:07", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lee-David-Li", "name": { "family": "Lee", "given": "David Li" }, "show_email": "NO" } ] }, "title": "Frameworks for analyzing and testing theories of gravity", "ispublished": "unpub", "full_text_status": "public", "abstract": "This thesis presents theoretical frameworks for the analysis and testing of gravitation theories - both metric and non-metric. For non-metric theories, the high-precision Eotvos-Dicke-Braginskii (EDB) experiments are demonstrated to be powerful tests of their gravitational coupling to electromagnetic interactions. All known non-metric theories are ruled out to within the precision of the EDB experiments. We present a new metric theory of gravity that cannot be distinguished from general relativity in all current and planned solar system experiments. However, this theory has very different gravitational-wave properties. Hence, we point out the need for further tests of metric theories beyond the Parametrized Post-Newtonian formalism, and emphasize the importance of the observation of gravitational waves as a tool for testing relativistic gravity in the future. A theory-independent formalism delineating the properties of weak, plane gravitational waves in metric theories is set up.\r\n\r\nGeneral conservation laws that follow from variational principles in metric theories of gravity are investigated.", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-04092004-111803", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04092004-111803", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-04-14", "doi": "10.7907/KC8C-MS78", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-04-09", "thesis_defense_date": "1974-04-22", "thesis_approved_date": "2004-04-14", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Lee, David Li" }, { "id": "/id/eprint/3818", "eprint_id": 3818, "rev_number": 9, "documents": [ { "id": "/id/document/6456", "doc_id": 6456, "rev_number": 2, "files": [ { "id": "/id/file/38810", "fileid": 38810, "datasetid": "document", "objectid": 6456, "filename": "Bieging_jh_1974.pdf", "mime_type": "application/pdf", "filesize": 10248114, "mtime": "2012-12-26 03:03:13", "url": "/3818/1/Bieging_jh_1974.pdf" } ], "eprint_id": 3818, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Bieging_jh_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Bieging_jh_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22988" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22988" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22988" } ] } }, { "id": "/id/document/22988", "doc_id": 22988, "rev_number": 2, "files": [ { "id": "/id/file/38808", "fileid": 38808, "datasetid": "document", "objectid": 22988, "filename": "preview.png", "mime_type": "image/png", "hash": "f8aa14e51e594036cdd7a48260719ac3", "hash_type": "MD5", "filesize": 8681, "mtime": "2012-12-26 03:03:12", "url": "/3818/2/preview.png" } ], "eprint_id": 3818, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6456" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6456" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6456" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/38/18", "datestamp": "2005-09-29", "lastmod": "2019-12-21 04:55:15", "status_changed": "2009-09-25 03:06:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bieging-J-H", "name": { "family": "Bieging", "given": "John Harold" }, "show_email": "NO" } ] }, "title": "Aperture synthesis observations of OH absorption in the galactic center", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe galactic center radio sources Sgr A and Sgr B2 have been mapped, by an aperture synthesis technique, in the 1667 MHz absorption line of the OH molecule. The angular resolution of the maps is [...] and the velocity resolution is 1.44 km [...]. The range of velocities covered by the maps is from -200 to +100 km [...] in the local standard of rest. The data are presented in two forms: (i) spectra of brightness temperature as a function of velocity, for fixed positions in right ascension and declination; and (ii) maps of the optical depth distribution in the spatial coordinates, for fixed velocity.\r\n\r\nThe deep absorption line at +40 km [...] in Sgr A is produced by two separate components. Both components appear to be very massive, dense clouds undergoing rapid rotation about axes perpendicular to the galactic plane. If the clouds are gravitationally bound, then their total masses must exceed [...].\r\n\r\nFifteen discrete molecular clouds are seen in absorption against Sgr B2 over a velocity range from -120 km [...] to +100 km [...]. The strong absorption feature at +60 [...] is resolved into four separate clouds, which are closely associated with the HII region GO.7-0.0. It is suggested that the ionized gas and the dense molecular clouds may be interacting dynamically to produce the observed difference in velocity between the [...] recombination line and the OH absorption lines.\r\n\r\nThe implications of these observations for various kinematical models of the galactic center are discussed. Simple models with one or two expanding and rotating rings are not adequate to explain the data.\r\n\r\nThe excitation temperature of the OH 1667 MHz transition is less than 10K, based on the maximum line temperature away from the continuum sources. However, one anomalous region north of G0.7-0.0 shows apparently thermal line emission, which implies an excitation temperature between 30K and 80K if the gas is optically thick. The thermal emission has a maximum angular extent of 12 arcminutes.\r\n\r\nThe molecular clouds fall into two groups. Those with positive radial velocities have linewidths which are, on-the average, twice as large as those for clouds with negative radial velocities. The positive-velocity clouds tend to have larger optical depths and column densities of OH. The mean value of [...] for the positive-velocity clouds is [...] , while for negative-velocity clouds, the mean is [...]. For an assumed excitation temperature of 10K, the space densities of OH molecules exceed by at least an order of magnitude the expected densities based on a theoretical model for the reaction rates of molecule formation. The parameters of the theoretical model may be inappropriate for the galactic center region.", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-09292005-082550", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09292005-082550", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-09-29", "doi": "10.7907/HD0Q-HN74", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Seielstad-G-A", "name": { "family": "Seielstad", "given": "George A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-09-29", "thesis_defense_date": "1973-12-17", "thesis_approved_date": "2005-09-29", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Bieging, John Harold" }, { "id": "/id/eprint/3344", "eprint_id": 3344, "rev_number": 7, "documents": [ { "id": "/id/document/5865", "doc_id": 5865, "rev_number": 2, "files": [ { "id": "/id/file/34828", "fileid": 34828, "datasetid": "document", "objectid": 5865, "filename": "Veeder_gj_1974.pdf", "mime_type": "application/pdf", "filesize": 2967584, "mtime": "2012-12-26 02:59:14", "url": "/3344/1/Veeder_gj_1974.pdf" } ], "eprint_id": 3344, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Veeder_gj_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Veeder_gj_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22405" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22405" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22405" } ] } }, { "id": "/id/document/22405", "doc_id": 22405, "rev_number": 2, "files": [ { "id": "/id/file/34826", "fileid": 34826, "datasetid": "document", "objectid": 22405, "filename": "preview.png", "mime_type": "image/png", "hash": "d50525e1f66055b59c59810714cf5139", "hash_type": "MD5", "filesize": 9415, "mtime": "2012-12-26 02:59:14", "url": "/3344/2/preview.png" } ], "eprint_id": 3344, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5865" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5865" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5865" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/33/44", "datestamp": "2008-09-12", "lastmod": "2019-12-20 19:54:01", "status_changed": "2009-09-25 02:57:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Veeder-G-J", "name": { "family": "Veeder", "given": "Glenn J." }, "show_email": "NO" } ] }, "title": "Temperatures and luminosities of M type dwarfs from infrared photometry", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nBroad-band infrared photometry at 1.65, 2.2 and 3.5[...] has yielded the first accurate bolometric magnitudes for a large number of M dwarfs. The intrinsic dispersion in these stars is found to be [\u2026] 0.4 magnitudes in M[\u2026] vs. V-K and M[\u2026] vs. R-I magnitude-color diagrams. This dispersion in the lower main sequence may be the result of differential blanketing in the UBVRI filter bands and thus there may be no such thing as a unique main sequence for the intrinsically faint M dwarfs. Scanner observations from 4500[\u2026]to 10000[\u2026] show severe blanketing by TiO in cool M dwarfs, but analysis shows that one parameter is sufficient to describe the blanketing in all of the UBVRI bands for all types of M dwarfs. In general, late M dwarfs seem to have lower effective temperatures than are predicted by theoretical models. Stars with hydrogen lines in emission average 0.2 to 0.3 bolometric magnitudes brighter than M dwarfs without any emission lines. The existence of flare stars with old disk space motions and also the existence of some flare stars below the main sequence complicates the picture of these stars as a pre-main sequence evolutionary stage. M dwarfs that belong to the halo population on the basis of their large space motions tend to be subluminous in M[\u2026] vs. V-K and M[\u2026] vs. R-I magnitude-color diagrams although there is a large scatter among the few objects of this type.\n\nThe data for late dwarfs with known masses imply the empirical mass-luminosity relation: [\u2026] for stars fainter than M[\u2026] = 7.5. In addition, the late M dwarfs are found to account for all of the \"missing mass\" in the plane of the galaxy.\n", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-09052008-144355", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09052008-144355", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-12", "doi": "10.7907/CRWW-Y818", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-05", "thesis_defense_date": "1973-08-21", "thesis_approved_date": "2008-09-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Veeder, Glenn J." }, { "id": "/id/eprint/4501", "eprint_id": 4501, "rev_number": 13, "documents": [ { "id": "/id/document/7317", "doc_id": 7317, "rev_number": 3, "files": [ { "id": "/id/file/44641", "fileid": 44641, "datasetid": "document", "objectid": 7317, "filename": "Lightman_ap_1974.pdf", "mime_type": "application/pdf", "filesize": 9448931, "mtime": "2012-12-26 03:09:16", "url": "/4501/1/Lightman_ap_1974.pdf" } ], "eprint_id": 4501, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Lightman_ap_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Lightman_ap_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23845" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23845" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23845" } ] } }, { "id": "/id/document/15172", "doc_id": 15172, "rev_number": 4, "files": [ { "id": "/id/file/204371", "fileid": 204371, "datasetid": "document", "objectid": 15172, "filename": "Lightman_Permission.pdf", "mime_type": "application/pdf", "filesize": 116640, "mtime": "2016-08-22 21:17:25", "url": "/4501/2/Lightman_Permission.pdf" } ], "eprint_id": 4501, "pos": 2, "format": "application/pdf", "format_desc": "author ok 2012", "language": "en", "security": "internal", "license": "other", "main": "Lightman_Permission.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", 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"http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7317" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7317" } ] } }, { "id": "/id/document/73134", "doc_id": 73134, "rev_number": 2, "files": [ { "id": "/id/file/204370", "fileid": 204370, "datasetid": "document", "objectid": 73134, "filename": "preview.png", "mime_type": "image/png", "hash": "96920496b995d44d20bed1eeb5274747", "hash_type": "MD5", "filesize": 58683, "mtime": "2016-08-22 21:17:25", "url": "/4501/4/preview.png" } ], "eprint_id": 4501, "pos": 4, "placement": 4, "format": "image/png", "language": "en", "security": "internal", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15172" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/15172" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15172" } ] } }, { "id": "/id/document/124347", "doc_id": 124347, "rev_number": 1, "files": [ { "id": "/id/file/369777", "fileid": 369777, "datasetid": "document", "objectid": 124347, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "d97780dbad5df3da506a779ff58d8b7a", "hash_type": "MD5", "filesize": 411, "mtime": "2021-06-23 23:29:07", "url": "/4501/5/indexcodes.txt" } ], "eprint_id": 4501, "pos": 5, "placement": 5, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from application/pdf to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/15172" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/15172" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/15172" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/45/01", "datestamp": "2003-11-11", "lastmod": "2020-03-10 23:39:07", "status_changed": "2009-09-25 03:19:45", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lightman-A-P", "name": { "family": "Lightman", "given": "Alan Paige" }, "show_email": "NO" } ] }, "title": "Time-dependent accretion disks around compact objects. Theoretical frameworks for analyzing and testing gravitation theories", "ispublished": "unpub", "full_text_status": "public", "abstract": "Part I.\r\n\r\nThe theory of time-independent accretion disks around compact objects is developed, generalizing the stationary models of various authors to allow time dependence on the radial-flow time scale. Equations are derived for the time evolution of matter surface density [Sigma] and for implicit expressions of relevant disk variables in terms of [Sigma]. Analytic and numerical studies of these equations yield numerical models of mass accretion from a disk onto a compact object and a discovery of the unstable nature of the \"inner region\" of the disk, causing a breakdown of current accretion disk models.\r\n\r\nPart II.\r\n\r\nTheoretical frameworks for analyzing and testing gravitation theories are developed for both nonmetric and metric theories. Highly precise experimental confirmation of the Weak Equivalence Principle is shown to be deadly if not fatal evidence for ruling out all nonmetric theories of gravity. For the class of metric theories we demonstrate the necessity for going beyond current frameworks of analysis (e.g.,the PPN framework) by constructing a new theory of gravity identical to GRT in the Post-Newtonian limit. As a first step in transcending current frameworks, we develop a formalism for delineating and testing all metric theories of gravity on the basis of their gravitational-wave properties and thereby emphasize gravitational-wave observations as a future tool for testing gravitation theories. We also investigate conservation laws and some common properties of Lagrangian-based metric theories of gravity.", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-11112003-091837", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-11112003-091837", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-11-11", "doi": "10.7907/1QYN-CQ82", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-11-11", "thesis_defense_date": "1974-02-27", "thesis_approved_date": "2003-11-11", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Lightman, Alan Paige" }, { "id": "/id/eprint/3219", "eprint_id": 3219, "rev_number": 7, "documents": [ { "id": "/id/document/5710", "doc_id": 5710, "rev_number": 2, "files": [ { "id": "/id/file/33770", "fileid": 33770, "datasetid": "document", "objectid": 5710, "filename": "Shectman_sa_1974.pdf", "mime_type": "application/pdf", "filesize": 2716293, "mtime": "2012-12-26 02:58:12", "url": "/3219/1/Shectman_sa_1974.pdf" } ], "eprint_id": 3219, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Shectman_sa_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Shectman_sa_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22252" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22252" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22252" } ] } }, { "id": "/id/document/22252", "doc_id": 22252, "rev_number": 2, "files": [ { "id": "/id/file/33768", "fileid": 33768, "datasetid": "document", "objectid": 22252, "filename": "preview.png", "mime_type": "image/png", "hash": "307f9c41e238d52c3d979e29f4531479", "hash_type": "MD5", "filesize": 9384, "mtime": "2012-12-26 02:58:12", "url": "/3219/2/preview.png" } ], "eprint_id": 3219, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5710" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5710" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5710" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/19", "datestamp": "2008-09-09", "lastmod": "2019-12-20 19:59:05", "status_changed": "2009-09-25 02:54:44", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shectman-S-A", "name": { "family": "Shectman", "given": "Stephen Alan" }, "show_email": "NO" } ] }, "title": "Clusters of galaxies and the cosmic light", "ispublished": "unpub", "full_text_status": "public", "abstract": "Because galaxies cluster in space, the cosmic background light due to galaxies is not smoothly distributed on the night sky. Part I predicts spatial power spectra for the cosmic light fluctuations, based on the luminosity function for nearby galaxies and on the dumpiness of the galaxy distribution derived from galaxy counts. Part II describes a measurement of the spatial power spectrum of the cosmic light on a series of photographic plates taken with the Palomar 48-inch (122cm) Schmidt camera. This power spectrum is interpreted to provide a measure of the covariance of the galaxy distribution and the mean emissivity of galaxies in space.\n", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-08252008-081823", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08252008-081823", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/APSH-4Q39", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Gunn-J-E", "name": { "family": "Gunn", "given": "James E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-25", "thesis_defense_date": "1973-06-28", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Shectman, Stephen Alan" }, { "id": "/id/eprint/2555", "eprint_id": 2555, "rev_number": 9, "documents": [ { "id": "/id/document/4814", "doc_id": 4814, "rev_number": 2, "files": [ { "id": "/id/file/27856", "fileid": 27856, "datasetid": "document", "objectid": 4814, "filename": "Shaffer_db_1974.pdf", "mime_type": "application/pdf", "filesize": 3355470, "mtime": "2012-12-26 02:52:32", "url": "/2555/1/Shaffer_db_1974.pdf" } ], "eprint_id": 2555, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Shaffer_db_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Shaffer_db_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21366" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21366" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21366" } ] } }, { "id": "/id/document/21366", "doc_id": 21366, "rev_number": 2, "files": [ { "id": "/id/file/27854", "fileid": 27854, "datasetid": "document", "objectid": 21366, "filename": "preview.png", "mime_type": "image/png", "hash": "b5e00d5317185c7da25a1b279d1f7544", "hash_type": "MD5", "filesize": 9588, "mtime": "2012-12-26 02:52:32", "url": "/2555/2/preview.png" } ], "eprint_id": 2555, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4814" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4814" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4814" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/25/55", "datestamp": "2008-06-12", "lastmod": "2019-12-21 03:08:01", "status_changed": "2009-09-25 02:40:18", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shaffer-D-B", "name": { "family": "Shaffer", "given": "David Bruce" }, "show_email": "NO" } ] }, "title": "The structure of compact radio sources at 10.7 GHz", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nVery long baseline interferometry has been used to study the compact structure of seven radio sources at 10709 MHz ([...] = 2.8 cm). The observations, the first of a series, were made on April 28 - May 1, 1972, using the NRAO Mark II recording system. Antennas of the Owens Valley Radio Observatory (California), the Harvard Radio Astronomy Station (Texas), and the National Radio Astronomy Observatory (West Virginia) were used to give three baselines that greatly improved the (u,v)-plane coverage compared to the coverage of previously used single baselines. The three baselines had lengths of 119, 84, and 54x10[...] [...].\r\n\r\nThe observed sources were 3C 84, NRAO 150, OJ 287, 4C 39.25, 3C 273, PKS 2134+004, and VRO 42.22.01 (BL Lac). They were tracked by all three antennas during the time of mutual visibility, giving 8 to 11.5 hours of continuous coverage. With the maximum baseline of 119x10[...] [...] and a u-v cell size of ~40x10[...] [...], it is unlikely that we have missed any important structure information in the range 0[...]0005 to 0[...]005.\r\n\r\nFourier inversion of the observations was impossible because there was no phase calibration, and model fitting procedures were used to interpret the data. For five of the sources (NRAO 150, OJ 287, 4C 39.25, 3C 273, and VRO 42.22.01) models were found that fit the observations quite well. For 3C 84 and PKS 2134+004 no simple model could be found, but a rough idea of the source structure was still possible. For most of the sources, interferometric results at other frequencies and resolutions are consistent with the present findings, and a joint interpretation is given.\r\n\r\nFor all the sources except OJ 287 (which looks like a point source at our resolution and was used to calibrate the correlated flux density scale) and possibly NRAO 150, two or more separate components are required to match the observations. Component separations range from 0[...]0006 to 0[...]005 and their sizes from [...]0[...]0003 to ~0[...]002. Components less than ~0[...]002 contribute 0.85 or more of the total 10.7 GHz flux density for all the sources. Assuming synchrotron self-absorbed components, the magnetic fields in the compact sources are %10-3\u00b11 gauss. This value is less than the equi-partition field, and the individual components are expected to expand from particle pressure.\r\n\r\nSuggestions are given for additional observations to improve our knowledge of the structure and nature of compact sources.", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-06112008-140732", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06112008-140732", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-06-12", "doi": "10.7907/FER5-8H88", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-06-11", "thesis_defense_date": "1973-09-25", "thesis_approved_date": "2008-06-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Shaffer, David Bruce" }, { "id": "/id/eprint/2997", "eprint_id": 2997, "rev_number": 19, "documents": [ { "id": "/id/document/5385", "doc_id": 5385, "rev_number": 3, "files": [ { "id": "/id/file/31683", "fileid": 31683, "datasetid": "document", "objectid": 5385, "filename": "Teukolsky_sa_1974.pdf", "mime_type": "application/pdf", "filesize": 11322674, "mtime": "2012-12-26 02:56:07", "url": "/2997/1/Teukolsky_sa_1974.pdf" } ], "eprint_id": 2997, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Scanned (no OCR) Teukolsky_sa_1974", "language": "en", "security": "internal", "license": "other", "main": "Teukolsky_sa_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/104561" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/104561" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/104561" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/29/97", "datestamp": "2006-08-02", "lastmod": "2020-10-09 22:24:01", "status_changed": "2009-09-25 02:49:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Teukolsky-Saul-Arno", "name": { "family": "Teukolsky", "given": "Saul Arno" }, "orcid": "0000-0001-9765-4526", "show_email": "NO" } ] }, "title": "Perturbations of a Rotating Black Hole", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "note": "Einstein Prize citation: \"For outstanding contributions to observational tests of general relativity with theories of gravitational waves, astrophysical black holes, and neutron stars.\"", "abstract": "Decoupled, separable equations describing perturbations of a Kerr black hole are derived. These equations can be used to study black-hole processes involving scalar, electromagnetic, neutrino or gravitational fields. A number of astrophysical applications are made: Misner's idea that gravitational synchrotron radiation might explain Weber's observations is shown to be untenable; rotating black holes are shown to be stable against small perturbations; energy amplification by \"superradiant scattering\" of waves off a rotating black hole is computed; the \"spin down\" (loss of angular momentum) of a rotating black hole caused by a stationary non-axisymmetric perturbation is calculated.", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-08022006-094950", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08022006-094950", "related_url": { "items": [ { "description": "Article adapted for Part III (a).", "type": "doi", "url": "https://doi.org/10.1086/151796" }, { "description": "Article adapted for Part III (b).", "type": "doi", "url": "https://doi.org/10.1038/238211a0" }, { "description": "Article adapted for Part IV (a).", "type": "doi", "url": "https://doi.org/10.1103/physrevlett.29.1114" }, { "description": "Article adapted for Appendix.", "type": "doi", "url": "https://doi.org/10.1086/152066" }, { "description": "Einstein Prize (APS) announcement, 2021", "type": "org", "url": "https://www.aps.org/programs/honors/prizes/prizerecipient.cfm?last_nm=Teukolsky&first_nm=Saul&year=2021" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Pretoria Portland Cement Company" }, { "agency": "United States Steel Foundation" }, { "agency": "NSF", "grant_number": "GP-28027" }, { "agency": "NSF", "grant_number": "GP-27304" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-08-02", "doi": "10.7907/N3AW-PV92", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-08-02", "thesis_defense_date": "1973-07-19", "thesis_approved_date": "2006-08-02", "thesis_awards": "Einstein Prize (APS), 2021. Member of the US National Academy of Sciences, 2003. Fellow of the American Academy of Arts and Sciences, 1996.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Teukolsky, Saul Arno" }, { "id": "/id/eprint/2978", "eprint_id": 2978, "rev_number": 13, "documents": [ { "id": "/id/document/5360", "doc_id": 5360, "rev_number": 3, "files": [ { "id": "/id/file/31511", "fileid": 31511, "datasetid": "document", "objectid": 5360, "filename": "Sorkin_rd_1974.pdf", "mime_type": "application/pdf", "filesize": 3028537, "mtime": "2012-12-26 02:55:58", "url": "/2978/1/Sorkin_rd_1974.pdf" } ], "eprint_id": 2978, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Sorkin_rd_1974.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21908" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21908" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21908" } ] } }, { "id": "/id/document/16521", "doc_id": 16521, "rev_number": 3, "files": [ { "id": "/id/file/203932", "fileid": 203932, "datasetid": "document", "objectid": 16521, "filename": "Sorkin_Rafael_D_1974.txt", "mime_type": "text/plain", "filesize": 1676, "mtime": "2016-08-22 21:16:25", "url": "/2978/2/Sorkin_Rafael_D_1974.txt" } ], "eprint_id": 2978, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Sorkin_Rafael_D_1974.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/21908", "doc_id": 21908, "rev_number": 2, "files": [ { "id": "/id/file/31509", "fileid": 31509, "datasetid": "document", "objectid": 21908, "filename": "preview.png", "mime_type": "image/png", "hash": "5de00a676047b1ec4c7d78765de3beda", "hash_type": "MD5", "filesize": 8953, "mtime": "2012-12-26 02:55:58", "url": "/2978/3/preview.png" } ], "eprint_id": 2978, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5360" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5360" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5360" } ] } }, { "id": "/id/document/123268", "doc_id": 123268, "rev_number": 1, "files": [ { "id": "/id/file/368677", "fileid": 368677, "datasetid": "document", "objectid": 123268, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "a2af1aa9b1a4a4ac4f1e1fa3930e35d9", "hash_type": "MD5", "filesize": 794, "mtime": "2021-06-23 22:29:30", "url": "/2978/4/indexcodes.txt" } ], "eprint_id": 2978, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from text/plain to indexcodes", "language": "en", "security": "internal", "license": "other", "main": "indexcodes.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/16521" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16521" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16521" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/29/78", "datestamp": "2007-07-24", "lastmod": "2023-03-27 19:17:47", "status_changed": "2009-09-25 02:48:34", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sorkin-Rafael-D", "name": { "family": "Sorkin", "given": "Rafael D." }, "show_email": "NO" } ] }, "title": "Development of Simplectic Methods for the Metrical and Electromagnetic Fields", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "The simplectic approach to discretization, as introduced by Regge, may be better suited to computer calculation than is the usual \"finite difference\" approach. This thesis describes a general simplectic formalism for coupled electromagnetic and metric fields including detailed discussion of nets for closed and open spacetimes. The rendering of this formalism into computer algorithms is then described, and indicative numerical results are reported.", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-07242007-143000", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-07242007-143000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-07-24", "doi": "10.7907/8Z57-5H36", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Gunn-J-E", "name": { "family": "Gunn", "given": "James E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-07-24", "thesis_defense_date": "1974-02-15", "thesis_approved_date": "2007-07-24", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1974", "author_list": "Sorkin, Rafael D." }, { "id": "/id/eprint/10392", "eprint_id": 10392, "rev_number": 18, "documents": [ { "id": "/id/document/82206", "doc_id": 82206, "rev_number": 2, "files": [ { "id": "/id/file/232207", "fileid": 232207, "datasetid": "document", "objectid": 82206, "filename": "Kwan_JYK_1973.pdf", "mime_type": "application/pdf", "hash": "ad3e7f859aebe8dda4431f159d671707", "hash_type": "MD5", "filesize": 24975678, "mtime": "2017-08-25 21:55:29", "url": "/10392/1/Kwan_JYK_1973.pdf" } ], "eprint_id": 10392, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Kwan_JYK_1973.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 87, "dir": "disk0/00/01/03/92", "datestamp": "2017-08-25 22:20:55", "lastmod": "2020-03-10 19:16:40", "status_changed": "2017-08-25 22:20:55", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kwan-John-Ying-Kuen", "name": { "family": "Kwan", "given": "John Ying-Kuen" } } ] }, "title": "Polarization Properties of Astrophysical Masers", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Observed interstellar OH and H2O maser lines at 18 cm and\r\n1.35 cm exhibit unusual polarization properties. The OH emitters with the\r\nhighest brightness temperatures, usually associated with H II regions, almost\r\nalways show a high degree of circular polarization. The H2O maser line,\r\non the other hand, is rarely polarized, and then only linearly polarized.
\r\n\r\nThe preference for circular polarization in the brightest OH\r\nsources was attributed by Litvak to the mechanism of parametric down-conversion.\r\nIn this process the higher-frequency components of a Zeeman\r\nsplit maser line are down-converted to lower-frequency components and to\r\nan electron cyclotron wave. This mechanism is shown to be too weak to be\r\nof importance in astrophysical masers.
\r\n\r\nThe polarization properties of the OH and H2O masers are related \r\nto the physical conditions in the maser clouds. It is found that the magnetic\r\nfield, the plasma, and trapped infrared lines in maser sources play an\r\nimportant role in determining the polarization on the emitted radiation.
", "date": "1973", "date_type": "degree", "id_number": "CaltechTHESIS:08252017-145131867", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08252017-145131867", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "IBM Foundation" }, { "agency": "Earle C. Anthony Foundation" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-25 22:20:55", "doi": "10.7907/906J-2N21", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1972-11-20", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1973", "author_list": "Kwan, John Ying-Kuen" }, { "id": "/id/eprint/3224", "eprint_id": 3224, "rev_number": 9, "documents": [ { "id": "/id/document/5715", "doc_id": 5715, "rev_number": 2, "files": [ { "id": "/id/file/33806", "fileid": 33806, "datasetid": "document", "objectid": 5715, "filename": "Greisen_ew_1973.pdf", "mime_type": "application/pdf", "filesize": 9388474, "mtime": "2012-12-26 02:58:14", "url": "/3224/1/Greisen_ew_1973.pdf" } ], "eprint_id": 3224, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Greisen_ew_1973.pdf", "language": "en", "security": "public", "license": "other", "main": "Greisen_ew_1973.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22257" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22257" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22257" } ] } }, { "id": "/id/document/22257", "doc_id": 22257, "rev_number": 2, "files": [ { "id": "/id/file/33804", "fileid": 33804, "datasetid": "document", "objectid": 22257, "filename": "preview.png", "mime_type": "image/png", "hash": "c13cc26badac0e80975d1fcdc35b1120", "hash_type": "MD5", "filesize": 9520, "mtime": "2012-12-26 02:58:14", "url": "/3224/2/preview.png" } ], "eprint_id": 3224, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5715" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5715" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5715" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/24", "datestamp": "2008-09-09", "lastmod": "2019-12-20 19:48:39", "status_changed": "2009-09-25 02:54:49", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Greisen-E-W", "name": { "family": "Greisen", "given": "Eric Winslow" }, "show_email": "NO" } ] }, "title": "Aperture synthesis of interstellar neutral hydrogen in absorption", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe Owens Valley Radio Observatory interferometer has been used to carry out a program of aperture synthesis in the interstellar neutral hydrogen line. Maps having resolutions of 1 KHz and about 1.3 arc minutes have been produced using a novel Fourier inversion procedure which is discussed in some detail. The equipment, observing procedure, noise, and gaussian analysis of spectra are also treated.\r\n\r\nThe Perseus arm feature in the spectrum of Cygnus A is of low optical depth but reveals considerable spatial structure. The data suggest that the hydrogen is located in a thin shell expanding at 2 km/sec, with a radius around 9.7 parsecs and a total mass of 175 solar masses. The Perseus arm feature in the spectrum of Cassiopeia A contains very large amounts of hydrogen with extremely complicated spatial structure. The results may be explained qualitatively by the two-arm spiral shock model of the Galaxy. The principal component in the spectrum of the Crab Nebula is found to show a considerable velocity gradient across the source and appears to contain several condensations within a large, less dense cloud. The absorption feature in the spectrum of 3C353 appears to have a gradient in the dispersion of one component. If real, this result suggests scale lengths in the interstellar hydrogen as small as 0.14 parsecs. The absorption spectra of W12, 3C147, Cygnus A (local arm), and 3C123 are also discussed briefly.\r\n\r\nUpper limits to the temperature as low as 50\u00b0K are found for some of the spectral components although upper limits between 80 and 160\u00b0K are more common. Hydrogen clouds with diameters about 1 parsec and densities on the order of 100 cm[\u2026] are shown to be common. The implications of these results for the two-phase model of the interstellar medium are discussed.\r\n", "date": "1973", "date_type": "degree", "id_number": "CaltechETD:etd-08252008-150426", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08252008-150426", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/3A2K-C664", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-25", "thesis_defense_date": "1972-07-31", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1973", "author_list": "Greisen, Eric Winslow" }, { "id": "/id/eprint/3221", "eprint_id": 3221, "rev_number": 9, "documents": [ { "id": "/id/document/5712", "doc_id": 5712, "rev_number": 2, "files": [ { "id": "/id/file/33784", "fileid": 33784, "datasetid": "document", "objectid": 5712, "filename": "Press_wh_1973.pdf", "mime_type": "application/pdf", "filesize": 7006451, "mtime": "2012-12-26 02:58:13", "url": "/3221/1/Press_wh_1973.pdf" } ], "eprint_id": 3221, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Press_wh_1973.pdf", "language": "en", "security": "public", "license": "other", "main": "Press_wh_1973.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22254" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22254" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22254" } ] } }, { "id": "/id/document/22254", "doc_id": 22254, "rev_number": 2, "files": [ { "id": "/id/file/33782", "fileid": 33782, "datasetid": "document", "objectid": 22254, "filename": "preview.png", "mime_type": "image/png", "hash": "23d8c63a722b14933dd2578ff14cb657", "hash_type": "MD5", "filesize": 8135, "mtime": "2012-12-26 02:58:12", "url": "/3221/2/preview.png" } ], "eprint_id": 3221, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5712" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5712" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5712" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/21", "datestamp": "2008-09-09", "lastmod": "2020-03-10 23:39:06", "status_changed": "2009-09-25 02:54:47", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Press-W-H", "name": { "family": "Press", "given": "William H." }, "show_email": "NO" } ] }, "title": "Applications of black-hole perturbation techniques", "ispublished": "unpub", "full_text_status": "public", "abstract": "Separable, decoupled differential equations which describe gravitational, electromagnetic, and scalar perturbations of nonrotating (Schwarzschild) and rotating (Kerr) black holes have recently become available. Fortuitously, many interesting astrophysical processes near black holes can accurately be studied with these perturbation equations. A number of such processes are here investigated (as well as some matters of principle in pure relativity): \"vibrations\" of black holes, and the long wave-trains of gravitational waves which such vibrations may generate; the spectrum and intensity of gravitational radiation from a particle falling radially into a Schwarzschild hole; the physical significance of the Newman-Penrose conserved quantities, the result that they are never physically measurable and do not always exist; the time evolution of a rotating black hole immersed in a static scalar field, a quantitative calculation of the hole's \"spin-down\" and \"alignment\"; scalar-field calculations of superradiant wave scattering from a rotating black hole, and of the possibility of \"floating orbits\" \u2014 these are both wave processes which extract a hole's rotational energy. Included is a discussion of how these scalar-field results can be extended to the electromagnetic and gravitational cases. The most important perturbation problem yet to be solved is the question of whether rotating black holes are stable (against processes which would spontaneously emit gravitational waves). The astrophysical implications of instabilities are discussed, and a method for deciding the stability question (on which work is in progress) is outlined in detail. An appendix includes additional work on peripherally related matters. Several papers included in this thesis are extended from their published form by a more detailed discussion of numerical methods.\r\n", "date": "1973", "date_type": "degree", "id_number": "CaltechETD:etd-08252008-111253", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08252008-111253", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/0HKZ-DJ23", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-25", "thesis_defense_date": "1972-10-20", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1973", "author_list": "Press, William H." }, { "id": "/id/eprint/3183", "eprint_id": 3183, "rev_number": 10, "documents": [ { "id": "/id/document/5647", "doc_id": 5647, "rev_number": 3, "files": [ { "id": "/id/file/33391", "fileid": 33391, "datasetid": "document", "objectid": 5647, "filename": "Purcell_gh_1973.pdf", "mime_type": "application/pdf", "filesize": 5775652, "mtime": "2012-12-26 02:57:47", "url": "/3183/1/Purcell_gh_1973.pdf" } ], "eprint_id": 3183, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Purcell_gh_1973.pdf", "language": "en", "security": "public", "license": "other", "main": "Purcell_gh_1973.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22190" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22190" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22190" } ] } }, { "id": "/id/document/22190", "doc_id": 22190, "rev_number": 3, "files": [ { "id": "/id/file/33389", "fileid": 33389, "datasetid": "document", "objectid": 22190, "filename": "preview.png", "mime_type": "image/png", "hash": "bda4f88e446096c14ca3b7074ca21571", "hash_type": "MD5", "filesize": 9221, "mtime": "2012-12-26 02:57:47", "url": "/3183/2/preview.png" } ], "eprint_id": 3183, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5647" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5647" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5647" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/83", "datestamp": "2008-09-09", "lastmod": "2021-04-16 22:10:53", "status_changed": "2009-09-25 02:53:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Purcell-G-H", "name": { "family": "Purcell", "given": "George H." }, "show_email": "NO" } ] }, "title": "The structure of compact radio sources at 606 MHz", "ispublished": "unpub", "full_text_status": "public", "abstract": "Long-baseline interferometry has been used to study the structure of thirteen compact radio sources at 606 MHz. The baseline was 3324 kilometers long and nearly east-west in orientation, so that the maximum angular resolution was about a hundredth of a second of arc for each source.\r\n\r\nThere were two series of observations, made on June 29 to July 1, 1971, and February 3 to 6, 1972. For most of the sources observed in each session, the correlated flux was measured from ten to forty times over a wide range of hour angle, with a standard error for each measurement of about 0.12 flux unit. A few sources were observed less often. Simple source models were then fitted to the data and compared to the models proposed by other observers.\r\n\r\nThe data for most of the sources were found to be consistent with models containing an elliptical halo concentric with an unresolved core. 3C 147, 3C 273, and 3C 279 appear to be more complicated, however. The observations of 3C 84, 3C 279, and 3C 345 also show evidence of weak structure at relatively large distances from the strong central components.\r\n\r\nP1345+12 and CTD 93 were observed only in the first session, and 3C 120 and 3C 286 only in the second session. CTA 21, 3C 84, 3C 147, 3C 273, 3C 279, 3C 345, 3C 380, CTA 102, and 3C 454.3 were observed in both sessions, and all but CTA 21 and 3C 380 gave strong evidence of changes in flux or structure during the interim. These changes appear to be intrinsic to the sources, and not the result of instrumental effects or scintillation phenomena.\r\n", "date": "1973", "date_type": "degree", "id_number": "CaltechETD:etd-08212008-100027", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08212008-100027", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/8jjw-z848", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Cohen-M-H", "name": { "family": "Cohen", "given": "Marshall H." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-21", "thesis_defense_date": "1973-05-14", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1973", "author_list": "Purcell, George H." }, { "id": "/id/eprint/2167", "eprint_id": 2167, "rev_number": 6, "documents": [ { "id": "/id/document/3947", "doc_id": 3947, "rev_number": 2, "files": [ { "id": "/id/file/23089", "fileid": 23089, "datasetid": "document", "objectid": 3947, "filename": "Shields_ga_1973.pdf", "mime_type": "application/pdf", "filesize": 3914251, "mtime": "2012-12-26 02:47:41", "url": "/2167/1/Shields_ga_1973.pdf" } ], "eprint_id": 2167, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Shields_ga_1973.pdf", "language": "en", "security": "public", "license": "other", "main": "Shields_ga_1973.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20582" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20582" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20582" } ] } }, { "id": "/id/document/20582", "doc_id": 20582, "rev_number": 2, "files": [ { "id": "/id/file/23087", "fileid": 23087, "datasetid": "document", "objectid": 20582, "filename": "preview.png", "mime_type": "image/png", "hash": "0cf4aa83c01128d8bf78a1c25daeff55", "hash_type": "MD5", "filesize": 10462, "mtime": "2012-12-26 02:47:41", "url": "/2167/2/preview.png" } ], "eprint_id": 2167, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3947" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3947" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3947" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/21/67", "datestamp": "2008-05-27", "lastmod": "2019-12-21 02:22:12", "status_changed": "2009-09-25 02:28:23", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shields-G-A", "name": { "family": "Shields", "given": "Gregory Alan" }, "show_email": "NO" } ] }, "title": "Ionization structure and emission line intensities of Seyfert galaxy nuclei", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThe ionizing radiation spectrum, geometry, and chemical abundances of the nuclei of the Seyfert galaxies NGC 1068 and 3C 120 are studied with the aid of detailed computer models. These objects represent opposite extremes of the Seyfert galaxy spectral types, but analysis indicates that they are similar in ionizing radiation and nebular geometry. The quantitative success of the models for the high excitation lines supports the idea that photoionization by a central continuum source is the ionization mechanism. However, the low excitation lines may indicate the importance of another process. The most attractive explanation of the observations of both 3C 120 and NGC 1068 involves ionizing radiation similar to that from a black body at 175,000\u00b0 K with a radius of about 1 a.u, rather than an exponential or power law continuum. Most of the mass ([...]) is contained in a region of gaseous filaments with densities up to about [...] and a radius near 50 pc, which constitutes the entire emission line region of NGC 1068 and the narrow line region of 3C 120. The broad permitted emission lines of 3C 120 come from an additional region of dense, narrow filaments with velocities up to [...] km s-1 located about a parsec from the continuum source. 3C 120 probably has the abnormally large helium abundance N(He)/N(H) = 0.22, but observations are suggested to test an alternative hypothesis involving X-ray ionization. Important constraints provided by existing radio, infrared, and X-ray observations are discussed, and the importance of ultraviolet measurements is emphasized.\n", "date": "1973", "date_type": "degree", "id_number": "CaltechETD:etd-05272008-083324", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05272008-083324", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-27", "doi": "10.7907/DAZ1-4251", "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" }, "role": "chair" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-27", "thesis_defense_date": "1972-10-16", "thesis_approved_date": "2008-05-27", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1973", "author_list": "Shields, Gregory Alan" }, { "id": "/id/eprint/874", "eprint_id": 874, "rev_number": 13, "documents": [ { "id": "/id/document/1307", "doc_id": 1307, "rev_number": 3, "files": [ { "id": "/id/file/8221", "fileid": 8221, "datasetid": "document", "objectid": 1307, "filename": "Ward_wr_1973.pdf", "mime_type": "application/pdf", "filesize": 8967564, "mtime": "2012-12-26 02:33:06", "url": "/874/1/Ward_wr_1973.pdf" } ], "eprint_id": 874, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Ward_wr_1973.pdf", "language": "en", "security": "public", "license": "other", "main": "Ward_wr_1973.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18106" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18106" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18106" } ] } }, { "id": "/id/document/18106", "doc_id": 18106, "rev_number": 3, "files": [ { "id": "/id/file/8219", "fileid": 8219, "datasetid": "document", "objectid": 18106, "filename": "preview.png", "mime_type": "image/png", "hash": "2df712e6f55bc075caf03bf1ab3ec2de", "hash_type": "MD5", "filesize": 10303, "mtime": "2012-12-26 02:33:06", "url": "/874/2/preview.png" } ], "eprint_id": 874, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1307" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/1307" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1307" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/08/74", "datestamp": "2009-03-06", "lastmod": "2020-11-17 01:39:00", "status_changed": "2009-09-25 01:48:28", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ward-William-Roger", "name": { "family": "Ward", "given": "William Roger" }, "show_email": "NO" } ] }, "title": "I. The Formation of Planetesimals. II. Tidal Friction and Generalized Cassini's Laws in the Solar System", "ispublished": "unpub", "full_text_status": "public", "keywords": "Planetary Science", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nIn Part 1, four stages in the accretion of planetesimals are described. The initial stage is the condensation of dust particles from the gaseous solar nebula as it cools. These dust particles settle into a thin disk which is gravitationally unstable. A first generation of planetesimals, whose radii range up to ~10\u207b\u00b9 kilometer, form from the dust disk by direct gravitational collapse to solid densities on a time scale of order one year. The resulting disk, composed of first generation planetesimals, is still gravitationally unstable and the planetesimals are grouped into clusters containing approximately 10\u2074 members. The contraction of these clusters is controlled by the rate at which gas drag damps their internal rotational and random kinetic energies. On a time scale of a few thousand years, the clusters contract to form a second generation of planetesimals having radii of the order of a few kilometers. Further coalescence of planetesimals proceeds by collisions which seem capable of producing objects with a growth rate of ~15 cm. yr\u207b\u00b9 at one A.U. The final stage of accretion during which planet-sized objects form is not considered here.
\r\n\r\nIn Part 2 of this thesis, an investigation of a dynamical problem which has considerable application to the solar system is undertaken. The evolution of the obliquity of an object is determined when under the influence of three phenomena: (1) the precession of the object's orbit plane, (2) the precession of the object's spin axis, and (3) tidal friction. In the absence of tidal friction, it is concluded that if the period for precession of the spin axis is much shorter than the orbit precession period, the obliquity of the object will remain very nearly constant in spite of the movement of the orbit normal. It is further concluded, that since the obliquity is not changed by the motion of the orbit plane, the decay of the obliquity towards zero by tidal friction is not significantly altered by this motion. These results are applied to Mercury, Venus, Iapetus, Triton, as well as the equatorial satellites of Mars, Jupiter, Saturn, and Uranus. The final spin states of these objects satisfy a generalization of Cassini's laws for the moon.
", "date": "1973", "date_type": "degree", "id_number": "CaltechETD:etd-03042009-085737", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03042009-085737", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-03-06", "doi": "10.7907/kqm5-4r97", "alt_title": { "items": [ "The Formation of Planetesimals", "Tidal Friction and Generalized Cassini's Laws in the Solar System" ] }, "divisions": { "items": [ "div_gps" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2009-03-04", "thesis_defense_date": "1972-11-21", "thesis_approved_date": "2009-03-06", "review_status": "approved", "option_major": { "items": [ "plansci" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1973", "author_list": "Ward, William Roger" }, { "id": "/id/eprint/10395", "eprint_id": 10395, "rev_number": 18, "documents": [ { "id": "/id/document/82240", "doc_id": 82240, "rev_number": 2, "files": [ { "id": "/id/file/232311", "fileid": 232311, "datasetid": "document", "objectid": 82240, "filename": "Ni_w-t_1973.pdf", "mime_type": "application/pdf", "hash": "7550054c26e6d0e5240f0492e677ff9f", "hash_type": "MD5", "filesize": 25024101, "mtime": "2017-08-28 23:28:40", "url": "/10395/1/Ni_w-t_1973.pdf" } ], "eprint_id": 10395, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Ni_w-t_1973.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 87, "dir": "disk0/00/01/03/95", "datestamp": "2017-08-29 14:28:40", "lastmod": "2020-03-10 23:39:09", "status_changed": "2017-08-29 14:28:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ni-Wei-Tou", "name": { "family": "Ni", "given": "Wei-Tou" } } ] }, "title": "Metric Theories of Gravity and their Astrophysical Implications", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "The increasing importance of relativistic gravity in astrophysics has led to the need for a detailed analysis of theories of gravity and their viability. Accordingly, in this thesis, metric theories of gravity are compiled, and are classified into four groups: (i) general relativity\r\n(ii) scalar-tensor theories (iii) conformally flat theories and (iv) stratified theories. The post-Newtonian limit of each theory is constructed and its Parametrized Post-Newtonian (PPN) values are obtained. These results, when combined with experimental data and with recent work by Nordtvedt and Will, show that, of all theories thus far examined by our group, the only currently viable ones are (i) general relativity, (ii) the Bergmann-Wagoner scalar-tensor theory and its special cases (Nordtvedt; Brans-Dicke-Jordan, (iii) recent, (as yet unpublished ) vector-tensor theory by Nordtvedt, Hellings,\r\nand Will, and (iv) a new stratified theory by the author, which is presented for the first time in this thesis.
\r\n\r\n\r\nThe PPN formalism is used to analyze stellar stability in any metric theory of gravity. This analysis enables one to infer, for any given gravitation theory, the extent to which post-Newtonian effects induce instabilities in white dwarfs, in neutron stars, and in supermassive stars. It also reveals the extent to which our current empirical knowledge of post-Newtonian gravity (based on solar-system experiments) actually guarantees that relativistic instabilities exist. In particular, it shows that for \"conservative theories of gravity\", current solar-system experiments gua\u00adrantee that relativistic corrections do induce \r\ndynamical instabilities in stars with adiabatic indices slightly greater than 4/3, while for \"non-conservative theories\", current experiments do not permit any firm conclusion.\r\n
", "date": "1973", "date_type": "degree", "id_number": "CaltechTHESIS:08282017-154628547", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:08282017-154628547", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "GP-19887" }, { "agency": "NSF", "grant_number": "GP-27304" }, { "agency": "NSF", "grant_number": "GP-28027" }, { "agency": "NASA", "grant_number": "NAS 7-100" }, { "agency": "NASA", "grant_number": "NGR 05-002-256" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2017-08-29 14:28:40", "doi": "10.7907/MCQM-3M81", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1972-09-11", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1973", "author_list": "Ni, Wei-Tou" }, { "id": "/id/eprint/8966", "eprint_id": 8966, "rev_number": 21, "documents": [ { "id": "/id/document/57666", "doc_id": 57666, "rev_number": 3, "files": [ { "id": "/id/file/163603", "fileid": 163603, "datasetid": "document", "objectid": 57666, "filename": "Dykla_jj_1973.pdf", "mime_type": "application/pdf", "hash": "666837acfbcfc3feef539b599afcef43", "hash_type": "MD5", "filesize": 11797133, "mtime": "2015-06-02 15:36:06", "url": "/8966/1/Dykla_jj_1973.pdf" } ], "eprint_id": 8966, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Dykla_jj_1973.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"2015-06-02 17:24:31", "lastmod": "2022-11-09 19:20:13", "status_changed": "2015-06-02 17:24:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dykla-J-J", "name": { "family": "Dykla", "given": "John Joseph" }, "show_email": "NO" } ] }, "title": "Conserved quantities and the formation of black holes in the Brans-Dicke theory of gravitation", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "In Part I, we construct a symmetric stress-energy-momentum\r\npseudo-tensor for the gravitational fields of Brans-Dicke theory, and use this to establish rigorously conserved integral expressions for energy-momentum Pi and angular momentum Jik. Application of the two-dimensional surface integrals to the exact static spherical vacuum solution of Brans leads to an identification of our conserved mass with the active gravitational mass. Application to the distant fields of an arbitrary stationary source reveals that Pi and Jik have the same physical interpretation as in general relativity. For gravitational waves whose wavelength is small on the scale of the background radius of curvature, averaging over several wavelengths in the Brill-Hartle-Isaacson manner produces a stress-energy-momentum tensor for gravitational radiation which may be used to calculate the changes in Pi and Jik of their source.
\r\n\r\nIn Part II, we develop strong evidence in favor of a conjecture by Penrose--that, in the Brans-Dicke theory, relativistic gravitational collapse in three dimensions produce black holes identical to those of general relativity. After pointing out that any black hole solution of general relativity also satisfies Brans-Dicke theory, we establish the Schwarzschild and Kerr geometries as the only possible spherical and axially symmetric black hole exteriors, respectively. Also, we show that a Schwarzschild geometry is necessarily formed in the collapse of an uncharged sphere.
\r\n\r\nAppendices discuss relationships among relativistic gravity theories and an example of a theory in which black holes do not exist.
\r\n", "date": "1973", "date_type": "degree", "id_number": "CaltechTHESIS:06022015-082916942", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:06022015-082916942", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "GP-27304" }, { "agency": "NSF", "grant_number": "GP-19887" }, { "agency": "NSF", "grant_number": "GP-28027" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_on": "2015-06-02 17:24:31", "doi": "10.7907/h455-hg42", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1972-09-28", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1973", "author_list": "Dykla, John Joseph" }, { "id": "/id/eprint/3184", "eprint_id": 3184, "rev_number": 7, "documents": [ { "id": "/id/document/5648", "doc_id": 5648, "rev_number": 2, "files": [ { "id": "/id/file/33398", "fileid": 33398, "datasetid": "document", "objectid": 5648, "filename": "Oinas_v_1971.pdf", "mime_type": "application/pdf", "filesize": 5248803, "mtime": "2012-12-26 02:57:48", "url": "/3184/1/Oinas_v_1971.pdf" } ], "eprint_id": 3184, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Oinas_v_1971.pdf", "language": "en", "security": "public", "license": "other", "main": "Oinas_v_1971.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22191" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22191" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22191" } ] } }, { "id": "/id/document/22191", "doc_id": 22191, "rev_number": 2, "files": [ { "id": "/id/file/33396", "fileid": 33396, "datasetid": "document", "objectid": 22191, "filename": "preview.png", "mime_type": "image/png", "hash": "b7edaa4168027f64a4717272767ef04c", "hash_type": "MD5", "filesize": 9469, "mtime": "2012-12-26 02:57:48", "url": "/3184/2/preview.png" } ], "eprint_id": 3184, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5648" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5648" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5648" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/84", "datestamp": "2008-09-09", "lastmod": "2019-12-20 19:57:07", "status_changed": "2009-09-25 02:53:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Oinas-V", "name": { "family": "Oinas", "given": "Valdar" }, "show_email": "NO" } ] }, "title": "Analysis of normal and strong - lined K - type dwarf and giant stars", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nIn this work a detailed analysis is carried out for twenty-six normal and super-metal-rich (SMR) K dwarfs and giants in the solar neighborhood. The observational material consists of line measurements on tracings of high dispersion spectra along with photoelectric scans covering a wide range of wavelengths. The program Atlas was employed to construct the model atmospheres; the temperature fit was provided by a matching of the predicted continua to the de-blanketed scans. H[...] wing profiles were also used to obtain information on the temperatures. The major conclusions that were reached are the following:\n\n1) A gravity defect sets in at about spectral type K2 in both dwarfs and giants; its nature is such that progressively lower gravities are required in order to obtain equal ion and neutral abundances as one goes to cooler stars. In the coolest stars the spectroscopic gravities imply masses lower than 0.1M[...]. It is suggested that the effect may be caused by a new opacity source that is acting to steepen the spectral gradient in the visual and near-infrared, thereby falsifying the temperatures. The dependence of the unknown absorber on the temperature and gravity. are discussed and a rough formula describing this dependence is given. It is shown that the new opacity also explains various discrepancies noted by other observers.\n\n2) The SMR stars are generally overabundant by about 0.2 - 0.3 dex relative to the normal-abundance comparison stars of the same temperature. An overabundance of sodium by about 0.5 dex is found for all the SMR stars, with the exception of the dwarf 54 Psc, which is found to have essentially normal metal abundances. [...]UMi, the coolest giant in the program, is also the most super-metal-rich, with a general overabundance of about 0.4 dex and a sodium enhancement of 0.8 dex. The iron overabundance is rather marginal in most of the giants ([...]).\n\n3) No correlation is found between metal abundance and turbulence. In particular, the SMR stars in this program are not found to possess high microturbulent velocities. The U-B deficiencies can be explained by the effects of a slight metal enhancement on the colors (Strom et al. 1971) and the line blocking due to the CN violet system.\n\n4) The SMR dwarfs all lie high on the main sequence, in keeping with their derived metal abundances. It is not necessary to invoke substantial variations in helium content to account for their positions.\n", "date": "1972", "date_type": "degree", "id_number": "CaltechETD:etd-08212008-100608", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08212008-100608", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/HHGN-ZB70", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-21", "thesis_defense_date": "1971-12-16", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Oinas, Valdar" }, { "id": "/id/eprint/3185", "eprint_id": 3185, "rev_number": 7, "documents": [ { "id": "/id/document/5649", "doc_id": 5649, "rev_number": 2, "files": [ { "id": "/id/file/33405", "fileid": 33405, "datasetid": "document", "objectid": 5649, "filename": "Persson_se_1972.pdf", "mime_type": "application/pdf", "filesize": 5952120, "mtime": "2012-12-26 02:57:48", "url": "/3185/1/Persson_se_1972.pdf" } ], "eprint_id": 3185, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Persson_se_1972.pdf", "language": "en", "security": "public", "license": "other", "main": "Persson_se_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22192" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22192" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22192" } ] } }, { "id": "/id/document/22192", "doc_id": 22192, "rev_number": 2, "files": [ { "id": "/id/file/33403", "fileid": 33403, "datasetid": "document", "objectid": 22192, "filename": "preview.png", "mime_type": "image/png", "hash": "b720736235038010fe3a89f102137983", "hash_type": "MD5", "filesize": 10093, "mtime": "2012-12-26 02:57:48", "url": "/3185/2/preview.png" } ], "eprint_id": 3185, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5649" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5649" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5649" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/85", "datestamp": "2008-09-09", "lastmod": "2019-12-20 19:50:49", "status_changed": "2009-09-25 02:53:42", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Persson-S-E", "name": { "family": "Persson", "given": "Sven Eric" }, "show_email": "NO" } ] }, "title": "Interpretation of the neutral helium triplet spectrum in planetary nebulae", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThe theory of the He I triplet spectrum is modified to include the effects of solid particles within the ionized regions of planetary nebulae. New observations of the emission lines [...]5876, 7065, and 10830 are presented for over twenty nebulae, extending the list of objects studied previously by O'Dell. The empirical ratios [...] and [...] are combined with the theory to study the discrepancies between the He I [...] depopulation rates D[...](derived from R[...]), D[...](from R[...]), and D[...] (theoretical). If the presence of dust is neglected, the discrepancies are such that D[...] > D[...] > D[...], in most cases. This is essentially the result found earlier by Capriotti for a smaller sample of objects. Estimates of [...], the [...]10830 dust optical depths which force D[...] = D[...], are derived by accounting for the resonance trapping and dust absorption of the [...]10830 radiation. These estimates are consistent, on an order-of-magnitude basis, with values implied by observed infrared excesses in planetary nebulae, and by simple models of reradiating dust shells.\n\nThe important effects of nebular structural features upon the He I triplet spectrum are studied theoretically and observationally. Overall correlations between the apparent [...] depopulation rate discrepancies and nebular parameters are shown to have a connection with a wide range of nebular problems.\n", "date": "1972", "date_type": "degree", "id_number": "CaltechETD:etd-08212008-101113", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08212008-101113", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/FNVG-6W53", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-21", "thesis_defense_date": "1971-07-28", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Persson, Sven Eric" }, { "id": "/id/eprint/3189", "eprint_id": 3189, "rev_number": 9, "documents": [ { "id": "/id/document/5653", "doc_id": 5653, "rev_number": 2, "files": [ { "id": "/id/file/33434", "fileid": 33434, "datasetid": "document", "objectid": 5653, "filename": "Smithson_rc_1972.pdf", "mime_type": "application/pdf", "filesize": 19568993, "mtime": "2012-12-26 02:57:49", "url": "/3189/1/Smithson_rc_1972.pdf" } ], "eprint_id": 3189, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Smithson_rc_1972.pdf", "language": "en", "security": "public", "license": "other", "main": "Smithson_rc_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22196" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22196" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22196" } ] } }, { "id": "/id/document/22196", "doc_id": 22196, "rev_number": 2, "files": [ { "id": "/id/file/33432", "fileid": 33432, "datasetid": "document", "objectid": 22196, "filename": "preview.png", "mime_type": "image/png", "hash": "43dac6e386236424a55a50dd0f89bce2", "hash_type": "MD5", "filesize": 8267, "mtime": "2012-12-26 02:57:49", "url": "/3189/2/preview.png" } ], "eprint_id": 3189, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5653" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5653" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5653" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/89", "datestamp": "2008-08-29", "lastmod": "2022-02-22 17:57:46", "status_changed": "2009-09-25 02:53:45", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smithson-Robert-Carroll", "name": { "family": "Smithson", "given": "Robert Carroll" }, "show_email": "NO" } ] }, "title": "A Videomagnetograph Study of Diffusion of Solar Magnetic Fields in Weak Plage Regions", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "A new instrument for use in astronomical research has been developed. This is the differential video photometer, a device for detecting differences in light intensity between two television pictures. With a suitable source of video, the device is capable of detecting intensity differences of the order of one part in one thousand. It should be useful in many applications, such as colorimetry, polarimetry, motion detection, and doppler shift measurements. It has been used thus far primarily as a videomagnetograph which measures the line-of-sight component of the solar magnetic field in the photosphere. Sensitivity to magnetic field strength is on the order of 5 to 10 gauss.
\r\n\r\nA study has been made of the characteristics of magnetic flux diffusion in weak plage regions. Points of enhanced magnetic field have been found to exist which have lifetimes of about 3 to 4 days, and which move in a random walk with a step time short compared to 24 hours. The random walk of these points considered as discrete entities is not, however, responsible for much of the flux diffusion in the weak plage regions. The R.M.S. displacement of the points is about 7800 km in 24 hours. A second form of flux transport has been found in which in a period of a few hours, a previously stable point will become unstable, and either shoot out a tongue of flux, or begin to move as a unit. This process can move flux over distances of the order of 10,000 km at apparent velocities of 1 to 2 km/sec. This process may be responsible for most of the flux transport in weak plage regions.
", "date": "1972", "date_type": "degree", "id_number": "CaltechETD:etd-08212008-142413", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08212008-142413", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-08-29", "doi": "10.7907/QGBD-XQ45", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Leighton-R-B", "name": { "family": "Leighton", "given": "Robert B." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-21", "thesis_defense_date": "1972-01-01", "thesis_approved_date": "2008-08-29", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Smithson, Robert Carroll" }, { "id": "/id/eprint/3186", "eprint_id": 3186, "rev_number": 10, "documents": [ { "id": "/id/document/5650", "doc_id": 5650, "rev_number": 2, "files": [ { "id": "/id/file/33413", "fileid": 33413, "datasetid": "document", "objectid": 5650, "filename": "Shostak_gs_1972.pdf", "mime_type": "application/pdf", "filesize": 11773262, "mtime": "2012-12-26 02:57:48", "url": "/3186/1/Shostak_gs_1972.pdf" } ], "eprint_id": 3186, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Shostak_gs_1972.pdf", "language": "en", "security": "public", "license": "other", "main": "Shostak_gs_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22193" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22193" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22193" } ] } }, { "id": "/id/document/22193", "doc_id": 22193, "rev_number": 2, "files": [ { "id": "/id/file/33411", "fileid": 33411, "datasetid": "document", "objectid": 22193, "filename": "preview.png", "mime_type": "image/png", "hash": "f291e8ee032c323bb68abd2e34714a80", "hash_type": "MD5", "filesize": 9506, "mtime": "2012-12-26 02:57:48", "url": "/3186/2/preview.png" } ], "eprint_id": 3186, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5650" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5650" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5650" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/31/86", "datestamp": "2008-09-09", "lastmod": "2019-12-20 20:03:25", "status_changed": "2009-09-25 02:53:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shostak-G-S", "name": { "family": "Shostak", "given": "G. Seth" }, "show_email": "NO" } ] }, "title": "Aperture synthesis observations of neutral hydrogen in three galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nAperture synthesis techniques have been used to study the three galaxies NGC2403 (Scd), NGC4236 (SBdm), and IC10 (Irr) in the 21-cm line of neutral hydrogen and off-line continuum. Spatial resolution was 2 minutes of arc; velocity resolution was 21 km-s[...]. The data yield information on the distribution of the HI, and its associated velocity field.\r\n\r\nHydrogen extent of the objects agrees well with their optical size, and evidences a lumpy structure. HI peaks occur away from the nuclei for NGC2403 and NGC4236, and are suggestive of a ring structure for the former galaxy. The hydrogen distribution of IC10 is similar in appearance to that of the Small Magellanic Cloud. In all objects HI peaks show good positional agreement with major HII regions.\r\n\r\nVelocity fields are derived for all objects, and rotation curves obtained for NGC2403 and NGC4236. These curves evidence differential rotation but do not include Keplerian tails, implying that the mass distributions are considerably extended and the total masses poorly determined. The velocity field of IC10 suggests rotation.\r\n\r\nNon-circular motions of ~10 km-s[...] are seen in NGC2403, and these agree well with the streaming motions predicted by the density-wave theory of spiral structure.\r\n\r\nA comparison of NGC2403 with the late-type spirals M33 and M101 reveals a progressive deepening of the central HI depression with increasing mass. Rotation curves for these three galaxies are similar, and consequently all are expected to have mass-to-light ratios which increase rapidly with radius. All have similar maximum HI surface densities (~10[...] atoms-cm[...]) and observed fractional hydrogen masses (~9%).\r\n", "date": "1972", "date_type": "degree", "id_number": "CaltechETD:etd-08212008-102427", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08212008-102427", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-09", "doi": "10.7907/FRRJ-YB73", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Moffet-A-T", "name": { "family": "Moffet", "given": "Alan Theodore" }, "role": "advisor" }, { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-21", "thesis_defense_date": "1971-12-06", "thesis_approved_date": "2008-09-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Shostak, G. Seth" }, { "id": "/id/eprint/9630", "eprint_id": 9630, "rev_number": 19, "documents": [ { "id": "/id/document/64401", "doc_id": 64401, "rev_number": 2, "files": [ { "id": "/id/file/180238", "fileid": 180238, "datasetid": "document", "objectid": 64401, "filename": "Schutz_bf_1972.pdf", "mime_type": "application/pdf", "hash": "754e0132bf50fea0ee2a3287d2af73e7", "hash_type": "MD5", "filesize": 47327250, "mtime": "2016-03-21 20:28:42", "url": "/9630/1/Schutz_bf_1972.pdf" } ], "eprint_id": 9630, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Schutz_bf_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/64402", "doc_id": 64402, "rev_number": 2, "files": [ { "id": "/id/file/180241", "fileid": 180241, "datasetid": "document", "objectid": 64402, "filename": "lightbox.jpg", 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"files": [ { "id": "/id/file/180246", "fileid": 180246, "datasetid": "document", "objectid": 64407, "filename": "Schutz_bf_1972.zip", "mime_type": "application/x-zip", "hash": "ba025784f92a5870abce692c71e94c6c", "hash_type": "MD5", "filesize": 287070703, "mtime": "2016-03-21 20:29:19", "url": "/9630/7/Schutz_bf_1972.zip" } ], "eprint_id": 9630, "pos": 7, "placement": 7, "mime_type": "application/x-zip", "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Schutz_bf_1972.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/130346", "doc_id": 130346, "rev_number": 1, "files": [ { "id": "/id/file/375783", "fileid": 375783, "datasetid": "document", "objectid": 130346, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "f8ca4946cf899d815716ca64abdf9d1e", "hash_type": "MD5", "filesize": 32289, "mtime": 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"Schutz-Bernard-Frederick", "name": { "family": "Schutz", "given": "Bernard Frederick" } } ] }, "title": "Relativistic velocity - potential hydrodynamics and stellar stability", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "The equations of relativistic, perfect-fluid hydrodynamics are cast in Eulerian form using six scalar \"velocity-potential\" fields, each of which has an equation of evolution. These equations determine the motion of the fluid through the equation
\r\n\r\nU\u028b=\u00b5-1 (\u00f8,\u028b + \u03b1\u03b2,\u028b + \u019fS,\u028b).
\r\n\r\nEinstein's equations and the velocity-potential hydrodynamical equations\r\nfollow from a variational principle whose action is
\r\n\r\nI = (R + 16\u03c0 p) (-g)1/2 d4x,
\r\n\r\nwhere R is the scalar curvature of spacetime and p is the pressure of the fluid. These equations are also cast into Hamiltonian form, with Hamiltonian density \u2013T00 (-goo)-1/2.
\r\n\r\nThe second variation of the action is used as the Lagrangian governing the evolution of small perturbations of differentially rotating stellar models. In Newtonian gravity this leads to linear dynamical stability criteria already known. In general relativity it leads to a new sufficient condition for the stability of such models against arbitrary perturbations.
\r\n\r\nBy introducing three scalar fields defined by
\r\n\r\n\u03c1 \u1d74 = \u2207\u03bb + \u2207x(xi + \u2207x\u0263i)
\r\n\r\n(where \u1d74 is the vector displacement of the perturbed fluid element, \u03c1 is the mass-density, and i, is an arbitrary vector), the Newtonian stability criteria are greatly simplified for the purpose of practical applications. The relativistic stability criterion is not yet in a form that permits practical calculations, but ways to place it in such a form are discussed.
\r\n\r\n", "date": "1972", "date_type": "degree", "id_number": "CaltechTHESIS:03212016-112353716", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:03212016-112353716", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "GP-15911" }, { "agency": "NSF", "grant_number": "GP-9114" }, { "agency": "NSF", "grant_number": "GP-27304" }, { "agency": "NSF", "grant_number": "GP-19887" }, { "agency": "NSF", "grant_number": "GP-28027" }, { "agency": "Office of Naval Research", "grant_number": "Nonr-220(47)" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_on": "2016-03-21 21:59:04", "doi": "10.7907/05NX-9C06", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1971-08-10", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Schutz, Bernard Frederick" }, { "id": "/id/eprint/9912", "eprint_id": 9912, "rev_number": 15, "documents": [ { "id": "/id/document/73975", "doc_id": 73975, "rev_number": 2, "files": [ { "id": "/id/file/208552", "fileid": 208552, "datasetid": "document", "objectid": 73975, "filename": "Strange_dlp_1972.pdf", "mime_type": "application/pdf", "hash": "1d05e3d2f31cc5b5422065e017c1d666", "hash_type": "MD5", "filesize": 14749505, "mtime": "2016-09-06 16:37:17", "url": "/9912/1/Strange_dlp_1972.pdf" } ], "eprint_id": 9912, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Strange_dlp_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"archive", "userid": 10575, "dir": "disk0/00/00/99/12", "datestamp": "2016-09-07 17:49:18", "lastmod": "2020-03-10 19:17:15", "status_changed": "2016-09-07 17:49:18", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Strange-Donald-Lionel-Patrick", "name": { "family": "Strange", "given": "Donald Lionel Patrick" } } ] }, "title": "Radiative processes in an intense magnetic field", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Three astrophysical problems relating to the intense magnetic fields associated with neutron stars (i.e. 1012 gauss) and white dwarfs (i.e. 108 gauss) are studied.
\r\n\r\n(1) The radiation rate for non-relativistic bremsstrahlung in 1012 gauss is computed by both quantum-mechanical and classical methods. The main features of this emissivity are a 1/pz dependence (magnetic field in the z-direction) characteristic of a one-dimensional momentum space, a larger flux perpendicular to \u0496 than parallel to it, and a net left-handed polarization in the flux parallel to \u0496.
\r\n\r\n(2) The electron energy levels and orbits for hydrogen in 1012 gauss are calculated with variational techniques. The ground state binding energy is found to be 200 ev. The other levels divide into a set of tightly bound states (binding energies 100 to 200 ev) and a double-set of hydrogen-like levels (0 to 13 ev). The overall electron density of the atom is elongated along the magnetic field direction. The thermal ionization fraction of a neutral hydrogen plasma is computed using an appropriately modified Saha equation, and is found to be 90%. Finally, high Z atoms are investigated via the Thomas-Fermi approximation with the result that the definitive equation is
\r\n\r\nX11 = X1/2x1/2
\r\n\r\ngiving an atomic radius of
\r\n\r\nR = 4 x 10-5 Z1/5 \u04962/5 cm.
\r\n\r\n(3) Cyclotron emission and absorption in a magnetic field of 108 gauss is studied as a possible mechanism for the observed degree of circular polarization in the optical emission from white dwarfs. A few simple models explain some of the quantitative and qualitative aspects of the polarization data.
\r\n\r\n", "date": "1972", "date_type": "degree", "id_number": "CaltechTHESIS:09062016-085609385", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09062016-085609385", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Woodrow Wilson Fellowship" }, { "agency": "NATO" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_on": "2016-09-07 17:49:18", "doi": "10.7907/TDYS-3Y25", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1972-05-15", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Strange, Donald Lionel Patrick" }, { "id": "/id/eprint/1924", "eprint_id": 1924, "rev_number": 9, "documents": [ { "id": "/id/document/3330", "doc_id": 3330, "rev_number": 2, "files": [ { "id": "/id/file/19808", "fileid": 19808, "datasetid": "document", "objectid": 3330, "filename": "Christensen_cg_1972.pdf", "mime_type": "application/pdf", "filesize": 7476014, "mtime": "2012-12-26 02:44:18", "url": "/1924/1/Christensen_cg_1972.pdf" } ], "eprint_id": 1924, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Christensen_cg_1972.pdf", "language": "en", "security": "public", "license": "other", "main": "Christensen_cg_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20014" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20014" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20014" } ] } }, { "id": "/id/document/20014", "doc_id": 20014, "rev_number": 2, "files": [ { "id": "/id/file/19806", "fileid": 19806, "datasetid": "document", "objectid": 20014, "filename": "preview.png", "mime_type": "image/png", "hash": "42d72b5228b9f80a05a63e34d3d3a4c0", "hash_type": "MD5", "filesize": 11670, "mtime": "2012-12-26 02:44:18", "url": "/1924/2/preview.png" } ], "eprint_id": 1924, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3330" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3330" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3330" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/19/24", "datestamp": "2008-05-22", "lastmod": "2019-12-21 02:56:31", "status_changed": "2009-09-25 02:20:14", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Christensen-C-G", "name": { "family": "Christensen", "given": "Clark G." }, "show_email": "NO" } ] }, "title": "The synthesis of composite spectra : a study of four globular clusters of the galaxy, five globular clusters of M31, and the nucleus of NGC 205", "ispublished": "unpub", "full_text_status": "public", "abstract": "A spectral synthesis technique similar to that of Spinrad and Taylor (1971) has been applied to the integrated light of globular clusters M5, M13, M15, and M92 of the Galaxy; H12, H55, H140, B282, and MIV of M31; and to the nucleus of the elliptical galaxy NGC 205. The derived stellar contents of the four local clusters have been compared with color-magnitude diagrams and luminosity functions based on studies of individual stars within these systems. Results agree.\n\nThe technique yields information on both the metal content of clusters and their horizontal-branch colors and thus is useful for extracting the two parameters which apparently describe galactic globular clusters.\n\nPrincipal results of the study of the six extragalactic systems are:\n(1) The clusters H12 and H140 have similar metal contents and similar luminosity functions except along their horizontal branches where H12 is concentrated to the red, resembling 47 Tuc, and H140 is rather blue, resembling M5. This result suggests that M31 clusters belong to at least a two-parameter family as do clusters in the Galaxy.\n(2) H55 and B282 have absorption features too strong to be artificially reproduced with a mixture of population I stellar spectra of normal feature strengths. This confirms a similar result by Spinrad and Schweizer (1972) for B282.\n(3) The strong-lined cluster H55 is a halo object. This corroborates van den Bergh's (1969) discovery of strong-lined halo clusters in M31.\n(4) The metal-richness of the stellar contents of the clusters correlates well with van den Bergh's line index L. This correlation strengthens his result that M31 globular clusters are generally more metal-rich than their galactic counterparts.\n(5) No firm evidence is found for the hot blue stars inferred to be present in B282 by Spinrad and Schweizer.\n(6) The nucleus of NGC 205 is composed of mild population II stars like clusters H12 and H140. However its color-magnitude distribution is unlike that of any known globular cluster. V-light contributions are about sixty per cent from its main sequence and only three per cent from its giant branch. The domination by dwarfs is greater by a factor of two than in the M81, M32, and M31 nuclear models of Spinrad and Taylor (1971). The apparent explanation is a different luminosity function.\n\nThere is some evidence for dispersion in the initial luminosity functions of clusters. The best models for the metal-rich clusters H55 and B282 have about one-half more V-light arising from their main\nsequences than the other clusters. The giant branch of M5 appears to contribute about one-third more V-light than giant branches of other clusters studied. There is some independent evidence for an abnormally heavily populated giant branch in M5.\n", "date": "1972", "date_type": "degree", "id_number": "CaltechETD:etd-05212008-111500", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05212008-111500", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-22", "doi": "10.7907/VTAK-FR10", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-21", "thesis_defense_date": "1972-01-24", "thesis_approved_date": "2008-05-22", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Christensen, Clark G." }, { "id": "/id/eprint/3769", "eprint_id": 3769, "rev_number": 19, "documents": [ { "id": "/id/document/6407", "doc_id": 6407, "rev_number": 3, "files": [ { "id": "/id/file/38427", "fileid": 38427, "datasetid": "document", "objectid": 6407, "filename": "Adelman_sj_1972.pdf", "mime_type": "application/pdf", "filesize": 9283206, "mtime": "2012-12-26 03:02:51", "url": "/3769/1/Adelman_sj_1972.pdf" } ], "eprint_id": 3769, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Adelman_sj_1972.pdf", "language": "en", "security": "internal", "license": "other", "main": "Adelman_sj_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/107635" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/107635" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/69", "datestamp": "2008-10-07", "lastmod": "2020-05-07 22:16:10", "status_changed": "2009-09-25 03:05:35", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adelman-Saul-Joseph", "name": { "family": "Adelman", "given": "Saul Joseph" }, "show_email": "NO" } ] }, "title": "A Study of Twenty-One Sharp-Lined Non-Variable Cool Peculiar A Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Elemental abundance analyses have been performed for twenty-one cool Ap stars, also known as SrCrEu stars, which are not known to be spectrum variables and whose projected rotational velocity is not greater than 10 km/sec. Zeeman and thermal Doppler broadening are the basic line intensification mechanisms considered. Effective temperatures estimated initially from UBV photoelectric data are modified by requiring that the iron abundances derived from both neutral and singly-ionized lines be equal. Log g has been assumed to be 4.0. In addition, two normal stars have been included in this study for comparison.
\r\n\r\nThe cool Ap stars, in general, have normal or over-abundances with respect to hydrogen for every element studied. The iron abundance is found to increase with effective temperature. Similar dependences are found for chromium, manganese, neodymium, gadolinium, and, perhaps, several other elements. The abundances are not dependent on the apparent rotational velocity or magnetic field strength.
\r\n\r\nThe elemental abundances are similar to those of the SrCrEu spectrum variables and agree reasonably well with the results of other studies of cool Ap stars. Comparisons with Mn and Si stars are similar to but not identical with those of other investigators. Substantial differences in certain abundance ratios are found which distinguish Am and cool Ap stars. The results of low dispersion classification spectroscopy correlate better with the appearance than with the derived abundances. The agreement between photometric indices and abundances is poor. Several stars are found whose properties are similar to those of Si stars studied by Sargent, Searle, and Lungershausen except with regard to their [Cr/Fe] values. Thus, in addition to the fact that both types have magnetic fields, the abundances indicate that the Si and cool Ap stars are probably closely related.
\r\n\r\nThe theories to account for the Ap star elemental abundances have difficulties in explaining the results of this study. The diffusion mechanism and the magnetic accretion hypothesis of Havnes and Conti cannot explain several features, for example, the abundance ratios of certain adjacent elements, and are at best incomplete. On the basis of the latter theory, it is hard to understand why the abundances are not correlated with magnetic field strength. Some features of the abundance anomalies are similar to those produced by the r- and by the s-processes. Theories which require mixing of the Ap star or binary companions are excluded.
", "date": "1972", "date_type": "degree", "id_number": "CaltechETD:etd-09252008-114349", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09252008-114349", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NDEA" }, { "agency": "ARCS Foundation" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-10-07", "doi": "10.7907/ZHSY-9B33", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Preston-G-W", "name": { "family": "Preston", "given": "George W." }, "role": "chair" }, { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "member" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-25", "thesis_defense_date": "1971-12-17", "thesis_approved_date": "2008-10-07", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Adelman, Saul Joseph" }, { "id": "/id/eprint/3218", "eprint_id": 3218, "rev_number": 9, "documents": [ { "id": "/id/document/5709", "doc_id": 5709, "rev_number": 2, "files": [ { "id": "/id/file/33763", "fileid": 33763, "datasetid": "document", "objectid": 5709, "filename": "Yip_kb_1972.pdf", "mime_type": "application/pdf", "filesize": 5776889, "mtime": "2012-12-26 02:58:11", "url": "/3218/1/Yip_kb_1972.pdf" } ], "eprint_id": 3218, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Yip_kb_1972.pdf", "language": "en", "security": "public", "license": "other", "main": "Yip_kb_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22251" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22251" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22251" } ] } }, { "id": "/id/document/22251", "doc_id": 22251, "rev_number": 2, "files": [ { "id": "/id/file/33761", "fileid": 33761, "datasetid": "document", "objectid": 22251, "filename": "preview.png", "mime_type": "image/png", "hash": "279226b79c3276a8bb2437b9b26258fb", "hash_type": "MD5", "filesize": 8032, "mtime": "2012-12-26 02:58:11", "url": "/3218/2/preview.png" } ], "eprint_id": 3218, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5709" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5709" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5709" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/18", "datestamp": "2008-09-08", "lastmod": "2019-12-20 19:48:13", "status_changed": "2009-09-25 02:54:44", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yip-K-B-W", "name": { "family": "Yip", "given": "Ka Bing Winson" }, "show_email": "NO" } ] }, "title": "Synthesis of the polarization properties of Cygnus A at 8300 and 9600 megahertz", "ispublished": "unpub", "full_text_status": "public", "abstract": "Methods of polarized interferometry have been used in conjunction with the earth rotation aperture synthesis technique to study the polarized intensity distributions of Cygnus A at 8300 MHz and 9600 MHz. The total intensity distribution at 8300 MHz has also been obtained.\r\n\r\nAlthough the resolutions obtained in these observations are about 20\", it is still quite insufficient to reveal the structures in the components for a detailed comparison with the theoretical model proposed by Mills and Sturrock. The general featere of the ram pressure confinement mechanism, however, is consistent with this observation.\r\n\r\nThe polarized distributions yield a rather fast variation of large rotation measures across the east component. There is also a reversal of the longitudinal magnetic field in the direction of the west component. Correlations with the distribution of small hydrogen clouds deduced from HI absorption measurements have been discussed.\r\n\r\nThere seems to be little depolarization across this source except in the bridge, and this is believed to be occurring outside of the emitting region. However, no detailed models can be worked out without further information about the conditions of the intervening medium.\r\n", "date": "1972", "date_type": "degree", "id_number": "CaltechETD:etd-08252008-075815", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08252008-075815", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-08", "doi": "10.7907/GVT6-PD26", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Seielstad-G-A", "name": { "family": "Seielstad", "given": "George A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-25", "thesis_defense_date": "1971-06-09", "thesis_approved_date": "2008-09-08", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1972", "author_list": "Yip, Ka Bing Winson" }, { "id": "/id/eprint/3839", "eprint_id": 3839, "rev_number": 11, "documents": [ { "id": "/id/document/6479", "doc_id": 6479, "rev_number": 2, "files": [ { "id": "/id/file/38977", "fileid": 38977, "datasetid": "document", "objectid": 6479, "filename": "Will_cm_1971.pdf", "mime_type": "application/pdf", "filesize": 4202593, "mtime": "2012-12-26 03:03:22", "url": "/3839/1/Will_cm_1971.pdf" } ], "eprint_id": 3839, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Will_cm_1971.pdf", "language": "en", "security": "public", "license": "other", "main": "Will_cm_1971.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23011" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23011" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23011" } ] } }, { "id": "/id/document/23011", "doc_id": 23011, "rev_number": 2, "files": [ { "id": "/id/file/38975", "fileid": 38975, "datasetid": "document", "objectid": 23011, "filename": "preview.png", "mime_type": "image/png", "hash": "688b51da14c922cae82321b050675b95", "hash_type": "MD5", "filesize": 12196, "mtime": "2012-12-26 03:03:22", "url": "/3839/2/preview.png" } ], "eprint_id": 3839, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6479" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6479" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6479" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/38/39", "datestamp": "2005-10-03", "lastmod": "2020-10-09 22:26:40", "status_changed": "2009-09-25 03:06:44", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Will-Clifford-Martin", "name": { "family": "Will", "given": "Clifford Martin" }, "show_email": "NO" } ] }, "title": "Theoretical Frameworks for Testing Relativistic Gravity; The Parametrized Post-Newtonian Formalism", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics ; Relativistic Gravity ; Post-Newtonian Formalism", "note": "Einstein Prize citation: \"For outstanding contributions to observational tests of general relativity with theories of gravitational waves, astrophysical black holes, and neutron stars.\"", "abstract": "Increasing sophistication and precision of experimental tests of relativistic gravitation theories has led to the need for a detailed theoretical framework for analysing and interpreting these experiments. Such a framework is the Parametrized Post-Newtonian (PPN) formalism, which treats the post-Newtonian limit of arbitrary metric theories of gravity in terms of nine metric parameters, whose values vary from theory to theory. The theoretical and experimental foundations of the PPN formalism are laid out and discussed, and the detailed definitions and equations for the formalism are given. It is shown that some metric theories of gravity predict that a massive, self-gravitating body's passive gravitational mass should not be equal to its inertial mass, but should be an anisotropic tensor which depends on the body's self-gravitational energy (violation of the \"principle of equivalence\"). Two theorems are presented which probe the theoretical structure of the PPN formalism. They state that (i) a metric theory of gravity possesses post-Newtonian integral conservation laws if and only if its nine PP parameters have values which satisfy a set of seven constraint equations, and (ii) a metric theory of gravity is invariant under asymptotic Lorentz transformations if and only if its PPN parameters satisfy a set of three constraint equations. Some theories of gravity (including Whitehead's theory and theories which violate one of the \"Lorentz-invariance\" parameter constraints) are shown to predict an anisotropy in the Newtonian gravitational constant. Gravimeter data on the tides of the solid Earth are used to put an upper limit on the magnitude of the predicted anisotropy, and thence to rule out such theories.", "date": "1971", "date_type": "degree", "id_number": "CaltechETD:etd-09302005-113319", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09302005-113319", "related_url": { "items": [ { "description": "Einstein Prize (APS) announcement, 2021", "type": "org", "url": "https://www.aps.org/programs/honors/prizes/prizerecipient.cfm?last_nm=Will&first_nm=Clifford&year=2021" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-10-03", "doi": "10.7907/NQNB-RK02", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-09-30", "thesis_defense_date": "1971-05-14", "thesis_approved_date": "2005-10-03", "thesis_awards": "Einstein Prize (APS), 2021. Albert Einstein Medal, 2019. Fellow of the International Society on General Relativity and Gravitation, 2016. Member of the US National Academy of Sciences, 2007. Fellow of the American Academy of Arts and Sciences, 2002. Fellow of the American Physical Society, 1989.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1971", "author_list": "Will, Clifford Martin" }, { "id": "/id/eprint/1926", "eprint_id": 1926, "rev_number": 14, "documents": [ { "id": "/id/document/3332", "doc_id": 3332, "rev_number": 3, "files": [ { "id": "/id/file/19825", "fileid": 19825, "datasetid": "document", "objectid": 3332, "filename": "Cohen_jg_1971.pdf", "mime_type": "application/pdf", "filesize": 12724133, "mtime": "2012-12-26 02:44:19", "url": "/1926/1/Cohen_jg_1971.pdf" } ], "eprint_id": 1926, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Scanned (no OCR) Cohen_jg_1971.pdf", "language": "en", "security": "internal", "license": "other", "main": "Cohen_jg_1971.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": 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"http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/105948" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/105948" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/19/26", "datestamp": "2008-05-22", "lastmod": "2020-02-03 20:09:41", "status_changed": "2009-09-25 02:20:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cohen-Judith-Gamora", "name": { "family": "Cohen", "given": "Judith Gamora" }, "orcid": "0000-0002-8039-4673", "show_email": "NO" } ] }, "title": "The Lithium Isotope Ratio in F and G Field Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Theoretical profiles of the resonance line of Li I have been computed using an absorption coefficient which is the sum of that for each of the four components and a model stellar atmosphere. These profiles have been used to verify the lithium abundances derived by previous investigators with various approximations. A study of the feasibility of measuring the lithium isotope ratio with high dispersion photographic spectra was made, with negative results.
\r\n\r\nWe obtain profiles of \u03bb6708 \u00c5 of Li I, \u03bb6717 \u00c5 Ca I, and sometimes \u03bb6710.3 \u00c5 of Fe I, and the D lines of Na I for a selected group of F, G, and early K field stars. These profiles were observed with the Fabry-Perot interferometer at the coud\u00e9 focus of the 100\" telescope with a resolution of 0.06-0.09 \u00c5. Extensive checks of the accuracy of the wavelength scale, the instrumental profile, and the parasitic light level are made, including observations of the lunar spectrum. The D line profiles were used to test the accuracy of the computed theoretical profiles. The observed stellar line profiles are fit by calculated ones to determine the lithium abundance, calcium abundance, rotational velocity, radial velocity, microturbulent velocity, and lithium isotope ratio for the program stars. The rotational velocities are all greater than 2 km/sec, and range up to 10 km/sec. The microturbulent velocities in the program stars must be greater than zero. The isotope ratio Li\u2076/Li\u2077, determined by two independent methods, is zero in all the stars, with the possible exception of \u03c7' Ori, for which we obtain Li\u2076/Li\u2077 = 0.1 (\u00b10.1).
", "date": "1971", "date_type": "degree", "id_number": "CaltechETD:etd-05212008-142244", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05212008-142244", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-22", "doi": "10.7907/1R06-FG25", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-21", "thesis_defense_date": "1971-05-27", "thesis_approved_date": "2008-05-22", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1971", "author_list": "Cohen, Judith Gamora" }, { "id": "/id/eprint/3254", "eprint_id": 3254, "rev_number": 15, "documents": [ { "id": "/id/document/5756", "doc_id": 5756, "rev_number": 3, "files": [ { "id": "/id/file/34093", "fileid": 34093, "datasetid": "document", "objectid": 5756, "filename": "Frogel_ja_1971.pdf", "mime_type": "application/pdf", "filesize": 23448051, "mtime": "2012-12-26 02:58:31", "url": "/3254/1/Frogel_ja_1971.pdf" } ], "eprint_id": 3254, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Frogel_ja_1971.pdf", "language": "en", "security": "public", "license": "other", "main": "Frogel_ja_1971.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22297" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22297" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22297" } ] } }, { "id": "/id/document/22297", "doc_id": 22297, "rev_number": 3, "files": [ { "id": "/id/file/34091", "fileid": 34091, "datasetid": "document", "objectid": 22297, "filename": "preview.png", "mime_type": "image/png", "hash": "5afe42411f4c01e5feb52831dad061c4", "hash_type": "MD5", "filesize": 2279, "mtime": "2012-12-26 02:58:30", "url": "/3254/2/preview.png" } ], "eprint_id": 3254, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5756" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5756" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5756" } ] } }, { "id": "/id/document/77623", "doc_id": 77623, "rev_number": 3, "files": [ { "id": "/id/file/220115", "fileid": 220115, "datasetid": "document", "objectid": 77623, "filename": "Frogel thesis Form submission from Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "3f9f8367b84532d9956ee873346bee36", "hash_type": "MD5", "filesize": 1105, "mtime": "2017-04-25 21:36:31", "url": "/3254/3/Frogel thesis Form submission from Thesis Permission Form.txt" } ], "eprint_id": 3254, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "author ok 4/25/2017", "language": "en", "security": "internal", "license": "other", "main": "Frogel thesis Form submission from Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/32/54", "datestamp": "2008-09-10", "lastmod": "2019-12-21 01:47:05", "status_changed": "2009-09-25 02:55:19", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jayfrogel@me.com", "id": "Frogel-Jay-Albert", "name": { "family": "Frogel", "given": "Jay Albert" }, "show_email": "YES" } ] }, "title": "Infrared Spectra of Late-Type Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "astronomy, stars, late-type, infrared, stellar spectra", "abstract": "Spectra have been obtained in the 2\u03bc atmospheric window with a resolution of 32 and 65\u00c5 of late-type dwarfs, giants, supergiants, and long period variables.
\r\n\r\nIn the non-variable stars, the first overtone band of C0 at 2.29\u03bc shows a systematic increase with both increasing luminosity and decreasing temperature. This increasing strength is interpreted as arising from an increase in turbulence and a decrease in atmospheric opacity. The 1.87\u03bc band of H2O appears only in stars of spectral type M6 and later. The observed strength of this band is considerably weaker than that predicted by model atmospheres. Strong bands of C13O16 are visible in most of the stars, and they are interpreted as indicating a number ratio [C12/C13] < 10.
\r\n\r\nVariations in the strengths of the H2O and C0 bands were measured in 18 long period variables as well as variations in the continuum flux at 2.25\u03bc, f(225). There is a phase lag between the visual and f(225) light curves in the sense that the maximum of the latter occurs after that of the former. The size of the lag is directly proportional to the range at 2.25\u03bc. The molecular absorption bands are stronger in the variables than in the non-variables of the same spectral type. The value of [C12/C13] for the variables is comparable to that for the non-variables.
\r\n\r\nThere is evidence for differences in the value of [0/C] among the variable stars. NML Tau seems to have a value similar to that of U Ori, a typical M-type variable. R Aur, T Cas, X Cyg, and RS Lib appear to have abnormally low values of [0/C].
\r\n\r\nA model involving the motion of a shock wave through the star's atmosphere is discussed as a possible means of explaining variations in both visual and infrared spectra.
\r\n\r\nThe evolutionary history of and the effect of convective mixing in late-type stars is discussed and it is concluded that: 1.) the value of [C12/C13] indicates that mixing has occurred; 2.) the degree of mixing may be greater in the non-variables than in the variables; 3.) the observations are not inconsistent with a high value of [0/C] in most of the stars observed, i.e. [0/C] ~2.
\r\n", "date": "1971", "date_type": "degree", "id_number": "CaltechETD:etd-08272008-152127", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-08272008-152127", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-09-10", "doi": "10.7907/F9GE-VF59", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "Gerry" }, "role": "chair" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-08-27", "thesis_defense_date": "1971-01-28", "thesis_approved_date": "2008-09-10", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1971", "author_list": "Frogel, Jay Albert" }, { "id": "/id/eprint/1781", "eprint_id": 1781, "rev_number": 7, "documents": [ { "id": "/id/document/2902", "doc_id": 2902, "rev_number": 2, "files": [ { "id": "/id/file/17652", "fileid": 17652, "datasetid": "document", "objectid": 2902, "filename": "Shipman_hl_1971.pdf", "mime_type": "application/pdf", "filesize": 14539929, "mtime": "2012-12-26 02:41:59", "url": "/1781/1/Shipman_hl_1971.pdf" } ], "eprint_id": 1781, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Shipman_hl_1971.pdf", "language": "en", "security": "public", "license": "other", "main": "Shipman_hl_1971.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19625" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19625" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19625" } ] } }, { "id": "/id/document/19625", "doc_id": 19625, "rev_number": 2, "files": [ { "id": "/id/file/17650", "fileid": 17650, "datasetid": "document", "objectid": 19625, "filename": "preview.png", "mime_type": "image/png", "hash": "ad73b4324c8ef493dbc717eafcdaac43", "hash_type": "MD5", "filesize": 11963, "mtime": "2012-12-26 02:41:59", "url": "/1781/2/preview.png" } ], "eprint_id": 1781, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2902" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2902" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2902" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/81", "datestamp": "2008-05-16", "lastmod": "2019-12-20 19:34:21", "status_changed": "2009-09-25 02:15:13", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Shipman-H-L", "name": { "family": "Shipman", "given": "Henry Longfellow" }, "show_email": "NO" } ] }, "title": "White dwarfs", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThe aim of this thesis is to use model-atmosphere techniques and intermediate-band photoelectric scans to determine the properties of white dwarfs. Model atmospheres have been calculated with [...] for solar composition and [...] for helium-rich (Y=1) models. Photoelectric scans of some 37 white dwarfs are the observational basis of the thesis.\n\nThe essential results for the program stars are that the DA stars have a mean radius of .013 [...]. With one or two exceptions, the program stars are on the upper sequence of the white dwarfs. The median mass is 0.58 [...]. One of the DA,F stars in the program L 870-2, has a radius of .04 [...]. The DA stars cover a wide range of effective temperature; the DB stars, with the exception of HZ 29, have 12,000\u00b0[...]18,000\u00b0K. The DA stars contain very little helium ([...]0.8% by number); and the DB stars contain very little metals. It is possible to interpret the spectrum of the one DC star in the program (L 1363-3) as a cooled-off DB star, since the helium lines fade out at [...].\n\nThe spectrum of Sirius B is analyzed; the hydrogen line profiles, combined with the mass of 1.02[...] (van den Bos 1960) and the visual magnitude of 8.29 (Lindenblad 1970) yield an effective temperature of 32,000\u00b0K and a surface gravity of 8.65, corresponding to a radius of 0.0078 [...]. These values are consistent with the measured gravitational redshift of +88 km/sec.\n\nUsing the program stars, I then define a U-V versus [...] relation for DA stars and for the DB and DC stars. Using this relation, and the [...] as measured by Graham (1969), I compute masses and radii for a much larger sample of white dwarfs than the program stars those with known distances. The median radius of these stars, which include quite a few on the lower sequence is 0.0095 [...]. Using these data, I find that the atmospherically derived masses of white dwarfs are in reasonable agreement with the mass-radius relation for degenerate stars and with the gravitational redshifts measured by Greenstein and Trimble (1967).\n\nThe effective temperatures of all the stars in the lists of Eggen and Greenstein were computed for the purpose of testing the convection-accretion theory of Strittmatter and Wickramasinghe (1971) which purports to account for the formation of DB stars. The results here contradict their prediction that there should be a shortage of DA stars with 15,000\u00b0 [...] 18,000\u00b0K. I propose a modification of their theory which explains the existence of both the DA and the DB stars in the temperature ranges in which they are observed. This modification also explains the DC stars, and suggests a possible explanation for the 4670 stars.\n\nThe wavelength dependence of the circular polarization of Grw+70\u00b08247 for 3000[...] 8000 [...] is explained in the context of radiative transfer theory.\n", "date": "1971", "date_type": "degree", "id_number": "CaltechETD:etd-05132008-145722", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05132008-145722", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-16", "doi": "10.7907/49SJ-WP05", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-13", "thesis_defense_date": "1971-05-17", "thesis_approved_date": "2008-05-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1971", "author_list": "Shipman, Henry Longfellow" }, { "id": "/id/eprint/1758", "eprint_id": 1758, "rev_number": 7, "documents": [ { "id": "/id/document/2858", "doc_id": 2858, "rev_number": 2, "files": [ { "id": "/id/file/17397", "fileid": 17397, "datasetid": "document", "objectid": 2858, "filename": "Weistrop_de_1971.pdf", "mime_type": "application/pdf", "filesize": 4058427, "mtime": "2012-12-26 02:41:43", "url": "/1758/1/Weistrop_de_1971.pdf" } ], "eprint_id": 1758, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Weistrop_de_1971.pdf", "language": "en", "security": "public", "license": "other", "main": "Weistrop_de_1971.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19582" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19582" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19582" } ] } }, { "id": "/id/document/19582", "doc_id": 19582, "rev_number": 2, "files": [ { "id": "/id/file/17395", "fileid": 17395, "datasetid": "document", "objectid": 19582, "filename": "preview.png", "mime_type": "image/png", "hash": "f185babf4e779d07f4e2a8d5388c1f5d", "hash_type": "MD5", "filesize": 8841, "mtime": "2012-12-26 02:41:43", "url": "/1758/2/preview.png" } ], "eprint_id": 1758, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2858" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2858" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2858" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/58", "datestamp": "2008-05-16", "lastmod": "2019-12-21 04:39:04", "status_changed": "2009-09-25 02:14:45", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Weistrop-D-E", "name": { "family": "Weistrop", "given": "Donna Etta" }, "show_email": "NO" } ] }, "title": "Characteristics of disk and halo populations derived from photographic photometry", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThe nature of faint stars at high galactic latitudes was investigated through U,B,V photometry of several thousand stars between V = 12 and 18 near the North Galactic Pole. Magnitudes were determined from iris photometer measurements of plates taken with the 48-inch Schmidt telescope. Calibration was provided by a photoelectric sequence in the field. Several models for the luminosity function and density distribution of Population II field stars were assumed. Assuming also that all stars bluer than (B-V)[...] = .5 and fainter than V = 17 are members of Population II, an upper limit of 7 x 10[...] solar masses per pc[...] was calculated for the local Population II density, a result significantly lower than local densities computed from the number of nearby stars suspected of halo membership. Some of the discrepancy may be due to the method used.\n\nHaving estimated the contributions to the star counts due to Population II stars and disk giants and subgiants, the remaining stars were assumed to constitute a pure disk dwarf population. Density distributions for stars in successive (B-V)[...] intervals were calculated and combined to form a composite disk density distribution. The agreement with Oort's K giant distribution is satisfactory. There was some indication that the faintest dwarfs are concentrated in a narrow layer in the plane, but further investigation is required. Determination of the luminosity function for the reddest disk dwarfs indicated these stars are five to ten times as numerous as was previously thought, thus accounting for a significant fraction of the missing mass in the solar neighborhood. Luminosity functions extrapolated to account for all the missing mass are indicated.\n", "date": "1971", "date_type": "degree", "id_number": "CaltechETD:etd-05122008-131358", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05122008-131358", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-16", "doi": "10.7907/YAZV-KE91", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-12", "thesis_defense_date": "1971-05-25", "thesis_approved_date": "2008-05-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1971", "author_list": "Weistrop, Donna Etta" }, { "id": "/id/eprint/5526", "eprint_id": 5526, "rev_number": 17, "documents": [ { "id": "/id/document/9275", "doc_id": 9275, "rev_number": 4, "files": [ { "id": "/id/file/58512", "fileid": 58512, "datasetid": "document", "objectid": 9275, "filename": "Price_rh_1971.pdf", "mime_type": "application/pdf", "filesize": 3054289, "mtime": "2012-12-26 03:21:15", "url": "/5526/1/Price_rh_1971.pdf" } ], "eprint_id": 5526, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Price_rh_1971.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/25351" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/25351" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/25351" } ] } }, { "id": "/id/document/15577", "doc_id": 15577, "rev_number": 3, "files": [ { "id": "/id/file/205085", "fileid": 205085, "datasetid": "document", "objectid": 15577, "filename": "Price_rh_1971.zip", "mime_type": "application/zip", "filesize": 6370636, "mtime": "2016-08-22 21:18:37", "url": "/5526/2/Price_rh_1971.zip" } ], "eprint_id": 5526, "pos": 2, "format": "application/zip", "language": "en", "security": "internal", "license": "other", "main": "Price_rh_1971.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "archival" }, { "id": "/id/document/25351", "doc_id": 25351, "rev_number": 2, "files": [ { "id": "/id/file/58510", "fileid": 58510, "datasetid": "document", "objectid": 25351, "filename": "preview.png", "mime_type": "image/png", "hash": "1ef279f4e5cceb8722b1fedf06275843", "hash_type": "MD5", "filesize": 8310, "mtime": "2012-12-26 03:21:15", "url": "/5526/3/preview.png" } ], "eprint_id": 5526, "pos": 3, "placement": 3, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/9275" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/9275" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/9275" } ] } } ], "eprint_status": "archive", "userid": 51, "dir": "disk0/00/00/55/26", "datestamp": "2010-01-19 17:27:26", "lastmod": "2020-03-10 23:39:07", "status_changed": "2010-01-19 17:27:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Price-R-H", "name": { "family": "Price", "given": "Richard H." } } ] }, "title": "Nonspherical perturbations of relativistic gravitational collapse", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "It is known that there can be no gravitational, electromagnetic, or scalar field perturbations (except angular momentum) of a Schwarzschild black hole. A gravitationally collapsing star with nonspherical perturbations must therefore radiate away its perturbations or halt its collapse. The results of computations in comoving coordinates are presented to show that the scalar field in a collapsing star neither disappears nor halts the collapse, as the star passes inside its gravitational radius.\r\n\r\nOn the star's surface, near the event horizon, the scalar field varies as a_1 + a_2 exp (-t/2M) due to time dilation. The dynamics of the field outside the star can be analyzed with a simple wave equation containing a spacetime-curvature induced potential. This potential is impenetrable to zero-frequency waves and thus a_1, the final value of the field on the stellar surface, is not manifested in the exterior; the field vanishes. The monopole perturbation falls off as t^(-2); higher \u2113-poles fall off as \u2113n t/t^(2\u2113+3).\r\n\r\nThe analysis of scalar-field perturbations works as well for electromagnetic and gravitational perturbations and also for zero-restmass perturbation fields of arbitrary integer spin. All these perturbation fields obey wave equations with curvature potentials that differ little from one field to another. For all fields, radiatable multipoles (\u2113 \u2265 spin of the field) fall off as \u2113nt/t^(2\u2113+3).\r\n", "date": "1971", "date_type": "degree", "id_number": "CaltechTHESIS:01192010-090920179", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:01192010-090920179", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "GP-27304" } ] }, "collection": "CaltechTHESIS", "reviewer": "Gayle Hammer", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Tony Diaz", "deposited_on": "2010-01-19 17:27:26", "doi": "10.7907/1EGC-Y160", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1971-04-15", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "Author's Rights Authorization: I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted here is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive license to archive and make accessible, under the conditions specified under \"Thesis Availability\" in this submission, my thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation, or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1971", "author_list": "Price, Richard H." }, { "id": "/id/eprint/1665", "eprint_id": 1665, "rev_number": 7, "documents": [ { "id": "/id/document/2643", "doc_id": 2643, "rev_number": 2, "files": [ { "id": "/id/file/16223", "fileid": 16223, "datasetid": "document", "objectid": 2643, "filename": "Keeley_da_1970.pdf", "mime_type": "application/pdf", "filesize": 4725152, "mtime": "2012-12-26 02:40:31", "url": "/1665/1/Keeley_da_1970.pdf" } ], "eprint_id": 1665, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Keeley_da_1970.pdf", "language": "en", "security": "public", "license": "other", "main": "Keeley_da_1970.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19382" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19382" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19382" } ] } }, { "id": "/id/document/19382", "doc_id": 19382, "rev_number": 2, "files": [ { "id": "/id/file/16221", "fileid": 16221, "datasetid": "document", "objectid": 19382, "filename": "preview.png", "mime_type": "image/png", "hash": "4c0265adb5ec09842531623ddb4a4523", "hash_type": "MD5", "filesize": 9349, "mtime": "2012-12-26 02:40:31", "url": "/1665/2/preview.png" } ], "eprint_id": 1665, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2643" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2643" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2643" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/16/65", "datestamp": "2008-05-09", "lastmod": "2019-12-21 04:06:21", "status_changed": "2009-09-25 02:11:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Keeley-D-A", "name": { "family": "Keeley", "given": "Douglas Allan" }, "show_email": "NO" } ] }, "title": "Static and dynamical models of long-period variable stars", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThe parameters of the models were M=1 and 1.3M[...], M[subscript B] = -3.8 to -5, and T[subscript e] = 2200[...]K. The equation of state included a detailed calculation of ionization equilibrium and the dissociation of H2, OH, CO, and H2O. The opacity of CO, OH, and H2O was included. The dynamical calculations show that large-amplitude pulsation can occur in convective models. The opacity mechanism causes strong driving of the pulsation in the region outside the hydrogen ionization zone, and the [gamma]-mechanism results in very low dissipation in the hydrogen zone. The phase relation between the bolo-metric luminosity and the radius variations is similar to that of Cepheids. The static models have large ionization and dissociation zones, which cause the pulsation parameter Q=P[subscript days](p/p[...])[...] to become greater than 0.15 in some models. The fundamental periods range from 180 days to greater than 2000 days; the overtone periods are about [...] as long. The positions of many observed stars in the theoretical HR diagram suggest that their periods should be associated with the overtone periods of the models.\n", "date": "1970", "date_type": "degree", "id_number": "CaltechETD:etd-05072008-142808", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05072008-142808", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-09", "doi": "10.7907/NTN2-HH47", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Goldreich-P-M", "name": { "family": "Goldreich", "given": "Peter Martin" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-07", "thesis_defense_date": "1969-09-10", "thesis_approved_date": "2008-05-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1970", "author_list": "Keeley, Douglas Allan" }, { "id": "/id/eprint/2643", "eprint_id": 2643, "rev_number": 7, "documents": [ { "id": "/id/document/4938", "doc_id": 4938, "rev_number": 2, "files": [ { "id": "/id/file/28646", "fileid": 28646, "datasetid": "document", "objectid": 4938, "filename": "Osmer_ps_1970.pdf", "mime_type": "application/pdf", "filesize": 4393856, "mtime": "2012-12-26 02:53:18", "url": "/2643/1/Osmer_ps_1970.pdf" } ], "eprint_id": 2643, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Osmer_ps_1970.pdf", "language": "en", "security": "public", "license": "other", "main": "Osmer_ps_1970.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21488" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21488" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21488" } ] } }, { "id": "/id/document/21488", "doc_id": 21488, "rev_number": 2, "files": [ { "id": "/id/file/28644", "fileid": 28644, "datasetid": "document", "objectid": 21488, "filename": "preview.png", "mime_type": "image/png", "hash": "fe88d915d08012385218e5d3860543fd", "hash_type": "MD5", "filesize": 6992, "mtime": "2012-12-26 02:53:18", "url": "/2643/2/preview.png" } ], "eprint_id": 2643, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4938" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4938" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4938" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/26/43", "datestamp": "2008-06-24", "lastmod": "2019-12-21 04:58:01", "status_changed": "2009-09-25 02:42:13", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Osmer-P-S", "name": { "family": "Osmer", "given": "Patrick Stewart" }, "show_email": "NO" } ] }, "title": "The atmospheres of the F supergiants", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nCoude spectra of 26 supergiants of spectral types F2-G5 were obtained, and spectrophotometric observations of four which occurred in clusters were made. A photoelectric system for measuring the 0 I 7774 line was established, and the line strength was determined in 59 A0-G3 stars of luminosity classes Ia-V, By calibrating the line strength in 10 F supergiants of known luminosity we find that it indicates the absolute magnitude of F stars brighter than [...] = -4 with an accuracy of [...]. The curves of growth obtained from the spectra show that the microturbulence determined from the Fe II lines increases with luminosity and is correlated with the oxygen line strength. However, the Fe I microturbulence exhibits a different behavior near spectral type F5, where it is insensitive to luminosity.\n\nThe applicability of model atmospheres to the F supergiants was checked by using the spectrophotometric observations. The derived temperatures were reasonable, but the gravities of the Ia stars were a factor of 5 less than expected from stellar interiors calculations. The difference was less for the Ib stars. It was shown that pulsational effects did not account for the discrepancy. Consideration of how the turbulent motions could affect the pressure equilibrium in the atmosphere indicated that the observed velocities were large enough to reduce the gas pressure and cause the observed low gravities. The models also indicated that a decrease in the continuous absorption combined with the observed microturbulence accounted for the increase in the oxygen line strength with luminosity. Although non-LTE effects may be present in the oxygen line, they do not change significantly with luminosity and do not contribute to the observed increase in strength.\n\nThe gradient in radiation pressure beneath the photosphere in F stars with log g <2 is large enough to cause an inversion in the gas pressure. The zone where this occurs is unstable and could be the cause of mass motions in supergiants. This hypothesis is supported by the fact that the zone appears at the gravity where the oxygen lines become sensitive to luminosity and the turbulence begins to increase. Simple calculations show how the existence of the zone depends on gravity and temperature.\n\nFinally, we demonstrated that a turbulent velocity which increases with height in the atmosphere explains the difference in the behavior of the Fe I and II lines at F5 as well as their similarities at other spectral types. At F5Ib the lines are formed at the same depth, but in the F5Ia stars the increased ionization causes the Fe II lines to be formed at greater heights in the atmosphere than the Fe I lines.\n", "date": "1970", "date_type": "degree", "id_number": "CaltechETD:etd-06182008-131615", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06182008-131615", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-06-24", "doi": "10.7907/8N4Y-K187", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-06-18", "thesis_defense_date": "1969-10-02", "thesis_approved_date": "2008-06-24", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1970", "author_list": "Osmer, Patrick Stewart" }, { "id": "/id/eprint/1925", "eprint_id": 1925, "rev_number": 8, "documents": [ { "id": "/id/document/3331", "doc_id": 3331, "rev_number": 2, "files": [ { "id": "/id/file/19816", "fileid": 19816, "datasetid": "document", "objectid": 3331, "filename": "Michaud_gj_1970.pdf", "mime_type": "application/pdf", "filesize": 28179342, "mtime": "2012-12-26 02:44:18", "url": "/1925/1/Michaud_gj_1970.pdf" } ], "eprint_id": 1925, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Michaud_gj_1970.pdf", "language": "en", "security": "public", "license": "other", "main": "Michaud_gj_1970.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/20015" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20015" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20015" } ] } }, { "id": "/id/document/20015", "doc_id": 20015, "rev_number": 2, "files": [ { "id": "/id/file/19814", "fileid": 19814, "datasetid": "document", "objectid": 20015, "filename": "preview.png", "mime_type": "image/png", "hash": "eb9948d7a16ca8874f3314f854d44f3e", "hash_type": "MD5", "filesize": 9323, "mtime": "2012-12-26 02:44:18", "url": "/1925/2/preview.png" } ], "eprint_id": 1925, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/3331" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/3331" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/3331" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/19/25", "datestamp": "2008-05-22", "lastmod": "2019-12-21 02:51:56", "status_changed": "2009-09-25 02:20:14", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Michaud-G", "name": { "family": "Michaud", "given": "Georges" }, "show_email": "NO" } ] }, "title": "I. Diffusion processes in A-PEC stars. II. Nucleosynthesis in Si burning", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nTwo problems related to elemental abundances have been studied: the abundance anomalies in A-pec stars and the nucleosynthesis of elements between [...] and [...].\n\nDiffusion processes were found to lead to most of the peculiar abundances observed in A-pec stars. If it is assumed that the atmos phere is stable enough for diffusion processes to be important, gravitational settling leads to the underabundances of He Ne and 0 in the stars where they are observed (that is with the [...] log g they are observed to have). Radiation pressure leads to the overabundances of Mn, Sr, Y, Zr and the rare earths in the stars where they are observed. Si would be expected to be overabundant onlyif it has wide auto-ionization features. The overabundance of P is not explained.\n\nThe magnetic fields observed in A-pec stars could bring to the atmosphere the stability needed for diffusion processes to be important. They would also guide diffusion into patches leading to the periodic variation of the observed overabundances.\n\nWe have also studied the conditions necessary to generate through nuclear reactions, the abundances observed between [...] and [...]. It was found that most of the observed abundances could have been generated in a single process, Si burning.\n\nA mixture of [...] at t = O, in proportions leading to the observed abundance of [...] and [...] was found to [...] \t lead to the generation of most elements between Si and Co if one added up the zone where no Si had burned, where little had burned ... and where all had burned.\n\nThe summation over the zones was seen to depend on essentially two parameters which most conveniently can be expressed as the lower and upper limits of integration. One then has essentially four parameters: [...], and the two limits of integration. The density was found to have no effect on our results. The temperature is more important but the range of freezing temperatures to be expected can be estimated accurately enough from the dynamic time scale. With four free parameters, one than fits the abundances of some 25 to 30 of the 41 nuclei between [...] and [...]. Some of the poorly fitted nuclei are very neutron rich nuclei [...] which could easily have been formed by a slight exposure of the material to a neutron flux.", "date": "1970", "date_type": "degree", "id_number": "CaltechETD:etd-05212008-112244", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05212008-112244", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-22", "doi": "10.7907/ZR0T-W227", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Fowler-W-A", "name": { "family": "Fowler", "given": "William A." }, "role": "advisor" }, { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-21", "thesis_defense_date": "1969-09-16", "thesis_approved_date": "2008-05-22", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1970", "author_list": "Michaud, Georges" }, { "id": "/id/eprint/1710", "eprint_id": 1710, "rev_number": 7, "documents": [ { "id": "/id/document/2727", "doc_id": 2727, "rev_number": 2, "files": [ { "id": "/id/file/16720", "fileid": 16720, "datasetid": "document", "objectid": 2727, "filename": "Peterson_av_1970.pdf", "mime_type": "application/pdf", "filesize": 5008745, "mtime": "2012-12-26 02:40:59", "url": "/1710/1/Peterson_av_1970.pdf" } ], "eprint_id": 1710, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Peterson_av_1970.pdf", "language": "en", "security": "public", "license": "other", "main": "Peterson_av_1970.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19460" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19460" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19460" } ] } }, { "id": "/id/document/19460", "doc_id": 19460, "rev_number": 2, "files": [ { "id": "/id/file/16718", "fileid": 16718, "datasetid": "document", "objectid": 19460, "filename": "preview.png", "mime_type": "image/png", "hash": "7cfdd89e01533009cb7c94e3c650a11f", "hash_type": "MD5", "filesize": 8856, "mtime": "2012-12-26 02:40:59", "url": "/1710/2/preview.png" } ], "eprint_id": 1710, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2727" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2727" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2727" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/10", "datestamp": "2008-05-16", "lastmod": "2019-12-21 03:58:57", "status_changed": "2009-09-25 02:12:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Peterson-A-V", "name": { "family": "Peterson", "given": "Arsine Victoria" }, "show_email": "NO" } ] }, "title": "A spectroscopic investigation of four O-type subdwarfs", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nThe spectra of four O-type subdwarfs, of the class with strong nitrogen lines and very weak carbon and oxygen lines, have been studied in some detail. Model atmospheres have been constructed for the stars HZ 44, +25\u00b04655, and HD 127493, and the computed profiles of selected hydrogen and helium lines have been compared with the observed profiles. The effective temperatures of the model atmospheres are [...] 40 000 \u00b0K and the surface gravities are g [...] 5 x [...] (cgs). A mass of approximately [...] and an absolute visual magnitude of about +4 for the stars HZ 44 and HD 127493 is found to be consistent with the available data. The star +25\u00b04655 is probably less luminous.\n\nHigh helium abundances have been inferred for these stars -- from Y [...] 0.4 for HZ 44 to Y [...] 0.9 for +25\u00b04655. Chemical abundances have been derived for heavier elements in a fine analysis. The nitrogen to carbon, and nitrogen to oxygen ratios derived for these stars are two orders of magnitude greater than is observed in the sun and in other main sequence stars. The high helium abundance and the observed CNO ratios are consistent with abundances predicted for material which has undergone hydrogen-burning in the CNO cycle.\n", "date": "1970", "date_type": "degree", "id_number": "CaltechETD:etd-05092008-145009", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05092008-145009", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-16", "doi": "10.7907/9AF4-BY55", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-09", "thesis_defense_date": "1969-09-24", "thesis_approved_date": "2008-05-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1970", "author_list": "Peterson, Arsine Victoria" }, { "id": "/id/eprint/1709", "eprint_id": 1709, "rev_number": 9, "documents": [ { "id": "/id/document/2726", "doc_id": 2726, "rev_number": 2, "files": [ { "id": "/id/file/16713", "fileid": 16713, "datasetid": "document", "objectid": 2726, "filename": "Sramek_ra_1970.pdf", "mime_type": "application/pdf", "filesize": 5632468, "mtime": "2012-12-26 02:40:59", "url": "/1709/1/Sramek_ra_1970.pdf" } ], "eprint_id": 1709, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Sramek_ra_1970.pdf", "language": "en", "security": "public", "license": "other", "main": "Sramek_ra_1970.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19459" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19459" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19459" } ] } }, { "id": "/id/document/19459", "doc_id": 19459, "rev_number": 2, "files": [ { "id": "/id/file/16711", "fileid": 16711, "datasetid": "document", "objectid": 19459, "filename": "preview.png", "mime_type": "image/png", "hash": "343fa3abbbc1288baacc95d030445062", "hash_type": "MD5", "filesize": 7641, "mtime": "2012-12-26 02:40:59", "url": "/1709/2/preview.png" } ], "eprint_id": 1709, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2726" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2726" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2726" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/09", "datestamp": "2008-05-16", "lastmod": "2019-12-21 01:43:12", "status_changed": "2009-09-25 02:12:35", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sramek-R-A", "name": { "family": "Sramek", "given": "Richard Anthony" }, "show_email": "NO" } ] }, "title": "The brightness distribution of core-halo radio sources", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe east-west visibility of 28 extragalactic radio sources with both large and very small components was obtained at 605 MHz using the radio interferometer at the Owens Valley Radio Observatory. A 2' HPBW fan beam was synthesized from observations made at twelve spacings between 62 and 977 wavelengths. The availability of such low spatial frequencies permitted the calculation of the brightness distribution of components as large as 56'. The brightness distributions of the following galaxies are plotted: (spiral galaxies) P0045-25, P1302-49 P1334-29, (elliptical galaxies) 3C40, 3C105, P0843-33, 3C236, 3C247, 3C264, P1216-10, 3C274, 3C287.1, 3C293, and P2247+11.\r\n\r\nFourteen of the observed sources had a core-halo or asymmetric double structure and had their large components well resolved at the 977[...] spacing. The spectral indices of the large and small components of these sources were obtained by comparing the flux densities given here with those at other frequencies. The spectra of the large components are generally steeper than those of the small components with an average difference of spectral indices of [...] = +0.3.\r\n\r\nAssuming equipartition of magnetic and particle energies the total energies of the large halos are ~ [...] ergs. This is sufficient energy to maintain the current radio luminosities for ~ [...] years.\r\n\r\nThree of these fourteen sources have a core-halo structure and are associated with spiral galaxies; the remaining eleven are associated with elliptical galaxies. Two of the remaining sources are asymmetric doubles, and nine have a core-halo structure. Four of the core-halo sources have simple halos, two have double halos, and three have an undetermined halo structure. The ratio of observed double to simple halos can be explained by the projection of double halos randomly oriented in three dimensions provided the ratio of component separation to diameter, R, is less than two. Since doubles without a core have R between two and four, the mechanism of radio galaxy formation is likely to produce a core for low values of R. From the present investigation it is impossible to conclude whether there exists a class of core-halo radio galaxies with simple halos (R [...] 1) or whether the observed core-halo objects represent the low-R end of the ensemble of double radio sources.\r\n", "date": "1970", "date_type": "degree", "id_number": "CaltechETD:etd-05092008-133654", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05092008-133654", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-16", "doi": "10.7907/3HJ1-PE18", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Moffet-A-T", "name": { "family": "Moffet", "given": "Alan Theodore" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-09", "thesis_defense_date": "1970-05-04", "thesis_approved_date": "2008-05-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1970", "author_list": "Sramek, Richard Anthony" }, { "id": "/id/eprint/1568", "eprint_id": 1568, "rev_number": 7, "documents": [ { "id": "/id/document/2419", "doc_id": 2419, "rev_number": 2, "files": [ { "id": "/id/file/14984", "fileid": 14984, "datasetid": "document", "objectid": 2419, "filename": "Webber_jc_1970.pdf", "mime_type": "application/pdf", "filesize": 2013283, "mtime": "2012-12-26 02:39:16", "url": "/1568/1/Webber_jc_1970.pdf" } ], "eprint_id": 1568, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Webber_jc_1970.pdf", "language": "en", "security": "public", "license": "other", "main": "Webber_jc_1970.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19159" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19159" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19159" } ] } }, { "id": "/id/document/19159", "doc_id": 19159, "rev_number": 2, "files": [ { "id": "/id/file/14982", "fileid": 14982, "datasetid": "document", "objectid": 19159, "filename": "preview.png", "mime_type": "image/png", "hash": "bf2a3b3a3426bc83aa6092b4ac2ef63f", "hash_type": "MD5", "filesize": 8610, "mtime": "2012-12-26 02:39:16", "url": "/1568/2/preview.png" } ], "eprint_id": 1568, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2419" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2419" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2419" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/68", "datestamp": "2008-05-16", "lastmod": "2019-12-20 19:31:51", "status_changed": "2009-09-25 02:07:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Webber-J-C", "name": { "family": "Webber", "given": "John Clinton" }, "show_email": "NO" } ] }, "title": "The molecular spectrum of sunspots", "ispublished": "unpub", "full_text_status": "public", "abstract": "The sunspot spectrum shows many molecular lines, of which some have been identified. These lines are formed farther out in the sunspot atmosphere than the atomic lines or the continuum, and are thus useful for probing the outer layers. Photographic spectrograms were obtained for three different sunspots under carefully selected seeing conditions, showing molecular absorption lines due to MgH, CaH, and TiO. Analysis led to estimates of the effective rotational temperatures of each; in the case of CaH, no definite conclusions could be drawn. Predicted rotational temperatures and observational f-values were calculated on the basis of model umbral atmospheres due to several authors. A new model was derived from the molecular lines measured here, and shown to differ widely from previous models. The usefulness of photographic spectra for this purpose is seriously questioned, and suggestions are made for new observations.\n", "date": "1970", "date_type": "degree", "id_number": "CaltechETD:etd-05012008-151521", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05012008-151521", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-16", "doi": "10.7907/FKJP-0C31", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-01", "thesis_defense_date": "1969-09-02", "thesis_approved_date": "2008-05-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1970", "author_list": "Webber, John Clinton" }, { "id": "/id/eprint/1567", "eprint_id": 1567, "rev_number": 12, "documents": [ { "id": "/id/document/2418", "doc_id": 2418, "rev_number": 2, "files": [ { "id": "/id/file/14977", "fileid": 14977, "datasetid": "document", "objectid": 2418, "filename": "O'Connell_rw_1970.pdf", "mime_type": "application/pdf", "filesize": 6279197, "mtime": "2012-12-26 02:39:15", "url": "/1567/1/O'Connell_rw_1970.pdf" } ], "eprint_id": 1567, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "O'Connell_rw_1970.pdf", "language": "en", "security": "public", "license": "other", "main": "O'Connell_rw_1970.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19158" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19158" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19158" } ] } }, { "id": "/id/document/19158", "doc_id": 19158, "rev_number": 2, "files": [ { "id": "/id/file/14975", "fileid": 14975, "datasetid": "document", "objectid": 19158, "filename": "preview.png", "mime_type": "image/png", "hash": "756108758d0b335bf6e739db5e240cf4", "hash_type": "MD5", "filesize": 8296, "mtime": "2012-12-26 02:39:15", "url": "/1567/2/preview.png" } ], "eprint_id": 1567, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2418" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2418" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2418" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/67", "datestamp": "2008-05-13", "lastmod": "2021-07-23 19:30:17", "status_changed": "2009-09-25 02:07:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "O'Connell-Robert-West", "name": { "family": "O'Connell", "given": "Robert West" }, "show_email": "NO" } ] }, "title": "The Stellar Content of M82", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "The stellar contents of two regions on the peculiar galaxy M82 are investigated by spectral synthesis. One of the regions is identified as the nucleus of the galaxy on the basis of its surface brightness and inferred mass density; the other is spectrally representative of the disk of M82. Narrow-band spectrophotometry for both regions can be satisfactorily interpreted in terms of ordinary kinds of stars and dust prevalent in the solar neighborhood if 10\u00b3 M\u2299 of dust is mixed with the stars in the nucleus. There is no evidence for stellar abundance anomalies or the presence of significant amounts of non-stellar radiation except for gaseous emission between 3400 and 11000 \u00c5. Approximately 50% of the observed Na I \u03bb5892 absorption feature originates in the interstellar medium of M82. The deduced main sequence luminosity functions for both regions resemble that for the galactic disk in the solar vicinity except that an excess of massive stars (Mv < -3) exists in the nucleus and a deficiency, in the disk. Sufficient numbers of hot stars are present in the nucleus to maintain the observed level of nuclear interstellar ionization. The absence of massive stars in the disk is corroborated by photographic and spectroscopic evidence and may be the result of a suppression of star formation by a nuclear disturbance. The mass density inferred from the synthesis for the small disk region observed is much higher than found in typical late-type galaxies.
\r\n\r\nThe results of extensive absorption feature index photometry of common galactic stars are also described.
", "date": "1970", "date_type": "degree", "id_number": "CaltechETD:etd-05012008-105635", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05012008-105635", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-13", "doi": "10.7907/AEZK-3E15", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-01", "thesis_defense_date": "1970-05-13", "thesis_approved_date": "2008-05-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1970", "author_list": "O'Connell, Robert West" }, { "id": "/id/eprint/1566", "eprint_id": 1566, "rev_number": 8, "documents": [ { "id": "/id/document/2417", "doc_id": 2417, "rev_number": 2, "files": [ { "id": "/id/file/14968", "fileid": 14968, "datasetid": "document", "objectid": 2417, "filename": "Defouw_rj_1970.pdf", "mime_type": "application/pdf", "filesize": 3662222, "mtime": "2012-12-26 02:39:15", "url": "/1566/1/Defouw_rj_1970.pdf" } ], "eprint_id": 1566, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Defouw_rj_1970.pdf", "language": "en", "security": "public", "license": "other", "main": "Defouw_rj_1970.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19157" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19157" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19157" } ] } }, { "id": "/id/document/19157", "doc_id": 19157, "rev_number": 2, "files": [ { "id": "/id/file/14966", "fileid": 14966, "datasetid": "document", "objectid": 19157, "filename": "preview.png", "mime_type": "image/png", "hash": "538619a4b85e7b360e1f3ccebc2ec837", "hash_type": "MD5", "filesize": 10889, "mtime": "2012-12-26 02:39:15", "url": "/1566/2/preview.png" } ], "eprint_id": 1566, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2417" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2417" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2417" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/66", "datestamp": "2008-05-13", "lastmod": "2019-12-21 04:40:46", "status_changed": "2009-09-25 02:07:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Defouw-Richard-John", "name": { "family": "Defouw", "given": "Richard John" }, "show_email": "NO" } ] }, "title": "Thermal instability and the convective stability of stellar chromospheres", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "It is generally believed that stellar chromospheres are stable against convection since the Schwarzschild criterion indicates stability when temperature increases with height. It is shown, however, that the Schwarzschild criterion does not apply to chromospheres because it ignores the possibility of thermal instability. In the absence of a magnetic field, thermally unstable regions of a chromosphere will be overstable if the temperature inversion is sufficiently steep. This overstability may explain the origin of a certain class of oscillations in the solar chromosphere. Thermally unstable regions containing magnetic fields are monotonically unstable for all values of the temperature gradient. It is suggested that this monotonic instability of magnetic regions is responsible for spicule formation in the solar chromosphere. Elementary considerations of thermal balance predict that the temperature gradient should diverge at levels of marginal stability. The chromospheric region of spicule formation should therefore be bounded below by an abrupt temperature jump.
\r\n\r\nThe above results are derived by analyzing the stability of a simple model chromosphere in which all neutral hydrogen atoms are assumed to be in the ground state. Although the model chromosphere emits only free-bound radiation, its thermal instability is caused by the same ionization effects which lead to instability in plasmas emitting line radiation. Thermally unstable regions of a stellar chromosphere, although not represented in detail by the model, should behave in a similar fashion.
\r\n", "date": "1970", "date_type": "degree", "id_number": "CaltechETD:etd-05012008-103453", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05012008-103453", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-13", "doi": "10.7907/QDN8-FH95", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Sargent-W-L-W", "name": { "family": "Sargent", "given": "Wallace L. W." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-01", "thesis_defense_date": "1970-01-19", "thesis_approved_date": "2008-05-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1970", "author_list": "Defouw, Richard John" }, { "id": "/id/eprint/1564", "eprint_id": 1564, "rev_number": 7, "documents": [ { "id": "/id/document/2415", "doc_id": 2415, "rev_number": 2, "files": [ { "id": "/id/file/14954", "fileid": 14954, "datasetid": "document", "objectid": 2415, "filename": "Peterson_ba_1969.pdf", "mime_type": "application/pdf", "filesize": 2248314, "mtime": "2012-12-26 02:39:14", "url": "/1564/1/Peterson_ba_1969.pdf" } ], "eprint_id": 1564, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Peterson_ba_1969.pdf", "language": "en", "security": "public", "license": "other", "main": "Peterson_ba_1969.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19155" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19155" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19155" } ] } }, { "id": "/id/document/19155", "doc_id": 19155, "rev_number": 2, "files": [ { "id": "/id/file/14952", "fileid": 14952, "datasetid": "document", "objectid": 19155, "filename": "preview.png", "mime_type": "image/png", "hash": "d670d38c1c2d76ab13416c8563f90639", "hash_type": "MD5", "filesize": 9082, "mtime": "2012-12-26 02:39:14", "url": "/1564/2/preview.png" } ], "eprint_id": 1564, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2415" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2415" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2415" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/64", "datestamp": "2008-05-13", "lastmod": "2019-12-21 04:53:07", "status_changed": "2009-09-25 02:07:47", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Peterson-B-A", "name": { "family": "Peterson", "given": "Bruce Alrick" }, "show_email": "NO" } ] }, "title": "A study of absorption and reddening using absolute magnitudes and colors of galaxies", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nFor the brightest galaxy in each of 48 nearby clusters and 7 groups of galaxies, photoelectric measurements of V and V-r magnitudes have been made. Redshifts have been measured for those 39 clusters and 3 groups which did not have previously published redshifts. Absolute magnitudes and colors were calculated for each cluster, and the cscb dependence of the absolute magnitudes and colors was attributed to galactic absorption.\n\nAfter correcting for selection effects, the ratio of total to selective absorption was found to be [...]=3.9 which is consistent with [...]=3.0. The values found for the color-excess and absorption at the galactic pole are [...]=0.016 and [...]=0.06. This value for the color-excess is in agreement with [...]=0.03 found by Sturch for the RR Lyrae stars.\n", "date": "1969", "date_type": "degree", "id_number": "CaltechETD:etd-05012008-091134", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05012008-091134", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-13", "doi": "10.7907/7WK7-V137", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-01", "thesis_defense_date": "1968-10-21", "thesis_approved_date": "2008-05-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1969", "author_list": "Peterson, Bruce Alrick" }, { "id": "/id/eprint/4107", "eprint_id": 4107, "rev_number": 9, "documents": [ { "id": "/id/document/6788", "doc_id": 6788, "rev_number": 2, "files": [ { "id": "/id/file/41158", "fileid": 41158, "datasetid": "document", "objectid": 6788, "filename": "Jacobs_kc_1969.pdf", "mime_type": "application/pdf", "filesize": 11164591, "mtime": "2012-12-26 03:05:28", "url": "/4107/1/Jacobs_kc_1969.pdf" } ], "eprint_id": 4107, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Jacobs_kc_1969.pdf", "language": "en", "security": "public", "license": "other", "main": "Jacobs_kc_1969.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23320" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23320" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23320" } ] } }, { "id": "/id/document/23320", "doc_id": 23320, "rev_number": 2, "files": [ { "id": "/id/file/41156", "fileid": 41156, "datasetid": "document", "objectid": 23320, "filename": "preview.png", "mime_type": "image/png", "hash": "38c3d5dbfef4eef1510104c65afebd58", "hash_type": "MD5", "filesize": 7907, "mtime": "2012-12-26 03:05:28", "url": "/4107/2/preview.png" } ], "eprint_id": 4107, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6788" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6788" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6788" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/41/07", "datestamp": "2002-10-16", "lastmod": "2020-03-10 23:39:06", "status_changed": "2009-09-25 03:11:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jacobs-K-C", "name": { "family": "Jacobs", "given": "Kenneth Charles" }, "show_email": "NO" } ] }, "title": "Bianchi type I cosmological models", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThis thesis begins with a brief review of observations of cosmological interest and with a sketch of the \"standard\" spatially homogeneous and isotropic cosmological models of our Universe that are currently in vogue. Following this introduction we investigate in great detail anisotropic cosmologies and cosmological models of Bianchi Type I. Our primary goal is to understand the consequences of expansion anisotropies in the general relativistic, hot big-bang theory of cosmology.\r\n\r\nWe use the Einstein field equations with vanishing cosmological constant, and Maxwell's equations, to study the temporal evolution of anisotropic Bianchi Type I cosmologies. These cosmologies are spatially homogeneous, but anisotropic; and they have no rotation. We consider only cosmologies with the \"flat\", diagonal, Bianchi Type I metric ds[superscript 2] - dt[superscript2] - A[superscript 2](t)dx[superscript 2] - B[superscript 2](t)dy[superscript 2] - C[superscript 2](t)dz[superscript 2].\r\n\r\nWe begin by studying the general properties of Bianchi Type I cosmologies. Then we consider the stress-energy tensor for massless-particle gases (either degenerate or non-degenerate) which decouple from thermal equilibrium and become freely-propagating in our diagonal Bianchi Type I metric. We investigate the dynamical effects of anisotropic neutrino stresses, and we show how neutrino viscosity damps out most of the existing expansion anisotropies when neutrinos decouple.\r\n\r\nFinally, we elucidate the structure and properties of the Einstein field equations for anisotropic Bianchi Type I cosmologies by deriving a large number of analytical and numerical solutions to these equations. Our stress-energy tensor consists, in general, of perfect-fluid matter with the barotropic equation of state p[subscript m] = [gamma] [rho][subscript m] (0 [<=] [gamma] [<=] 1), and a uniform comoving magnetic field, with energy-density [rho][subscript b], aligned along the z-axis. We first consider the PERFECT-FLUID case where [rho][subscript b] = 0. We find the general analytical solution (for all [gamma]), and construct semi-realistic cosmological models of our Universe using this solution. Then we consider the PERFECT-FLUID-MAGNETIC case where [rho][subscript b] [is not equal to] 0. We derive several analytical solutions, find the behavior near the initial physical singularity for the remaining cases, and study those remaining cases by numerical integration of the field equations. We then consider semi-realistic PERFECT-FLUID-MAGNETIC cosmological models of our Universe.\r\n\r\nIn our semi-realistic cosmological models we study the possible effects of expansion anisotropies and of a uniform primordial magnetic field upon the following: (a) the type of initial physical singularity, (b) the thermal history and temporal evolution of our Universe, (c) primordial element formation, (d) the time when expansion anisotropies become small, and (e) the temperature isotropy of the observed 2.7[degrees]K cosmic microwave radiation.\r\n", "date": "1969", "date_type": "degree", "id_number": "CaltechETD:etd-10162002-080822", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10162002-080822", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-10-16", "doi": "10.7907/KSSQ-R708", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-10-16", "thesis_defense_date": "1968-10-01", "thesis_approved_date": "2002-10-16", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1969", "author_list": "Jacobs, Kenneth Charles" }, { "id": "/id/eprint/4096", "eprint_id": 4096, "rev_number": 9, "documents": [ { "id": "/id/document/6772", "doc_id": 6772, "rev_number": 2, "files": [ { "id": "/id/file/41052", "fileid": 41052, "datasetid": "document", "objectid": 6772, "filename": "Ipser_jr_1969.pdf", "mime_type": "application/pdf", "filesize": 9780542, "mtime": "2012-12-26 03:05:22", "url": "/4096/1/Ipser_jr_1969.pdf" } ], "eprint_id": 4096, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Ipser_jr_1969.pdf", "language": "en", "security": "public", "license": "other", "main": "Ipser_jr_1969.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23304" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23304" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23304" } ] } }, { "id": "/id/document/23304", "doc_id": 23304, "rev_number": 2, "files": [ { "id": "/id/file/41050", "fileid": 41050, "datasetid": "document", "objectid": 23304, "filename": "preview.png", "mime_type": "image/png", "hash": "dd61d1c347fe4104e54c8ef9c7fbe76e", "hash_type": "MD5", "filesize": 11251, "mtime": "2012-12-26 03:05:22", "url": "/4096/2/preview.png" } ], "eprint_id": 4096, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6772" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6772" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6772" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/40/96", "datestamp": "2002-10-16", "lastmod": "2020-03-10 23:39:06", "status_changed": "2009-09-25 03:11:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ipser-J-R", "name": { "family": "Ipser", "given": "James Reid" }, "show_email": "NO" } ] }, "title": "The stability of relativistic, spherically symmetric star clusters", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nIt has been suggested that very dense star clusters might play important roles in quasi-stellar sources and in the nuclei of certain galaxies, where violent events occur. Such star clusters should become unstable against relativistic gravitational collapse when, in the course of evolution, they contract down to a certain critical density. In this thesis the study of the relativistic instability which triggers such collapse is initiated: The theory of the stability of a spherically symmetric star cluster against small radial perturbations is developed within the framework of general relativity. Collisions between stars in the cluster are neglected, since in realistic situations the time scale for collisions should be much greater than the time scale for the growth of the relativistic instability. The equation of motion governing the small radial perturbations of a spherical cluster is derived and is shown to be self-conjugate. Associated with the equation of motion is a dynamically conserved quantity, and a multidimensional variational principle for the normal modes of radial pulsation. The variational principle provides a necessary and sufficient criterion for the stability of the cluster. Also derived are much simpler, one-dimensional, sufficient (but not necessary) criteria for stability. The most important sufficient criterion is this: A relativistic, spherical cluster is stable against radial perturbations if the gas sphere with the same distributions of density and pressure is stable against radial perturbations with adiabatic index [Gamma][subscript 1] = ([rho] + p)p[subscript -1](dp/dr) (d[rho]/dr)[superscript -1].\r\n\r\nThe stability criteria are used to diagnose numerically the stability of (i) clusters of identical stars with heavily-truncated Maxwell-Boltzmann velocity distributions, and (ii) clusters whose densities and isotropic pressures obey polytropic laws of index 2 or 3. The calculations show that a cluster of either type is unstable against collapse if the redshift of a photon emitted from its center and received at infinity is z[subscript c][...] 0.5. The cluster is stable if z[subscript c][...]0.5.\r\n\r\nFor purposes of motivation, two new theorems on the theory of the stability of highly relativistic stars (not star clusters!) are also presented in this thesis. The first theorem states that a highly relativistic, spherical star is stable if and only if its adiabatic index (assumed to be constant in the interior regions) is greater than a certain critical value, [gamma][subscript crit], which depends in a specified way on the high-density equation of state. Because of relativistic effects this critical value is somewhat larger than the Newtonian value [gamma][subscript crit] = 4/3. The second theorem shows that, at high central densities, the curves of - (binding energy) versus radius for certain hot, isentropic sequences of stellar models must exhibit damped clockwise spirals. This spiraling reflects the onset of instability in one radial mode of pulsation after another as the central density increases along the sequence.\r\n\r\n", "date": "1969", "date_type": "degree", "id_number": "CaltechETD:etd-10152002-160828", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10152002-160828", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-10-16", "doi": "10.7907/GF6C-JN05", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-10-15", "thesis_defense_date": "1969-04-21", "thesis_approved_date": "2002-10-16", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1969", "author_list": "Ipser, James Reid" }, { "id": "/id/eprint/4091", "eprint_id": 4091, "rev_number": 10, "documents": [ { "id": "/id/document/6767", "doc_id": 6767, "rev_number": 2, "files": [ { "id": "/id/file/41016", "fileid": 41016, "datasetid": "document", "objectid": 6767, "filename": "Burke_w_1969.pdf", "mime_type": "application/pdf", "filesize": 4247810, "mtime": "2012-12-26 03:05:19", "url": "/4091/1/Burke_w_1969.pdf" } ], "eprint_id": 4091, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Burke_w_1969.pdf", "language": "en", "security": "public", "license": "other", "main": "Burke_w_1969.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23299" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23299" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23299" } ] } }, { "id": "/id/document/23299", "doc_id": 23299, "rev_number": 2, "files": [ { "id": "/id/file/41014", "fileid": 41014, "datasetid": "document", "objectid": 23299, "filename": "preview.png", "mime_type": "image/png", "hash": "b9596595e0f674bafa159a946025ab75", "hash_type": "MD5", "filesize": 8423, "mtime": "2012-12-26 03:05:19", "url": "/4091/2/preview.png" } ], "eprint_id": 4091, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6767" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6767" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6767" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/40/91", "datestamp": "2002-10-16", "lastmod": "2020-03-10 23:39:06", "status_changed": "2009-09-25 03:11:19", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Burke-W-L", "name": { "family": "Burke", "given": "William Lionel" }, "show_email": "NO" } ] }, "title": "The coupling of gravitational radiation to nonrelativistic sources", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThis thesis examines the problem of the coupling of gravitational radiation to its sources in the limit of weak fields and slowly-moving sources; it shows in detail how the irreversibility caused by the escape of radiation can be included in the formalism.\r\n\r\nThe usual slow-motion expansions of General Relativity (EIH and post-Newtonian) have the difficulty that they are not uniformly valid for large distances - distances where radiation becomes important and where the outgoing wave-boundary condition must be imposed. This difficulty is eliminated by using the method of matched asymptotic expansions. A second asymptotic expansion, in the same slowness parameter as enters in the near zone, is used to represent the radiation. This outer expansion provides matching conditions on the inner expansion that generate radiative corrections to the inner expansion.\r\n\r\nUsing this technique we show that the escape of radiation leads to an extraction of energy from the sources, without ever having to define the energy carried in the gravitational waves. The damping is found by calculating the work done by the fields that react back on the source. Explicit expressions are given for these fields, and these can be used to calculate, in lowest order, all the irreversible effects caused by radiation.\r\n\r\nIn this thesis the problem of calculating radiation reaction for bodies with very weak gravitational fields (U/c[superscript 2] << v[superscript 2]/c[superscript 2] << 1) is solved definitely. The case of gravitationally bound systems (U/c[superscript 2] [...] v[superscript 2/c[superscript 2] << 1) is discussed and a program for dealing with this case is set up, but the calculations for this case have not yet been done.", "date": "1969", "date_type": "degree", "id_number": "CaltechETD:etd-10152002-090530", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10152002-090530", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "TAPIR", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-10-16", "doi": "10.7907/89HA-6J10", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-10-15", "thesis_defense_date": "1969-05-22", "thesis_approved_date": "2002-10-16", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1969", "author_list": "Burke, William Lionel" }, { "id": "/id/eprint/1582", "eprint_id": 1582, "rev_number": 9, "documents": [ { "id": "/id/document/2447", "doc_id": 2447, "rev_number": 2, "files": [ { "id": "/id/file/15145", "fileid": 15145, "datasetid": "document", "objectid": 2447, "filename": "Anderson_ksj_1969.pdf", "mime_type": "application/pdf", "filesize": 8377324, "mtime": "2012-12-26 02:39:25", "url": "/1582/1/Anderson_ksj_1969.pdf" } ], "eprint_id": 1582, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Anderson_ksj_1969.pdf", "language": "en", "security": "public", "license": "other", "main": "Anderson_ksj_1969.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19187" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19187" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19187" } ] } }, { "id": "/id/document/19187", "doc_id": 19187, "rev_number": 2, "files": [ { "id": "/id/file/15143", "fileid": 15143, "datasetid": "document", "objectid": 19187, "filename": "preview.png", "mime_type": "image/png", "hash": "fa0d9044e6d37b125b4aa50d53798046", "hash_type": "MD5", "filesize": 8772, "mtime": "2012-12-26 02:39:24", "url": "/1582/2/preview.png" } ], "eprint_id": 1582, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2447" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2447" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2447" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/82", "datestamp": "2008-05-16", "lastmod": "2019-12-20 19:30:14", "status_changed": "2009-09-25 02:08:18", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Anderson-Kurt-Steven-Jarl", "name": { "family": "Anderson", "given": "Kurt Steven Jarl" }, "show_email": "NO" } ] }, "title": "A Spectrophotometric Study of Seyfert Nuclei", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Photoelectric and photographic spectrophotometry have been utilized to infer some of the properties of the nuclear regions of eight Seyfert galaxies and two additional objects displaying somewhat more normal spectra. The observations were principally made during 1966 and 1967 and cover much of the region between 3300\u00c5 and 10,000\u00c5. For each of the objects, absolute continuous energy distributions are obtained. In addition, the relative and absolute emission-line intensities and profiles were derived from the observational data. It is found that the emission-line profiles, and the profiles of the Balmer line cores can be consistently interpreted in terms of mass-motions and/or turbulence within the emitting regions. The wings of the Balmer lines are difficult to interpret in this fashion and evidence is presented which indicates that the relevant broadening mechanism is electron scattering. This process requires that the emission nuclei possess significant optical depth in the Balmer lines. The anomalously steep Balmer decrements which are observed, as well as the presence of the Balmer wings, may also be consistent with such optical depth. Absorption lines seem to be extremely weak, or absent, in the nuclear spectra and the continuous energy distributions bear little resemblance to those of normal nuclei. The presence of a relatively flat non-thermal component to the observed spectrum is indicated. Approximate forms for these non-thermal spectra are derived from the observational data and auxiliary calculations. It is found that this non-thermal flux constitutes a large part of the blue and ultraviolet fluxes observed in the Seyfert nuclei. It is this component which is responsible for the unusually blue colors of these objects and for the weakness of the absorption lines. This non-thermal component may also be responsible for the observed wide ranges of ionization. Rough calculations indicate that sufficient ionizing flux will result from an extrapolation of the optical non-thermal spectrum to the far ultraviolet.
\r\n\r\nIt is concluded that the Seyfert nuclei are objects characterized by large internal velocity dispersions, a sizeable non-thermal component, and significant optical thickness in the Balmer lines. The levels of ionization are quite mixed in the line-emitting regions and the source of this ionization is either synchrotron photons or the conversion of the kinetic energy of cloud motions into ionization energy by means of cloud interactions. Of the two, the former seems the more likely. Finally, the sources of the excitation are considered, but no clear distinction between the various mechanisms is possible on the basis of the available data.
\r\n", "date": "1969", "date_type": "degree", "id_number": "CaltechETD:etd-05022008-085808", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05022008-085808", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-16", "doi": "10.7907/H52P-ZH29", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-02", "thesis_defense_date": "1968-10-08", "thesis_approved_date": "2008-05-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1969", "author_list": "Anderson, Kurt Steven Jarl" }, { "id": "/id/eprint/3673", "eprint_id": 3673, "rev_number": 11, "documents": [ { "id": "/id/document/6275", "doc_id": 6275, "rev_number": 2, "files": [ { "id": "/id/file/37602", "fileid": 37602, "datasetid": "document", "objectid": 6275, "filename": "Griffel_dh_1968.pdf", "mime_type": "application/pdf", "filesize": 3759571, "mtime": "2012-12-26 03:01:58", "url": "/3673/1/Griffel_dh_1968.pdf" } ], "eprint_id": 3673, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Griffel_dh_1968.pdf", "language": "en", "security": "public", "license": "other", "main": "Griffel_dh_1968.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22813" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22813" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22813" } ] } }, { "id": "/id/document/22813", "doc_id": 22813, "rev_number": 2, "files": [ { "id": "/id/file/37600", "fileid": 37600, "datasetid": "document", "objectid": 22813, "filename": "preview.png", "mime_type": "image/png", "hash": "2f58635e9f8408c9070944bedc53fa17", "hash_type": "MD5", "filesize": 8518, "mtime": "2012-12-26 03:01:58", "url": "/3673/2/preview.png" } ], "eprint_id": 3673, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6275" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6275" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6275" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/36/73", "datestamp": "2008-11-06", "lastmod": "2021-06-16 23:32:37", "status_changed": "2009-09-25 03:03:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Griffel-David-Henry", "name": { "family": "Griffel", "given": "David Henry" }, "show_email": "NO" } ] }, "title": "The Kinetic Theory of the Solar Wind and its Interaction with the Moon", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\n\r\nBeyond about .1 A.U. from the sun, fluid mechanics is not a good approximation for the solar wind, because the collision frequency is low. Analysis of the particle dynamics shows that if there are no collisions beyond .1 A.U., then at the earth T[...]/T[...] = 35; this is much greater than is observed. We study the effects of interactions by means of the Boltzmann equation. Solving it with Krook's collision term, we find that the temperature anisotropy observed by the Vela satellite requires each particle to make an average of 2 or 3 collisions between .1 and 1 A.U. The temperature averaged over direction roughly follows an adiabatic law, with \u03b3 = 3/2; \u03b3 tends to increase with distance. The theory predicts an excess of high-velocity particles, as is observed by Vela, even when the collision frequency is independent of velocity; but to produce an effect as strong as that observed requires a fairly strong velocity-dependence of the collision frequency.
\r\n\r\nWe proceed to study the interaction of the wind with the moon, treated as a solid body, with neither magnetic field nor atmosphere, absorbing and neutralizing all incident particles. We construct an exact theory of the boundary layer between such a body and a plasma with a magnetic field parallel to the surface, valid when the plasma has no velocity towards the surface. The thickness of the layer is about two gyroradii, and the magnetic field rises across it according to the equation of pressure balance.
\r\n\r\nWe then consider two-dimensional models of the complete wind-planet interaction, and show that in any steady two-dimensional flow, the plasma velocity must be tangential to the body. Then, using the model of the sheath constructed above, we show that there can be no steady flow at all around a finitely conducting cylinder.
\r\n\r\nFinally, we consider the magnetic fields induced by the interplanetary field inside the moon, taking account of its rotation. If the applied field is uniform, then in the steady state there is a constant axial field inside the sphere; near the surface there is a complex toroidal field, dying away to zero in the interior if the sphere is spinning rapidly. If the external field is non-uniform, there is a residual toroidal field throughout the sphere. If the diffusion time is longer than the time between reversals of the inter-planetary field, then the moon will contain concentric shells of toroidal and axial fields, independently diffusing inwards.
\r\n", "date": "1968", "date_type": "degree", "id_number": "CaltechETD:etd-09202008-111601", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09202008-111601", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-06", "doi": "10.7907/DH61-ZQ91", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Davis-Leverett", "name": { "family": "Davis", "given": "Leverett" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-20", "thesis_defense_date": "1967-12-18", "thesis_approved_date": "2008-11-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1968", "author_list": "Griffel, David Henry" }, { "id": "/id/eprint/3723", "eprint_id": 3723, "rev_number": 9, "documents": [ { "id": "/id/document/6339", "doc_id": 6339, "rev_number": 2, "files": [ { "id": "/id/file/38026", "fileid": 38026, "datasetid": "document", "objectid": 6339, "filename": "Anderson_cm_1968.pdf", "mime_type": "application/pdf", "filesize": 5870988, "mtime": "2012-12-26 03:02:26", "url": "/3723/1/Anderson_cm_1968.pdf" } ], "eprint_id": 3723, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Anderson_cm_1968.pdf", "language": "en", "security": "public", "license": "other", "main": "Anderson_cm_1968.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22877" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22877" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22877" } ] } }, { "id": "/id/document/22877", "doc_id": 22877, "rev_number": 2, "files": [ { "id": "/id/file/38024", "fileid": 38024, "datasetid": "document", "objectid": 22877, "filename": "preview.png", "mime_type": "image/png", "hash": "24a5ffd872b57b8b6029fe2ab987b3ea", "hash_type": "MD5", "filesize": 10378, "mtime": "2012-12-26 03:02:26", "url": "/3723/2/preview.png" } ], "eprint_id": 3723, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6339" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6339" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6339" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/23", "datestamp": "2005-09-23", "lastmod": "2024-03-25 21:12:20", "status_changed": "2009-09-25 03:04:13", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Anderson-Christopher-Marlowe", "name": { "family": "Anderson", "given": "Christopher Marlowe" }, "show_email": "NO" } ] }, "title": "The Interstellar Extinction of Stars in H II Regions", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nSpectrophotometric observations of several stars which appear to be associated with H II regions have been obtained in an attempt to locate other occurences of the reddening anomaly which is seen in the Trapezium stars [...] in the Orion Nebula. Several cases of the Orion-like anomaly have been found. The radiation pressure mechanism for the removal of the smallest grains from the nebula has been discussed and has been found to be inoperative because of the drag forces acting upon the grains. It has been shown that the temperature of the grains depends upon the grain size such that the smaller grains might experience more rapid evaporation. The processes of grain-grain fusion and condensation nucleus exhaustion have been investigated as possible causes of the anomalous grain size distribution. Finally, the anomaly has been discussed as if it were a peculiarity in the intrinsic colors of the stars. The large infrared excess observed in these stars could be due to the presence of late-type stellar companions or circumstellar shells.\r\n", "date": "1968", "date_type": "degree", "id_number": "CaltechETD:etd-09232005-080803", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232005-080803", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-09-23", "doi": "10.7907/DH4K-AB89", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-09-23", "thesis_defense_date": "1968-01-19", "thesis_approved_date": "2005-09-23", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1968", "author_list": "Anderson, Christopher Marlowe" }, { "id": "/id/eprint/1555", "eprint_id": 1555, "rev_number": 7, "documents": [ { "id": "/id/document/2406", "doc_id": 2406, "rev_number": 2, "files": [ { "id": "/id/file/14891", "fileid": 14891, "datasetid": "document", "objectid": 2406, "filename": "Larson_rb_1968.pdf", "mime_type": "application/pdf", "filesize": 8459284, "mtime": "2012-12-26 02:39:12", "url": "/1555/1/Larson_rb_1968.pdf" } ], "eprint_id": 1555, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Larson_rb_1968.pdf", "language": "en", "security": "public", "license": "other", "main": "Larson_rb_1968.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19146" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19146" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19146" } ] } }, { "id": "/id/document/19146", "doc_id": 19146, "rev_number": 2, "files": [ { "id": "/id/file/14889", "fileid": 14889, "datasetid": "document", "objectid": 19146, "filename": "preview.png", "mime_type": "image/png", "hash": "315167eae010365e5f8936f71f460202", "hash_type": "MD5", "filesize": 7266, "mtime": "2012-12-26 02:39:11", "url": "/1555/2/preview.png" } ], "eprint_id": 1555, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2406" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2406" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2406" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/55", "datestamp": "2008-05-13", "lastmod": "2019-12-20 19:30:59", "status_changed": "2009-09-25 02:07:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Larson-R-B", "name": { "family": "Larson", "given": "Richard Bondo" }, "show_email": "NO" } ] }, "title": "Dynamics of a collapsing protostar", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nNumerical calculations of the dynamics of a spherically symmetric collapsing protostar have been made for various assumed initial conditions. In all cases the collapse is found to be extremely nonhomologous, the density distribution becoming more and more sharply peaked at the center as the collapse proceeds. As a result, a very small part of the cloud's mass at the center reaches stellar densities and temperatures and stops collapsing before most of the cloud has had time to collapse very far. The central stellar core thus formed subsequently grows in mass as the surrounding material falls into it, finally becoming an ordinary star when all of the original protostellar material has been accreted. During most of this time the forming star is completely obscured by the dust in the infalling cloud, the absorbed radiation reappearing in the infrared as thermal emission from the dust grains. For M = [...] the resulting star is almost a conventional Hayashi pre-main sequence model, but it appears quite low on the Hayashi track, at about [...]. For masses greater than about 2 or [\u2026] the convective Hayashi phase does not exist at all. The emitted spectrum of a protostar has been calculated from a simple approximation for the radiative transfer problem in the infalling cloud, and the results have been compared with some observations which may be relevant. It appears that some observations of infrared objects and some properties of T Tauri stars may be explainable from our results.\n", "date": "1968", "date_type": "degree", "id_number": "CaltechETD:etd-04302008-143923", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04302008-143923", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-13", "doi": "10.7907/B8XQ-F688", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-04-30", "thesis_defense_date": "1968-03-18", "thesis_approved_date": "2008-05-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1968", "author_list": "Larson, Richard Bondo" }, { "id": "/id/eprint/1583", "eprint_id": 1583, "rev_number": 7, "documents": [ { "id": "/id/document/2448", "doc_id": 2448, "rev_number": 2, "files": [ { "id": "/id/file/15152", "fileid": 15152, "datasetid": "document", "objectid": 2448, "filename": "Scargle_jd_1968.pdf", "mime_type": "application/pdf", "filesize": 19959527, "mtime": "2012-12-26 02:39:25", "url": "/1583/1/Scargle_jd_1968.pdf" } ], "eprint_id": 1583, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Scargle_jd_1968.pdf", "language": "en", "security": "public", "license": "other", "main": "Scargle_jd_1968.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19188" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19188" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19188" } ] } }, { "id": "/id/document/19188", "doc_id": 19188, "rev_number": 2, "files": [ { "id": "/id/file/15150", "fileid": 15150, "datasetid": "document", "objectid": 19188, "filename": "preview.png", "mime_type": "image/png", "hash": "8c7048db1eb6eaa0637d9097efd129e2", "hash_type": "MD5", "filesize": 9600, "mtime": "2012-12-26 02:39:25", "url": "/1583/2/preview.png" } ], "eprint_id": 1583, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2448" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2448" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2448" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/83", "datestamp": "2008-05-16", "lastmod": "2019-12-20 19:32:50", "status_changed": "2009-09-25 02:08:19", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scargle-J-D", "name": { "family": "Scargle", "given": "Jeffrey D." }, "show_email": "NO" } ] }, "title": "Activity in the Crab Nebula", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\n\nChanges in the structure shown by the continuous emission from the Crab Nebula are investigated observationally and theoretically. A beautiful series of 200-inch plates from 1955 to the present provides the data on the morphology of the activity. Near the center of the nebula is a striking series of strongly polarized, elongated features called \"wisps\". The wisps in this series appear to move at velocities a significant fraction of the speed of light. The first and most prominent wisp is probably a permanent feature which moves about a characteristic position. Nearby is a fainter but similar region which sometimes shows one or more wisps. Centrally placed with respect to these two regions is a very thin wisp which shows more restricted notions. Since the two active regions are symmetrically placed about it, this thin wisp is in a sense the center of the activity. The nearby star is probably not associated with the nebula. Motion can be detected as well at the edges of the nebula. At the northwest edge in particular are rapidly moving objects which may be wisps which have propagated outward from the central region. The area of the nebula intermediate between the central wisps and these features near the edge is studied with a special technique, and there are indications of motions here too. In a general way all of the motions can be understood as disturbances in the plasma composed of relativistic gas, thermal gas, and magnetic field. The main wisp may act as a piston, exciting the other wisps in the form of propagating compressional waves. The velocity of propagation is set by the density of the thermal gas, which must be on the order of [...] to produce the observed velocities. Damping of these waves by resonance phenomena may be a source of energy for the relativistic particles sufficient to restore the synchrotron losses. Photoelectric observations show that the intrinsic spectrum is probably a power law with a slight excess of ultraviolet radiation. The power law, which decreases with increasing frequency, becomes steeper away from the center of the activity. This may be caused by the evolution of the electron energy distribution or by the injection of energy where the activity is strongest.\n", "date": "1968", "date_type": "degree", "id_number": "CaltechETD:etd-05022008-113526", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05022008-113526", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-16", "doi": "10.7907/4E5Y-0V49", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-02", "thesis_defense_date": "1968-02-08", "thesis_approved_date": "2008-05-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1968", "author_list": "Scargle, Jeffrey D." }, { "id": "/id/eprint/1562", "eprint_id": 1562, "rev_number": 8, "documents": [ { "id": "/id/document/2413", "doc_id": 2413, "rev_number": 2, "files": [ { "id": "/id/file/14940", "fileid": 14940, "datasetid": "document", "objectid": 2413, "filename": "Trimble_vl_1968.pdf", "mime_type": "application/pdf", "filesize": 4549736, "mtime": "2012-12-26 02:39:14", "url": "/1562/1/Trimble_vl_1968.pdf" } ], "eprint_id": 1562, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Trimble_vl_1968.pdf", "language": "en", "security": "public", "license": "other", "main": "Trimble_vl_1968.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19153" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19153" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19153" } ] } }, { "id": "/id/document/19153", "doc_id": 19153, "rev_number": 2, "files": [ { "id": "/id/file/14938", "fileid": 14938, "datasetid": "document", "objectid": 19153, "filename": "preview.png", "mime_type": "image/png", "hash": "9ae88948dc0ec6c84c0b2b4396119613", "hash_type": "MD5", "filesize": 10601, "mtime": "2012-12-26 02:39:13", "url": "/1562/2/preview.png" } ], "eprint_id": 1562, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2413" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2413" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2413" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/62", "datestamp": "2008-05-13", "lastmod": "2021-06-18 00:13:59", "status_changed": "2009-09-25 02:07:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Trimble-Virginia-Louise", "name": { "family": "Trimble", "given": "Virginia Louise" }, "show_email": "NO" } ] }, "title": "Motions and structure of the filamentary envelope of the Crab Nebula", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy", "abstract": "Proper motions have been measured for 132 line-emitting filaments in the Crab Nebula on direct plates taken with the 100 and 200-inch telescopes. These motions, if assumed constant and extrapolated backwards in time, converge toward a point about 12\" southeast of the double star near the center of the nebula. The filaments approach, on the average, most closely to that point or expansion center in about the year 1140, indicating that the expansion has been somewhat accelerated.\r\n\r\nProper motions and radial velocities were measured for an additional 126 features on the same direct plates and Mt. Wilson and Palomar spectra. These, along with other, nondynamical data, indicate a most probable distance to the object of 2.02 kpc. Two projections of the nebula perpendicular to the one seen in the plane of the sky are constructed and do not differ significantly from that presented to us.\r\n\r\nThe proper motion and radial velocity of the nebula as a whole are found and converted into galactic coordinates. This requires several assumptions of questionable validity. The nebula seems to be moving about 112 km/sec faster than the galactic rotation at its position. The proper motion of the so-called central star translates into an equally unlikely space motion, but this is also extremely uncertain. The likelihood of a physical connection between the star and the nebula is discussed.\r\n\r\nThe line-emitting filaments are shown to be distributed throughout the nebula rather than being confined to a thin outer envelope. The motions are largely radial, each filament having a velocity approximately proportional to its distance from the expansion center. The deviations from this proportionality are as large as .032\"/yr or 300 km/sec and have mean values near .010\"/yr or 70 km/sec. These deviations are correlated with the scatter of the filaments around the expansion center in 1140.\r\n\r\nPhotographic materials on pp. 99 and 101 are essential and will not reproduce clearly on Xerox copies. Photographic copies should be ordered.", "date": "1968", "date_type": "degree", "id_number": "CaltechETD:etd-05012008-085729", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05012008-085729", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-13", "doi": "10.7907/7DCP-QS42", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-01", "thesis_defense_date": "1968-04-17", "thesis_approved_date": "2008-05-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1968", "author_list": "Trimble, Virginia Louise" }, { "id": "/id/eprint/1682", "eprint_id": 1682, "rev_number": 9, "documents": [ { "id": "/id/document/2660", "doc_id": 2660, "rev_number": 2, "files": [ { "id": "/id/file/16347", "fileid": 16347, "datasetid": "document", "objectid": 2660, "filename": "Castor_ji_1967.pdf", "mime_type": "application/pdf", "filesize": 4800261, "mtime": "2012-12-26 02:40:37", "url": "/1682/1/Castor_ji_1967.pdf" } ], "eprint_id": 1682, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Castor_ji_1967.pdf", "language": "en", "security": "public", "license": "other", "main": "Castor_ji_1967.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19399" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19399" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19399" } ] } }, { "id": "/id/document/19399", "doc_id": 19399, "rev_number": 2, "files": [ { "id": "/id/file/16345", "fileid": 16345, "datasetid": "document", "objectid": 19399, "filename": "preview.png", "mime_type": "image/png", "hash": "f0086ff2018c5906874fb6f6c96ce382", "hash_type": "MD5", "filesize": 8835, "mtime": "2012-12-26 02:40:37", "url": "/1682/2/preview.png" } ], "eprint_id": 1682, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2660" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2660" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2660" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/16/82", "datestamp": "2008-05-09", "lastmod": "2024-03-15 18:22:02", "status_changed": "2009-09-25 02:11:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Castor-John-Irvin", "name": { "family": "Castor", "given": "John Irvin" }, "show_email": "NO" } ] }, "title": "Atmospheric Dynamics in a Model RR Lyrae Star", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nA dynamical model of an RR Lyrae star has been constructed which is similar to those of Christy (1) in its treatment of the envelope interior to the hydrogen ionization zone but which describes the hydrogen ionization zone and the outer atmosphere in some detail. In the optically thin region heat transfer is described with the gray equation of radiation transfer which yields an integral expression for the heating rate, assuming small deviations from sphericity.\r\n\r\nThe model which has been constructed has the parameters:\r\n\r\n\tM[subscript bol] = .76, T[subscript e] = 6500\u00b0K, [...] = .58[...], Y = .30.\r\n\r\nThe model results of Christy for the same parameters have been used as initial conditions.\r\n\r\nThe results have indicated a close connection between the complex hydrogen ionization zone dynamics and the observable phenomena in the star, such as rising branch shocks and the shape of the velocity curve during the decreasing light phase.\r\n\r\nThe work done by the hydrogen ionization zone to maintain pulsation has been found in this calculation to be in excellent agreement with the figure obtained by Christy for this star.\r\n\r\nDeviations from radiative equilibrium in the optically thin layers have been found to be confined to tau less than 0.1 and to high gravity, low temperature phases, when they may exceed 500\u00b0 K.\r\n\r\nModel atmospheres have been constructed with the dynamical pressure and temperature distributions using Mihalas' program (2). The emergent continuum fluxes obtained show considerable similarity to observed monochromatic light variation, although the amplitudes are greater and the rise time is less than is observed. The errors in temperature determinations based on fitting equilibrium models to the continuum have been found to be of the same order as fluctuations which appear in observational determinations of the radius variation.\r\n\r\nIt has been concluded that the differences between the model and the observed stars may be due in part to the omission of convection from the model, since it may become quite important during high gravity phases.", "date": "1967", "date_type": "degree", "id_number": "CaltechETD:etd-05082008-142946", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05082008-142946", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-09", "doi": "10.7907/EKJM-HV30", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-08", "thesis_defense_date": "1966-08-12", "thesis_approved_date": "2008-05-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1967", "author_list": "Castor, John Irvin" }, { "id": "/id/eprint/1556", "eprint_id": 1556, "rev_number": 10, "documents": [ { "id": "/id/document/2407", "doc_id": 2407, "rev_number": 2, "files": [ { "id": "/id/file/14896", "fileid": 14896, "datasetid": "document", "objectid": 2407, "filename": "Fomalont_eb_1967.pdf", "mime_type": "application/pdf", "filesize": 9905223, "mtime": "2012-12-26 02:39:12", "url": "/1556/1/Fomalont_eb_1967.pdf" } ], "eprint_id": 1556, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Fomalont_eb_1967.pdf", "language": "en", "security": "public", "license": "other", "main": "Fomalont_eb_1967.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19147" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19147" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19147" } ] } }, { "id": "/id/document/19147", "doc_id": 19147, "rev_number": 2, "files": [ { "id": "/id/file/14894", "fileid": 14894, "datasetid": "document", "objectid": 19147, "filename": "preview.png", "mime_type": "image/png", "hash": "267091ccf4c85ffa03bf53586fa81213", "hash_type": "MD5", "filesize": 9607, "mtime": "2012-12-26 02:39:12", "url": "/1556/2/preview.png" } ], "eprint_id": 1556, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2407" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2407" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2407" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/56", "datestamp": "2008-05-13", "lastmod": "2024-03-18 18:50:58", "status_changed": "2009-09-25 02:07:38", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fomalont-Edward-Berel", "name": { "family": "Fomalont", "given": "Edward Berel" }, "show_email": "NO" } ] }, "title": "The East-West Structure of Radio Sources at 1425 MHz", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe east-west radio structures of 532 sources have been obtained with the Caltech variable spacing interferometer at a frequency of 1425 MHz. The visibility functions, measured at nine interferometer spacings between 144[...] and 2626[...], are presented in tabular form for all of the sources. The east-west source structures were calculated by a model fit of the data or by a direct numerical inversion of the data.\r\n\r\nThe statistics of the radio structures have been analyzed. There are three major structure types: simple double, halo-core and triple. The simple double sources have two distinct components of emission having nearly equal intensities and diameters with the radio galaxy lying at the center of the two components in most cases. The halo-core sources consist of a small radio core, usually complex, coincident with the radio galaxy and a much larger region of emission, the halo, not necessarily symmetrically disposed around the radio core. The triple and more complex sources are discussed briefly and it is suggested that many are genetically related to double and halo-core sources.\r\n\r\nOther results from the observations are: a slight correlation of the radio and optical structure of galaxies; a difference for the N-S relationship of quasars and radio galaxies based on their statistical separation by brightness temperature; a model for the evolution of a double source in which the component separation increases at five times the rate of the expansion of the component diameters; the lack of simple sources characterized by one main region of emission; and the suggestion that 3C120 and 3C236 are involved in a violent explosion.\r\n", "date": "1967", "date_type": "degree", "id_number": "CaltechETD:etd-04302008-153110", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04302008-153110", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-13", "doi": "10.7907/W9HN-MY72", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Moffet-A-T", "name": { "family": "Moffet", "given": "Alan Theodore" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-04-30", "thesis_defense_date": "1966-08-20", "thesis_approved_date": "2008-05-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1967", "author_list": "Fomalont, Edward Berel" }, { "id": "/id/eprint/4408", "eprint_id": 4408, "rev_number": 9, "documents": [ { "id": "/id/document/7201", "doc_id": 7201, "rev_number": 2, "files": [ { "id": "/id/file/43875", "fileid": 43875, "datasetid": "document", "objectid": 7201, "filename": "Gunn_je_1966.pdf", "mime_type": "application/pdf", "filesize": 7396392, "mtime": "2012-12-26 03:08:26", "url": "/4408/1/Gunn_je_1966.pdf" } ], "eprint_id": 4408, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Gunn_je_1966.pdf", "language": "en", "security": "public", "license": "other", "main": "Gunn_je_1966.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23730" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23730" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23730" } ] } }, { "id": "/id/document/23730", "doc_id": 23730, "rev_number": 2, "files": [ { "id": "/id/file/43873", "fileid": 43873, "datasetid": "document", "objectid": 23730, "filename": "preview.png", "mime_type": "image/png", "hash": "229d9c4f242d1dee1e237eaa249dbd22", "hash_type": "MD5", "filesize": 10983, "mtime": "2012-12-26 03:08:26", "url": "/4408/2/preview.png" } ], "eprint_id": 4408, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7201" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7201" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7201" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/44/08", "datestamp": "2003-11-05", "lastmod": "2021-07-27 00:22:55", "status_changed": "2009-09-25 03:18:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gunn-James-Edward", "name": { "family": "Gunn", "given": "James Edward" }, "show_email": "NO" } ] }, "title": "A Mathematical Framework for Discussing the Statistical Distribution of Galaxies in Space and its Cosmological Implications", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "The spectral-theoretic techniques of stationary time-series analysis are generalized and applied to the study of the statistical distribution of galaxies in space and the observed distribution on the sky. Sampling techniques and criteria are developed for the measurement of the Fourier transform of the autocovariance function, the so-called \"power spectrum\". The theory is extended to curved, nonstatic space-times and the possibility of using the spectral density obtained from counts of galaxies in the formulation of cosmological tests is discussed. A similar development is made for the statistical structure of the background light due to very faint galaxies, and the possibility of measurement of this structure and its application to cosmological tests is considered. It is shown that in both cases (counts and background) significant cosmological data can be obtained if our knowledge of the luminosity function, the spectra, and the evolution of galaxies is improved. Finally, application is made of the theory to the analysis of a small count problem in order to learn something about the general form of the spatial covariance.", "date": "1966", "date_type": "degree", "id_number": "CaltechETD:etd-11052003-090546", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-11052003-090546", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department", "Caltech Distinguished Alumni Award" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-11-05", "doi": "10.7907/EV32-TQ73", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-11-05", "thesis_defense_date": "1965-10-01", "thesis_approved_date": "2003-11-05", "thesis_awards": "Caltech Distinguished Alumni Award, 2003", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1966", "author_list": "Gunn, James Edward" }, { "id": "/id/eprint/1563", "eprint_id": 1563, "rev_number": 9, "documents": [ { "id": "/id/document/2414", "doc_id": 2414, "rev_number": 2, "files": [ { "id": "/id/file/14947", "fileid": 14947, "datasetid": "document", "objectid": 2414, "filename": "Chandra_s_1966.pdf", "mime_type": "application/pdf", "filesize": 9292927, "mtime": "2012-12-26 02:39:14", "url": "/1563/1/Chandra_s_1966.pdf" } ], "eprint_id": 1563, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Chandra_s_1966.pdf", "language": "en", "security": "public", "license": "other", "main": "Chandra_s_1966.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19154" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19154" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19154" } ] } }, { "id": "/id/document/19154", "doc_id": 19154, "rev_number": 2, "files": [ { "id": "/id/file/14945", "fileid": 14945, "datasetid": "document", "objectid": 19154, "filename": "preview.png", "mime_type": "image/png", "hash": "92a0db977e21be40407caaf47730b6a7", "hash_type": "MD5", "filesize": 9648, "mtime": "2012-12-26 02:39:14", "url": "/1563/2/preview.png" } ], "eprint_id": 1563, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2414" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2414" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2414" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/63", "datestamp": "2008-05-13", "lastmod": "2024-02-23 00:13:46", "status_changed": "2009-09-25 02:07:46", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chandra-Subhash", "name": { "family": "Chandra", "given": "Subhash" }, "show_email": "NO" } ] }, "title": "A Study of Spectroscopic and Kinematic Characteristics of Peculiar A-Type Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nA spectroscopic survey of the different types of peculiar-A (Ap) stars has been made to discover the systematics of behavior of the various elements. Spectroscopic results are preceded by an account of some of the \"gross Properties\" investigated from the published data.\r\n\r\nGross Properties: (Chapter II): Under this group of investigations (a) intrinsic frequency distribution of the various peculiarity types is derived, (b) the controversy \"whether Ap stars are too blue for their HD spectral types\" is resolved, (c) mean absolute magnitudes of the different peculiarity types are derived by a statistical analysis of trigonometric parallaxes, and (d) space velocities are calculated which show significantly different solar motions for the different groups, but the velocity dispersions are found to be comparable.\r\n\r\nSpectroscopic Studies: This study is based mainly on 21 to 45 (A/mm) dispersion plates, in the UV and blue regions of the spectrum of [...] Ap and [...] normal stars. k (A) (Chapter III) By eliminating the effects of temperature, electron pressure, continuous absorption and microturbulence, \"strengthening\" and \"weakening\" of various elements has been estimated. From these estimates (Chapter VI): (i) behavior of the various elements in Ap stars is described, (ii) several interesting correlations between the observed anomalies of various elements have been discovered, and (iii) for Ap stars, a new system of classification is proposed which is based on the general pattern of abnormalities rather than on single most prominent features. (B) Extensive tables of reliable blend-free UV and blue lines are given for detection of the various elements (Chapter III). A similar table is given for the detection of all the rare-earths (Chapter V). In different stars, relative distribution of the rare-earths is found to be different. (C) A survey of BeII [...]3130-31 is made. In seven Ap stars, from \"Mn\" and \"Si-4200\" groups, this doublet is very strong. A quantitative Be abundance analysis is given (Chapter IV).\r\n\r\nVarious explanations for the appearance of the abnormal line strengths -- including the predicted nuclear processes -- are discussed in the light of the present results. Some specific suggestions for further work are also made (Chapter VI).", "date": "1966", "date_type": "degree", "id_number": "CaltechETD:etd-05012008-090141", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05012008-090141", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-13", "doi": "10.7907/KDF0-XZ45", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-01", "thesis_defense_date": "1966-05-20", "thesis_approved_date": "2008-05-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1966", "author_list": "Chandra, Subhash" }, { "id": "/id/eprint/3708", "eprint_id": 3708, "rev_number": 10, "documents": [ { "id": "/id/document/6324", "doc_id": 6324, "rev_number": 2, "files": [ { "id": "/id/file/37918", "fileid": 37918, "datasetid": "document", "objectid": 6324, "filename": "Kayser_se_1966.pdf", "mime_type": "application/pdf", "filesize": 9530941, "mtime": "2012-12-26 03:02:20", "url": "/3708/1/Kayser_se_1966.pdf" } ], "eprint_id": 3708, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Kayser_se_1966.pdf", "language": "en", "security": "public", "license": "other", "main": "Kayser_se_1966.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22862" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22862" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22862" } ] } }, { "id": "/id/document/22862", "doc_id": 22862, "rev_number": 2, "files": [ { "id": "/id/file/37916", "fileid": 37916, "datasetid": "document", "objectid": 22862, "filename": "preview.png", "mime_type": "image/png", "hash": "7800b454bcc68496a2b52d541fe59455", "hash_type": "MD5", "filesize": 9227, "mtime": "2012-12-26 03:02:20", "url": "/3708/2/preview.png" } ], "eprint_id": 3708, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6324" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6324" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6324" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/08", "datestamp": "2002-09-24", "lastmod": "2024-02-24 00:18:40", "status_changed": "2009-09-25 03:04:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "sukayser@gmail.com", "id": "Kayser-Susan-Elizabeth", "name": { "family": "Kayser", "given": "Susan Elizabeth" }, "show_email": "NO" } ] }, "title": "Photometry in the Nearby Irregular Galaxy, NGC 6822", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics) ; irregular galaxy; Local Group; NGC 6822", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nNGC 6822 is a member of the Local Group, type Im, coordinates [...]. The main body has a diameter of 3.6 c kpc and a mass (from radio rotation curves) of [...]. Mass-to-light ratio is 6.1 x c[superscript -1]. The color-magnitude diagram is plotted from measures on photographic plates calibrated by a photoelectric sequence. Photometry is complete to 19.5 (M[subscript v] = -5). Major features are bright blue supergiants, the brightest star having M [subscript v] = -9, and a sequence of very red supergiants one magnitude fainter than the blue, many of which show variations of over 1000 days. A significant number of stars lie in the Hertzsprung gap. Two-color photometry shows there is intervening reddening of [...]. A luminosity function is calculated.\r\n\r\nThirty-two variable stars are discussed, of which thirteen are Cepheids, two are red semi-regulars, one may be eclipsing, and the others are irregular. The period-luminosity relations for the Cepheids are < V > = 23.35 - 2. 97 log P and < B > = 23.91 - 2.61 log P. These lead to a true distance modulus (m-M) = 23.75 [plus or minus] 0.10. Secular changes in period are less than 0.001% in 40 years. The eleven variables with 1.6 < (B-V)[...] < 2. 1 have cycles 200-2500 days.\r\n\r\nComparisons with evolutionary models indicate that the stars observed have masses of 9 to 63 [...].", "date": "1966", "date_type": "degree", "id_number": "CaltechETD:etd-09232002-112325", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232002-112325", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-09-24", "doi": "10.7907/ZKRJ-7R03", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Arp-H-C", "name": { "family": "Arp", "given": "Halton C." }, "role": "advisor" }, { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-09-23", "thesis_defense_date": "1965-12-13", "thesis_approved_date": "2002-09-24", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1966", "author_list": "Kayser, Susan Elizabeth" }, { "id": "/id/eprint/1831", "eprint_id": 1831, "rev_number": 9, "documents": [ { "id": "/id/document/2997", "doc_id": 2997, "rev_number": 2, "files": [ { "id": "/id/file/18168", "fileid": 18168, "datasetid": "document", "objectid": 2997, "filename": "Divine_tn_1965.pdf", "mime_type": "application/pdf", "filesize": 9784833, "mtime": "2012-12-26 02:42:28", "url": "/1831/1/Divine_tn_1965.pdf" } ], "eprint_id": 1831, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Divine_tn_1965.pdf", "language": "en", "security": "public", "license": "other", "main": "Divine_tn_1965.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19707" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19707" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19707" } ] } }, { "id": "/id/document/19707", "doc_id": 19707, "rev_number": 2, "files": [ { "id": "/id/file/18166", "fileid": 18166, "datasetid": "document", "objectid": 19707, "filename": "preview.png", "mime_type": "image/png", "hash": "18ca875230ec1c9c07963dc3d9a35ec6", "hash_type": "MD5", "filesize": 8922, "mtime": "2012-12-26 02:42:28", "url": "/1831/2/preview.png" } ], "eprint_id": 1831, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2997" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2997" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2997" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/18/31", "datestamp": "2003-05-16", "lastmod": "2024-02-20 22:32:54", "status_changed": "2009-09-25 02:16:25", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Divine-Theodore-Neil", "name": { "family": "Divine", "given": "Theodore Neil" }, "show_email": "NO" } ] }, "title": "Structure and Evolution of Model Helium Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nNumerical models have been constructed which describe the evolution of stars which are initially pure helium. The iterative technique, programed for a large computer, permits the inclusion of radiation pressure, electron degeneracy, electron scattering opacity, gravitational contraction, and detailed composition changing brought about by triple-alpha and ([alpha],[gamma]) reactions.\r\n\r\nThe twenty homogeneous (pure helium) models, which range in mass from 0.4 to 60M[...] form a \"main sequence\" on the left of the H-R diagram. Evolutionary sequences of models at 0.5, 1, and 6M[...] exhaust their central helium supply in times of 80, 12, and 0.8 million years. Thereafter the connective core models, which have remained near their main sequence positions, are replaced by shell source models of increasing luminosity. At all three masses the final composition of the helium-exhausted core is almost exclusively oxygen, although a reduced rate for C[superscript 12]([alpha],[gamma])0[superscript 16] can lead to moderate fractions of carbon.\r\n\r\nThere is no clear indication that the models correspond to any group of observed stars. Massive helium star models may resemble Wolf-Rayet stars in mass, luminosity, and effective temperature.", "date": "1965", "date_type": "degree", "id_number": "CaltechETD:etd-05162003-095204", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05162003-095204", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-05-16", "doi": "10.7907/G079-F390", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-05-16", "thesis_defense_date": "1964-11-05", "thesis_approved_date": "2003-05-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1965", "author_list": "Divine, Theodore Neil" }, { "id": "/id/eprint/3479", "eprint_id": 3479, "rev_number": 9, "documents": [ { "id": "/id/document/6035", "doc_id": 6035, "rev_number": 2, "files": [ { "id": "/id/file/35965", "fileid": 35965, "datasetid": "document", "objectid": 6035, "filename": "Berge_g_1965.pdf", "mime_type": "application/pdf", "filesize": 6042946, "mtime": "2012-12-26 03:00:20", "url": "/3479/1/Berge_g_1965.pdf" } ], "eprint_id": 3479, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Berge_g_1965.pdf", "language": "en", "security": "public", "license": "other", "main": "Berge_g_1965.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22575" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22575" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22575" } ] } }, { "id": "/id/document/22575", "doc_id": 22575, "rev_number": 2, "files": [ { "id": "/id/file/35963", "fileid": 35963, "datasetid": "document", "objectid": 22575, "filename": "preview.png", "mime_type": "image/png", "hash": "1a7cb9647136f4373592e808e37a4ce3", "hash_type": "MD5", "filesize": 9044, "mtime": "2012-12-26 03:00:20", "url": "/3479/2/preview.png" } ], "eprint_id": 3479, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6035" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6035" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6035" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/79", "datestamp": "2002-09-13", "lastmod": "2019-12-21 01:54:37", "status_changed": "2009-09-25 02:59:15", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Berge-G-L", "name": { "family": "Berge", "given": "Glenn LeRoy" }, "show_email": "NO" } ] }, "title": "An interferometric study of Jupiter's decimeter radio emission", "ispublished": "unpub", "full_text_status": "public", "abstract": "NOTE: Text or symbols not rederable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nAn interferometric study of the decimeter radio emission from the planet Jupiter has recently been carried out at the Owens Valley Radio Observatory. Using the two 90-foot paraboloids as an interference polarimeter, observations have been made with various eastwest spacings ranging from 300 to [.......] at 10.4 cm. and 300 to [......] at 21.2 cm. and also with some critical north-south spacings at 10.4 cm.\r\n\r\nThe visibility functions obtained are consistent with earlier measurements, which gave the polar and equatorial dimensions as one and three planetary diameters respectively, but they are more complete and extend to larger baselines. They permit the fitting of a rather detailed model for the decimeter brightness distribution. The observations are consistent with a symmetrical synchrotron emission source having the polarization properties one would expect with a dipole magnetic field. It probably is centered quite closely on the planetary disk, which is itself seen as a thermal radio source.\r\n\r\nThe observations also indicate the presence of a small circularly polarized component in the radiation which varies in magnitude and sense as Jupiter rotates. Another result is that the disk emission at 10.4 cm. is about twice the thermal emission one would expect for a temperature of 130 [degrees] K.\r\n\r\nThe implications of the various results are discussed.", "date": "1965", "date_type": "degree", "id_number": "CaltechETD:etd-09122002-090152", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09122002-090152", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-09-13", "doi": "10.7907/QYHG-PN18", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stanley-G-J", "name": { "family": "Stanley", "given": "Gordon J." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-09-12", "thesis_defense_date": "1965-04-30", "thesis_approved_date": "2002-09-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1965", "author_list": "Berge, Glenn LeRoy" }, { "id": "/id/eprint/400", "eprint_id": 400, "rev_number": 14, "documents": [ { "id": "/id/document/580", "doc_id": 580, "rev_number": 2, "files": [ { "id": "/id/file/3726", "fileid": 3726, "datasetid": "document", "objectid": 580, "filename": "Trafton_lm_1965.pdf", "mime_type": "application/pdf", "filesize": 8570618, "mtime": "2012-12-26 02:29:24", "url": "/400/1/Trafton_lm_1965.pdf" } ], "eprint_id": 400, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Trafton_lm_1965.pdf", "language": "en", "security": "public", "license": "other", "main": "Trafton_lm_1965.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17406" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17406" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17406" } ] } }, { "id": "/id/document/17406", "doc_id": 17406, "rev_number": 2, "files": [ { "id": "/id/file/3724", "fileid": 3724, "datasetid": "document", "objectid": 17406, "filename": "preview.png", "mime_type": "image/png", "hash": "cea6c4621aef1218bc4eb0334209118f", "hash_type": "MD5", "filesize": 11235, "mtime": "2012-12-26 02:29:23", "url": "/400/2/preview.png" } ], "eprint_id": 400, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/580" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/580" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/580" } ] } }, { "id": "/id/document/46081", "doc_id": 46081, "rev_number": 3, "files": [ { "id": "/id/file/134996", "fileid": 134996, "datasetid": "document", "objectid": 46081, "filename": "Trafton Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "7b984f1f1ec0bf3a920b954f4129f0ca", "hash_type": "MD5", "filesize": 836, "mtime": "2014-02-14 18:35:07", "url": "/400/3/Trafton Thesis Permission Form.txt" } ], "eprint_id": 400, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "author ok feb 2014", "language": "en", "security": "internal", "license": "other", "main": "Trafton Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/04/00", "datestamp": "2004-01-30", "lastmod": "2019-12-20 19:49:14", "status_changed": "2009-09-25 01:36:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "lmt@astro.as.utexas.edu", "id": "Trafton-L-M", "name": { "family": "Trafton", "given": "Laurence Munro" }, "show_email": "YES" } ] }, "title": "A study of the energy balance in the atmospheres of the major planets", "ispublished": "unpub", "full_text_status": "public", "keywords": "Major planets, atmospheres, energy balance, radiation", "abstract": "The monochromatic absorption of infrared and microwave radiation due to pressure-induced rotational and translational transitions in H2 gas and gaseous mixtures of H2 and He is investigated quantitatively. Existing laboratory data are used to obtain semi-empirical absorption coefficients of the rotational transitions as a function of frequency. A quantum mechanical calculation is carried out to obtain the translational absorption coefficient as a function of frequency for a diatomic gas, mixtures of diatomic and monatomic gases and mixtures of monatomic gases. The resulting expressions are used to compute the translational absorption coefficient for H2 and the enhancement in H2-He mixtures using a 6 - 12 Lennard-Jones potential for the molecular interaction and the EXP-4 model for the expectation value of the induced dipole moment over the ground electronic and vibrational states. A numerical method is devised for the efficient computation of the translational absorption and the results of the computations are given. The infrared opacity of NH3 is also considered. With certain assumptions, existing laboratory data are used to obtain approximate, semi-empirical mean transmissions over the rotation structure of NH3 as a function of frequency.
\r\n\r\nSeveral non-gray model atmospheres are constructed for Jupiter, Saturn, Uranus and Neptune for various effective temperatures and He-H2 ratios taking the opacity due to H2 and He into account. The effect of adding the opacity due to NH3 is considered. The models are examined for self consistency and characteristic phenomena. They are then compared with the observations.
\r\n\r\nThe observations are used to restrict the range of the free parameters of the models. It is found that models of Jupiter and Neptune for which only the thermal opacity of H2 and NH3 is taken into account are incompatible with the observations. The presence of He is strongly indicated in the atmospheres of Jupiter, Uranus and Neptune. In the case of Jupiter, a rather large N(He)/N(H2) value is implied if there is no internal heat source. However, the observations indicate a preference for N(He)/N(H2) less than 2 and thus imply the existence of a small internal heat source greater than one-tenth of the incident solar flux. The effect of NH3 on the thermal equilibrium of the major planets is negligible except possibly in the case of Jupiter. However, its presence in the Jovian atmosphere does not alter the above conclusions.
", "date": "1965", "date_type": "degree", "id_number": "CaltechETD:etd-01292004-100142", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01292004-100142", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-01-30", "doi": "10.7907/F2DM-WX77", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "chair" }, { "id": "Christy-R-F", "name": { "family": "Christy", "given": "Robert F." }, "role": "member" }, { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "member" }, { "id": "Wildey-R", "name": { "family": "Wildey", "given": "Robert" }, "role": "member" }, { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverly" }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-01-29", "thesis_defense_date": "1965-03-19", "thesis_approved_date": "2004-01-30", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1965", "author_list": "Trafton, Laurence Munro" }, { "id": "/id/eprint/3454", "eprint_id": 3454, "rev_number": 14, "documents": [ { "id": "/id/document/5997", "doc_id": 5997, "rev_number": 2, "files": [ { "id": "/id/file/35733", "fileid": 35733, "datasetid": "document", "objectid": 5997, "filename": "Clark_b_1964.pdf", "mime_type": "application/pdf", "filesize": 7042163, "mtime": "2012-12-26 03:00:04", "url": "/3454/1/Clark_b_1964.pdf" } ], "eprint_id": 3454, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Clark_b_1964.pdf", "language": "en", "security": "public", "license": "other", "main": "Clark_b_1964.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22537" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22537" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22537" } ] } }, { "id": "/id/document/22537", "doc_id": 22537, "rev_number": 2, "files": [ { "id": "/id/file/35731", "fileid": 35731, "datasetid": "document", "objectid": 22537, "filename": "preview.png", "mime_type": "image/png", "hash": "95734f0f45f83c943cc598460e17a7c3", "hash_type": "MD5", "filesize": 9287, "mtime": "2012-12-26 03:00:04", "url": "/3454/2/preview.png" } ], "eprint_id": 3454, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5997" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5997" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5997" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/54", "datestamp": "2002-09-13", "lastmod": "2024-01-18 23:18:43", "status_changed": "2009-09-25 02:58:43", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Clark-Barry-Gillespie", "name": { "family": "Clark", "given": "Barry Gillespie" }, "show_email": "NO" } ] }, "title": "The Twenty-One Centimeter Hydrogen Line in Absorption", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe brightness distributions across five intense radio sources have been investigated in the hydrogen line absorption features. In some cases there has been found a variation of the absorption across the face of a source, which, with the kinematical distance to the cloud in question, allowed a typical length to be estimated, which in turn allows estimations of densities and masses. Densities range from a few atoms per cubic centimeter, to, in the case of a small cloud in front of Orion A, as much as 700 atoms per cubic centimeter. Masses range from a few solar masses up to perhaps a thousand solar masses in the cloud causing the deep line in Cas A.\r\n\r\nThe absorption profiles of the bright sources were analysed into Gaussian components, allowing parameters to be quoted for individual clouds, and, in a few cases, allowing an interesting upper limit to the temperature to be set from the dispersions of the separated components.\r\n\r\nThe absorption features in several other sources were briefly investigated, including three absorption spectra never before published, and new upper limits for the absorption of apparently unabsorbed sources were set in six cases. This material is briefly analysed statistically, from which it is concluded that the distribution law for central optical depths is approximately [...] and that a line of sight, on the average, intersects 4.1 clouds per kiloparsec in the galactic plane. There is some evidence that the density is about twice this in the local spiral arm.\r\n\r\nSome evidence is presented in favor of a \"raisin pudding\" model of the interstellar medium, in which clouds with temperatures of less than a hundred degrees supply all absorption, and most of the hydrogen line emission, while an appreciable part of the emission profiles is due to a hot intercloud medium of neutral hydrogen, at a temperature of several thousand degrees, and a density of about one half atom per cubic centimeter.", "date": "1964", "date_type": "degree", "id_number": "CaltechETD:etd-09112002-180017", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09112002-180017", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-09-13", "doi": "10.7907/385M-0W22", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "advisor" }, { "id": "Stanley-G-J", "name": { "family": "Stanley", "given": "Gordon J." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-09-11", "thesis_defense_date": "1964-04-04", "thesis_approved_date": "2002-09-13", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1964", "author_list": "Clark, Barry Gillespie" }, { "id": "/id/eprint/4149", "eprint_id": 4149, "rev_number": 9, "documents": [ { "id": "/id/document/6849", "doc_id": 6849, "rev_number": 2, "files": [ { "id": "/id/file/41551", "fileid": 41551, "datasetid": "document", "objectid": 6849, "filename": "Mendez_me_1964.pdf", "mime_type": "application/pdf", "filesize": 7395643, "mtime": "2012-12-26 03:05:54", "url": "/4149/1/Mendez_me_1964.pdf" } ], "eprint_id": 4149, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Mendez_me_1964.pdf", "language": "en", "security": "public", "license": "other", "main": "Mendez_me_1964.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23380" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23380" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23380" } ] } }, { "id": "/id/document/23380", "doc_id": 23380, "rev_number": 2, "files": [ { "id": "/id/file/41549", "fileid": 41549, "datasetid": "document", "objectid": 23380, "filename": "preview.png", "mime_type": "image/png", "hash": "84de38e5e903572a49328a278b0de0f1", "hash_type": "MD5", "filesize": 8038, "mtime": "2012-12-26 03:05:54", "url": "/4149/2/preview.png" } ], "eprint_id": 4149, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6849" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6849" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6849" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/41/49", "datestamp": "2002-10-21", "lastmod": "2024-01-19 23:19:37", "status_changed": "2009-09-25 03:12:30", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "M\u00e9ndez-Manuel-E", "name": { "family": "M\u00e9ndez", "given": "Manuel E." }, "show_email": "NO" } ] }, "title": "The Spectrophotometry of the Orion Nebula", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe spectral range from [lamda]3600 to [lamda]11 000 has been observed in the spectra of the Orion nebula. The large amount of dust in the nebula effects the intensity of the lines, according to their wavelengths. The correction, which takes into account this effect, has been obtained using the ratio of the Paschen to the Balmer lines, which arise from the same upper level. The unreddened spectrum-emission lines plus continuum has been analyzed.\r\n\r\nThe self-absorption of the Balmer lines has been proven to be non-existent. The Balmer decrement observed is almost equal to that produced by pure recombination. The helium lines indicate small departures from the prediction of the recombination theory. The metastability of the 2[superscript 3]S level has been investigated, including the ionization of the neutral atom, from this level, by Ly-[alpha] quanta. It has been demonstrated that the idea of the exciting star being in the center of the nebula, is consistent with the strengths of the [lamda]3889 lines observed in absorption. Since the self-absorption of the triplet lines of HeI is significant, the H/He ratio has been redetermined. The result indicates a ratio of 11 to 1 (by number).\r\n\r\nSince the recombination theory has been found to explain the Balmer decrement, the electron density distribution was obtained from surface brightness determinations and compared with the densities indicated by the [lamda]3726-29 [0II] lines obtained by Osterbrock in the past. A direct comparison of those two sets of observations has shown that the density fluctuations grow with distance from the center of the nebula. The mass of the nebula is about 30M[...] with a probable dust content of about 0.15M[...]. The latter quantity derived with the assumption that the radius of the solid particles can be represented by an average size of 0.16[microns].\r\n\r\nWith the use of the [0III] forbidden lines, the electron temperature was determined at several points in the nebula. The distribution obtained clearly indicates that the inner regions are colder than the outer. Since the lines of various elements were observed, an abundance determination was undertaken. The ratio, by number, of He to heavier elements is close to 50, which agrees with the abundance found in the solar cosmic rays. Then by mass, the chemical composition of the nebula can be represented by the following three numbers: X = 0.72, Y = 0.26,, and Z = 0.02.\r\n\r\nThe collision strengths for SII are not well known. Therefore an empirical determination of these parameters is also presented. The ratio of the nebular to auroral lines of [0II] also indicates the existence of density variations. The ratios observed in the nebula have been used to determine the extent of those fluctuations.", "date": "1964", "date_type": "degree", "id_number": "CaltechETD:etd-10182002-085141", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10182002-085141", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-10-21", "doi": "10.7907/SPX8-CV53", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-Guido", "name": { "family": "M\u00fcnch", "given": "Guido" } } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-10-18", "thesis_defense_date": "1964-01-01", "thesis_approved_date": "2002-10-21", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1964", "author_list": "M\u00e9ndez, Manuel E." }, { "id": "/id/eprint/4005", "eprint_id": 4005, "rev_number": 9, "documents": [ { "id": "/id/document/6673", "doc_id": 6673, "rev_number": 2, "files": [ { "id": "/id/file/40335", "fileid": 40335, "datasetid": "document", "objectid": 6673, "filename": "Mihalas_dm_1964.pdf", "mime_type": "application/pdf", "filesize": 11701620, "mtime": "2012-12-26 03:04:41", "url": "/4005/1/Mihalas_dm_1964.pdf" } ], "eprint_id": 4005, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Mihalas_dm_1964.pdf", "language": "en", "security": "public", "license": "other", "main": "Mihalas_dm_1964.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23207" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23207" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23207" } ] } }, { "id": "/id/document/23207", "doc_id": 23207, "rev_number": 2, "files": [ { "id": "/id/file/40333", "fileid": 40333, "datasetid": "document", "objectid": 23207, "filename": "preview.png", "mime_type": "image/png", "hash": "8cbe37cbaf5edd850ad06bb9020661ec", "hash_type": "MD5", "filesize": 7795, "mtime": "2012-12-26 03:04:41", "url": "/4005/2/preview.png" } ], "eprint_id": 4005, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6673" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6673" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6673" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/40/05", "datestamp": "2002-10-11", "lastmod": "2024-01-19 23:31:10", "status_changed": "2009-09-25 03:09:40", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mihalas-Dimitri-Manuel", "name": { "family": "Mihalas", "given": "Dimitri Manuel" }, "show_email": "NO" } ] }, "title": "Model Atmosphere Studies of Early Type Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nModel atmospheres have been constructed over a wide range of temperature and gravities. The condition of radiative equilibrium is enforced using a variation of the temperature correction scheme devised by M. Krook, thus extending the work of Gingerich to the realm of higher temperatures; flux constancy is attained to within [plus or minus]1% to a depth of [tau][subscript STD] = 10 or more, the standard wavelength being either [lamda]4000 or [lamda]5050. The source function is determined from the Milne-Eddington equation allowing for coherent scattering in the continuum. The properties of the atmospheres are described and given in detailed tabular form, and data of rather general use is presented.\r\n\r\nFor each model we have computed H[beta] and H[alpha] profiles and equivalent widths, and for the hotter models, profiles and equivalent widths of [lamda]4686, [lamda]4200, [lamda]4542 [lamda]5412 of He II and [lamda]5876, [lamda]4713, [lamda]4438, and [lamda]4121 of He I. Interpolating formulae are devised to describe the temperature and gravity variations of the line strengths.\r\n\r\nA fit is carried out between theory and observations made with the 100\" coude scanner of six O-type stars, yielding the effective temperature, gravity, and an estimate of the helium abundance for these stars. It is found that the computed hydrogen and ionized helium lines appear consistent with observation whereas the computed neutral helium lines seem to be incorrect for these spectral types.\r\n \r\nThe results indicate that a typical O9 star has the following properties: [theta][subscript e] = 0.146, log g = 4.2, N(He)/N(H) ~ 0.15 or 0.2, and from an assumed mass-luminosity law we find: R/R[...] = 10, [...] = 60, and L/L [...] = 1.4 x 10 [superscript 5]. The helium abundance derived here is in substantial agreement with that found by the Kiel group but in disagreement with nebular studies. The masses and radii are probably quite doubtful because of the possible incorrectness of the assumed mass-luminosity law.", "date": "1964", "date_type": "degree", "id_number": "CaltechETD:etd-10102002-094425", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10102002-094425", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-10-11", "doi": "10.7907/7TH1-H154", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Oke-J-B", "name": { "family": "Oke", "given": "J. Beverley" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-10-10", "thesis_defense_date": "1964-01-01", "thesis_approved_date": "2002-10-11", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1964", "author_list": "Mihalas, Dimitri Manuel" }, { "id": "/id/eprint/3427", "eprint_id": 3427, "rev_number": 10, "documents": [ { "id": "/id/document/5962", "doc_id": 5962, "rev_number": 2, "files": [ { "id": "/id/file/35499", "fileid": 35499, "datasetid": "document", "objectid": 5962, "filename": "Arpigny_c_1964.pdf", "mime_type": "application/pdf", "filesize": 7039668, "mtime": "2012-12-26 02:59:51", "url": "/3427/1/Arpigny_c_1964.pdf" } ], "eprint_id": 3427, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Arpigny_c_1964.pdf", "language": "en", "security": "public", "license": "other", "main": "Arpigny_c_1964.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22502" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22502" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22502" } ] } }, { "id": "/id/document/22502", "doc_id": 22502, "rev_number": 2, "files": [ { "id": "/id/file/35497", "fileid": 35497, "datasetid": "document", "objectid": 22502, "filename": "preview.png", "mime_type": "image/png", "hash": "88d45ed656d58cc9c6da90d38d206ef7", "hash_type": "MD5", "filesize": 8528, "mtime": "2012-12-26 02:59:50", "url": "/3427/2/preview.png" } ], "eprint_id": 3427, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/5962" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/5962" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/5962" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/27", "datestamp": "2002-09-16", "lastmod": "2024-01-18 22:50:58", "status_changed": "2009-09-25 02:58:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arpigny-Claude", "name": { "family": "Arpigny", "given": "Claude" }, "show_email": "NO" } ] }, "title": "A Study of Molecular and Physical Processes in Comets", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "The rotational structure of the violet CN (0, 0) band in cometary spectra is investigated from a new point of view. The usual assumption of a Boltzmann distribution of populations of the rotational levels in the ground state is abandoned. These populations are determined by solving the system of steady-state equations which describes the resonance-fluorescence of the CN band. As expected, it is possible in this way to reproduce the observed profile more satisfactorily than in the case when a Boltzmann distribution is used. Furthermore, it is shown that the Swings effect (presence of absorption lines in the solar exciting light) has to be taken into account from the beginning in the resolution of the system of the steady-state equations, to achieve complete agreement between observed and computed profiles.\r\nThe Greenstein effect (differences in relative intensities of rotational lines in different regions of the comet) has been studied in high-resolution spectrograms of Comet Seki-Lines (1962c). The observations can be interpreted partly by means of either of two simple models for the comet's head (uniform, isotropic expansion, or \"fountain model\"). In addition there are random motions of the order of a few km/sec.\r\nA detailed analysis of spectra of Comet Humason (1961e) has furnished the following results:\r\n\r\na) The CO+ comet-tail bands are excited by the same resonance-fluorescence mechanism known to be responsible for the emissions of the neutral molecules observed in the head.\r\n\r\nb) The continuum is of the pure reflection type: there is no detectable selective scattering.\r\n\r\nc) Molecular abundances are estimated (at 10[superscript 4] km from the nucleus) \r\n\tN(CO+)=10[superscript 13] cm[superscript -2]\r\n\tN(N2+)=10[superscript 11] cm[superscript -2]\r\n\tN(CN) = 5X10[superscript 10] cm[superscript -2]\r\n\r\nThe probable error on these estimates corresponds to a factor of 2 or 3.\r\n\r\nd) The infra-red surface brightness produced by the CO+ ions in pure vibration transitions v\" = 1 -> v\" = 0([lambda] approx.= 4.6 [mu]) is found to be rather large: approx.= 0.001 erg cm[superscript -2] sec[superscript -1].\r\n\r\ne) The radial distributions of the various molecules are discussed. While CN follows the usual l/[rho] law ([rho] being the projected distance from the nucleus), it is suggested that the remarkable flatness of the ion distributions might be explained in terms of a \"magnetic model.\"\r\n\r\nA critical discussion of some physical and chemical characteristics of comets is presented in the last chapter. In particular, the results of a number of abundance determinations are tabulated.\r\n\r\n\r\n(Photographic material on page 46 will not reproduce clearly on Xerox copies).", "date": "1964", "date_type": "degree", "id_number": "CaltechETD:etd-09102002-154144", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09102002-154144", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-09-16", "doi": "10.7907/Y86M-JB16", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-09-10", "thesis_defense_date": "1964-01-01", "thesis_approved_date": "2002-09-16", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1964", "author_list": "Arpigny, Claude" }, { "id": "/id/eprint/3979", "eprint_id": 3979, "rev_number": 10, "documents": [ { "id": "/id/document/6636", "doc_id": 6636, "rev_number": 2, "files": [ { "id": "/id/file/40097", "fileid": 40097, "datasetid": "document", "objectid": 6636, "filename": "Norton_rh_1964.pdf", "mime_type": "application/pdf", "filesize": 6996799, "mtime": "2012-12-26 03:04:26", "url": "/3979/1/Norton_rh_1964.pdf" } ], "eprint_id": 3979, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Norton_rh_1964.pdf", "language": "en", "security": "public", "license": "other", "main": "Norton_rh_1964.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23170" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23170" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23170" } ] } }, { "id": "/id/document/23170", "doc_id": 23170, "rev_number": 2, "files": [ { "id": "/id/file/40095", "fileid": 40095, "datasetid": "document", "objectid": 23170, "filename": "preview.png", "mime_type": "image/png", "hash": "e5f1dcf9e1a0f62ca2e6450d2239bb42", "hash_type": "MD5", "filesize": 7729, "mtime": "2012-12-26 03:04:26", "url": "/3979/2/preview.png" } ], "eprint_id": 3979, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6636" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6636" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6636" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/39/79", "datestamp": "2002-10-09", "lastmod": "2024-01-19 23:58:11", "status_changed": "2009-09-25 03:09:12", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Norton-Robert-Henry", "name": { "family": "Norton", "given": "Robert Henry" }, "show_email": "NO" } ] }, "title": "HeH\u207a in Model Stellar Atmospheres", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nApproximate quantum-mechanical calculations for the two lowest '[Sigma][superscript +] states of the helium hydride molecule ion HeH[superscript +] have been made. The molecular potential energy curves resulting from these calculations have been found to agree reasonably well with the results of other investigators. Using classical statistics for the distribution of internuclear separations, approximate absorption coefficients for radiative transitions between these two states have been obtained.\r\n\r\nA program to compute model stellar atmospheres in strict radiative equilibrium is described and was used to compute eight models with log g = 4.0 and effective temperatures between 9500[degrees]K and 30000[degrees]K. Total flux constant to within 1% was attained for these models excluding HeH[superscript +] as a source of opacity. When the final models were re-computed including the opacity of HeH[superscript +], radiative equilibrium was found to be destroyed by as much as 15%. Radiative equilibrium was re-established for the model with T[subscript e] = 16000[degrees] K, and a comparison between this model with and without HeH[superscript +] is given.\r\n\r\nIt is found that HeH[superscript +] introduces a striking discontinuity in the continuous spectrum of the model at 1130 A; the ratio of the emergent monochromatic flux on the red side of the discontinuity to the flux on the violet side is 8.2 for the 16000[degrees]K model. It is concluded that the wings of the Lyman lines, except L[...], are probably weaker than previously supposed.\r\n \r\nIn addition, numerical quadrature formulae of high accuracy and efficiency are given for integrals of the Schwarzschild-Milne type.", "date": "1964", "date_type": "degree", "id_number": "CaltechETD:etd-10082002-163233", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10082002-163233", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-10-09", "doi": "10.7907/YRJA-NP26", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-10-08", "thesis_defense_date": "1964-05-01", "thesis_approved_date": "2002-10-09", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1964", "author_list": "Norton, Robert Henry" }, { "id": "/id/eprint/1548", "eprint_id": 1548, "rev_number": 11, "documents": [ { "id": "/id/document/2399", "doc_id": 2399, "rev_number": 2, "files": [ { "id": "/id/file/14839", "fileid": 14839, "datasetid": "document", "objectid": 2399, "filename": "Parker_rar_1963.pdf", "mime_type": "application/pdf", "filesize": 7673942, "mtime": "2012-12-26 02:39:09", "url": "/1548/1/Parker_rar_1963.pdf" } ], "eprint_id": 1548, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Parker_rar_1963.pdf", "language": "en", "security": "public", "license": "other", "main": "Parker_rar_1963.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19139" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19139" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19139" } ] } }, { "id": "/id/document/19139", "doc_id": 19139, "rev_number": 2, "files": [ { "id": "/id/file/14837", "fileid": 14837, "datasetid": "document", "objectid": 19139, "filename": "preview.png", "mime_type": "image/png", "hash": "adde342d7f06148647d28288c6fe8a6f", "hash_type": "MD5", "filesize": 7571, "mtime": "2012-12-26 02:39:09", "url": "/1548/2/preview.png" } ], "eprint_id": 1548, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2399" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2399" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2399" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/48", "datestamp": "2008-04-30", "lastmod": "2024-01-08 23:54:25", "status_changed": "2009-09-25 02:07:27", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Parker-Robert-Allan-Ridley", "name": { "family": "Parker", "given": "Robert Allan Ridley" }, "show_email": "NO" } ] }, "title": "The Physical Conditions Pertaining to Some Possible Supernova Remnants", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nA large number of spectrophotometric observations have been made of 16 individual filaments in five possible supernova remnants, S 22, S 147, IC 443, NGC 6888, and the Cygnus Loop. Using these observations and making certain assumptions regarding abundances (that relative to Hydrogen we will expect abundances to be at least normal), it is shown that temperatures vary greatly within the filaments but are generally of the order of ten to fifteen thousand degrees for the regions from which we receive most of the [OII], [NII], [SII] , and Balmer emission. The densities for these same regions are of the order of a few hundred electrons per cubic centimeter. From these conclusions it is further indicated that: 1) the source of excitation of the Balmer lines is collisional; 2) all of the observed radio radiation from IC 443 and the Cygnus Loop can, by extrapolation from the observed total H[...] flux, be accounted for as thermal radiation; 3) the total mass of the visible filaments of IC 443, NGC 6888 and the Cygnus Loop is of the order of several tens of solar masses; and 4) the apparent filaments are actually only the results of the projection effect for shells.\r\n", "date": "1963", "date_type": "degree", "id_number": "CaltechETD:etd-04292008-090916", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04292008-090916", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-04-30", "doi": "10.7907/XGR5-7574", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-04-29", "thesis_defense_date": "1963-01-01", "thesis_approved_date": "2008-04-30", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1963", "author_list": "Parker, Robert Allan Ridley" }, { "id": "/id/eprint/3731", "eprint_id": 3731, "rev_number": 9, "documents": [ { "id": "/id/document/6347", "doc_id": 6347, "rev_number": 2, "files": [ { "id": "/id/file/38088", "fileid": 38088, "datasetid": "document", "objectid": 6347, "filename": "Wildey_rl_1962.pdf", "mime_type": "application/pdf", "filesize": 6628492, "mtime": "2012-12-26 03:02:30", "url": "/3731/1/Wildey_rl_1962.pdf" } ], "eprint_id": 3731, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Wildey_rl_1962.pdf", "language": "en", "security": "public", "license": "other", "main": "Wildey_rl_1962.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22885" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22885" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22885" } ] } }, { "id": "/id/document/22885", "doc_id": 22885, "rev_number": 2, "files": [ { "id": "/id/file/38086", "fileid": 38086, "datasetid": "document", "objectid": 22885, "filename": "preview.png", "mime_type": "image/png", "hash": "df2349b9bc0f8be430916f97033d6e22", "hash_type": "MD5", "filesize": 8444, "mtime": "2012-12-26 03:02:29", "url": "/3731/2/preview.png" } ], "eprint_id": 3731, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6347" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6347" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6347" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/31", "datestamp": "2008-11-06", "lastmod": "2023-11-27 21:26:39", "status_changed": "2009-09-25 03:04:20", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wildey-Robert-LeRoy", "name": { "family": "Wildey", "given": "Robert LeRoy" }, "show_email": "NO" } ] }, "title": "The Stellar Content of the Perseus Galactic Arm in the Region of h and Chi Persei", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy)", "abstract": "A total of 944 stars in the general region of h and chi Persei in the Perseus Galactic arm have been observed photometrically in U, B, and V of the Johnson-Morgan photometric system. Supergiants, O stars, giants, subgiants, and their fainter immediate neighbors (used to obtain reddenings) totaling 336 stars have been measured photoelectrically in the general OB association of which the galactic clusters form the nucleus. Within the extreme nuclei of the clusters-proper, photoelectrically calibrated photographic observations have been made with completeness down to about 18th magnitude on an additional 608 stars; however, the photoelectric limit is V = 17. 0. Fine structure is exhibited by the stars above the vertical main sequence and a slightly fainter red off-shoot is found. A sequence of stars is found in apparent gravitational contraction but with main-sequence stars extending, nevertheless, to the observational limit. At present the data is best represented by theories of gravitational contraction, hydrogen-burning, and helium-burning, together with a non-unique epoch of stellar condensation. Contraction and nuclear time-scales for the different features are compatible. The differences in apparent evolutionary tracks between the Galaxy, LMC, and SMC are reconfirmed. The 2-color diagram of the bluest stars is of a gray-body character. Sp vs (B-V)[subscript o] is monotonic for all stars. The M supergiants are shifted red-ward over previous studies and form a steep 2-color relation.", "date": "1962", "date_type": "degree", "id_number": "CaltechETD:etd-09232008-080747", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09232008-080747", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-06", "doi": "10.7907/TNJ1-XF88", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Arp-H-C", "name": { "family": "Arp", "given": "Halton C." }, "role": "advisor" }, { "id": "Sandage-A-R", "name": { "family": "Sandage", "given": "Allan R." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-09-23", "thesis_defense_date": "1962-01-01", "thesis_approved_date": "2008-11-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1962", "author_list": "Wildey, Robert LeRoy" }, { "id": "/id/eprint/1237", "eprint_id": 1237, "rev_number": 22, "documents": [ { "id": "/id/document/1875", "doc_id": 1875, "rev_number": 2, "files": [ { "id": "/id/file/11753", "fileid": 11753, "datasetid": "document", "objectid": 1875, "filename": "Wilson_rw_1962.pdf", "mime_type": "application/pdf", "filesize": 10504319, "mtime": "2012-12-26 02:36:32", "url": "/1237/1/Wilson_rw_1962.pdf" } ], "eprint_id": 1237, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Wilson_rw_1962.pdf", "language": "en", "security": "public", "license": "other", "main": "Wilson_rw_1962.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18655" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18655" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18655" } ] } }, { "id": "/id/document/18655", "doc_id": 18655, "rev_number": 2, "files": [ { "id": "/id/file/11751", "fileid": 11751, "datasetid": "document", "objectid": 18655, "filename": "preview.png", "mime_type": "image/png", "hash": "e3b46b7e361db776296a18739b96ecc4", "hash_type": "MD5", "filesize": 8357, "mtime": "2012-12-26 02:36:32", "url": "/1237/2/preview.png" } ], "eprint_id": 1237, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1875" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/1875" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1875" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/12/37", "datestamp": "2003-04-01", "lastmod": "2023-11-27 21:33:09", "status_changed": "2009-09-25 01:58:48", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wilson-Robert-Woodrow", "name": { "family": "Wilson", "given": "Robert Woodrow" }, "show_email": "NO" } ] }, "title": "Observations of the Galactic Plane at 960 Mc/s", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "note": "Thesis title in 1962 Commencement program varies slightly: \"Observations of the Galactic Plane at 960 Megacycles per Second\".\r\n\r\nThe Nobel Prize in Physics 1978 was divided, one half awarded to Pyotr Leonidovich Kapitsa \"for his basic inventions and discoveries in the area of low-temperature physics\", the other half jointly to Arno Allan Penzias and Robert Woodrow Wilson \"for their discovery of cosmic microwave background radiation.\"", "abstract": "A survey of the radio radiation at 960 Mc/s from the part of the plane of the Galaxy with declination above 48\u00b0 has been made. 112 discrete sources were found in the region studied. The positions, intensities, and sizes of these sources have been catalogued, and a search for optical identifications made. The broadly distributed radiation is interpreted in terms of a space distribution of ionized hydrogen and of emissivity from synchrotron emission.", "date": "1962", "date_type": "degree", "id_number": "CaltechETD:etd-04012003-131925", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04012003-131925", "related_url": { "items": [ { "description": "Nobel Prize announcement (Physics, 1978)", "type": "org", "url": "https://www.nobelprize.org/prizes/physics/1978/summary/" } ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Nobel Prize", "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-04-01", "doi": "10.7907/1R1X-J090", "alt_title": { "items": [ "Observations of the Galactic Plane at 960 Megacycles per Second" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Bolton-J-G", "name": { "family": "Bolton", "given": "John G." }, "role": "advisor" }, { "id": "Schmidt-M", "name": { "family": "Schmidt", "given": "Maarten" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-04-01", "thesis_defense_date": "1962-01-01", "thesis_approved_date": "2003-04-01", "thesis_awards": "The Nobel Prize in Physics, 1978.", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1962", "author_list": "Wilson, Robert Woodrow" }, { "id": "/id/eprint/1070", "eprint_id": 1070, "rev_number": 20, "documents": [ { "id": "/id/document/1647", "doc_id": 1647, "rev_number": 2, "files": [ { "id": "/id/file/10252", "fileid": 10252, "datasetid": "document", "objectid": 1647, "filename": "Harris_de_1961.pdf", "mime_type": "application/pdf", "filesize": 9860925, "mtime": "2012-12-26 02:35:07", "url": "/1070/1/Harris_de_1961.pdf" } ], "eprint_id": 1070, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Harris_de_1961.pdf", "language": "en", "security": "public", "license": "other", "main": "Harris_de_1961.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/18427" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/18427" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/18427" } ] } }, { "id": "/id/document/18427", "doc_id": 18427, "rev_number": 2, "files": [ { "id": "/id/file/10250", "fileid": 10250, "datasetid": "document", "objectid": 18427, "filename": "preview.png", "mime_type": "image/png", "hash": "457a9405db392549d34528fddf79b39b", "hash_type": "MD5", "filesize": 9948, "mtime": "2012-12-26 02:35:07", "url": "/1070/2/preview.png" } ], "eprint_id": 1070, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/1647" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/1647" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/1647" } ] } }, { "id": "/id/document/45781", "doc_id": 45781, "rev_number": 3, "files": [ { "id": "/id/file/134224", "fileid": 134224, "datasetid": "document", "objectid": 45781, "filename": "Harris Thesis Permission Form.txt", "mime_type": "message/rfc822\\0117bit", "hash": "cfb333ad9ee5e5f5c4d9460ff617dd45", "hash_type": "MD5", "filesize": 849, "mtime": "2014-02-10 20:00:56", "url": "/1070/3/Harris Thesis Permission Form.txt" } ], "eprint_id": 1070, "pos": 3, "placement": 3, "mime_type": "message/rfc822\\0117bit", "format": "text/plain", "format_desc": "author ok feb 2014", "language": "en", "security": "internal", "license": "other", "main": "Harris Thesis Permission Form.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/10/70", "datestamp": "2006-03-27", "lastmod": "2023-11-17 00:37:44", "status_changed": "2009-09-25 01:54:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "harris.d.e.42@gmail.com", "id": "Harris-Daniel-Everett", "name": { "family": "Harris", "given": "Daniel Everett" }, "show_email": "YES" } ] }, "title": "The Continuous Spectra of Radio Sources with Particular Reference to Non-Thermal Galactic Sources", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics) ; 3C radio sources; spectral index; Owens Valley Radio Observatory", "note": "This was the first PhD thesis coming out of the Owens Valley Radio Observatory.", "abstract": "960 Mc observations of over 400 sources are reported in two parts. Part I contains position and intensity measurements of 106 sources (chiefly taken from the recent Cambridge surveys), and the results of 376 intensity measurements of sources previously observed at Sydney. Spectral indices are derived from the intensity measurements and the previous investigator's observations. The resulting spectral index distribution has a median value of -0.65 \u00b1 0.10 and a dispersion such that 75% of the values lie within 0.25 of the median. Galactic sources show a larger dispersion of spectral index than do the sources assumed to be external galaxies.
\r\n\r\nPart II is based on 960 Mc observations of extended galactic nebulae, usually identified with supernova remnants. Contour diagrams of antenna temperature are presented for four of the larger objects. A detailed study of the Cygnus Loop shows that the radio emission is chiefly non-thermal, with a spectral index of -0.1 \u00b1 0.1. An attempt to detect linear polarization places an upper limit of 30% for selected regions of the Cygnus Loop. Spectral indices ranging from -0.8 to +0.5 are derived for 12 other sources. Calculations show that the occurrence of optical synchrotron radiation is not ruled out by existing observations. An empirical relation between spectral index and physical size of supernova remnants suggests that the energy spectrum of relativistic particles flattens with age. A possible mechanism for this behavior is considered.
", "date": "1961", "date_type": "degree", "id_number": "CaltechETD:etd-03232006-111338", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-03232006-111338", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Owens Valley Radio Observatory (OVRO)", "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-03-27", "doi": "10.7907/N09S-3J04", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stanley-G-J", "name": { "family": "Stanley", "given": "Gordon J." }, "role": "advisor" }, { "id": "Bolton-J-G", "name": { "family": "Bolton", "given": "John G." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-03-23", "thesis_defense_date": "1961-01-01", "thesis_approved_date": "2006-03-27", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1961", "author_list": "Harris, Daniel Everett" }, { "id": "/id/eprint/416", "eprint_id": 416, "rev_number": 9, "documents": [ { "id": "/id/document/636", "doc_id": 636, "rev_number": 2, "files": [ { "id": "/id/file/4007", "fileid": 4007, "datasetid": "document", "objectid": 636, "filename": "Bonsack_wk_1959.pdf", "mime_type": "application/pdf", "filesize": 12066530, "mtime": "2012-12-26 02:29:42", "url": "/416/1/Bonsack_wk_1959.pdf" } ], "eprint_id": 416, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Bonsack_wk_1959.pdf", "language": "en", "security": "public", "license": "other", "main": "Bonsack_wk_1959.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17462" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17462" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17462" } ] } }, { "id": "/id/document/17462", "doc_id": 17462, "rev_number": 2, "files": [ { "id": "/id/file/4005", "fileid": 4005, "datasetid": "document", "objectid": 17462, "filename": "preview.png", "mime_type": "image/png", "hash": "23f8a3bfa294e978028e3dbaf65b8ed4", "hash_type": "MD5", "filesize": 7666, "mtime": "2012-12-26 02:29:42", "url": "/416/2/preview.png" } ], "eprint_id": 416, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/636" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/636" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/636" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/04/16", "datestamp": "2006-01-31", "lastmod": "2023-10-18 16:33:25", "status_changed": "2009-09-25 01:37:06", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bonsack-Walter-Karl", "name": { "family": "Bonsack", "given": "Walter Karl" }, "show_email": "NO" } ] }, "title": "The Abundance of Lithium in the Atmospberes of Cool Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "The abundance of lithium relative to vanadium, or its upper limit, has been determined for forty-six normal stars of spectral types from G8 to MO, inclusive. These results are based upon high-dispersion spectrograms obtained with the coude spectrograph of the Hooker telescope. The abundance ratio for the sun has also been determined, using the equivalent width for lithium measured by Greenstein and Richardson and measurements of vanadiumm lines in the Utrecht Atlas.\r\n\r\nValues have also been obtained of quantities related to the physical conditions in the stellar atmoshperes.\r\n\r\nA range of up to a factor of one hundred in the abundance ratio is found among stars of similar surface characteristics. However, the maximum abundance ratio observed among similar stars declines with surface temperature.\r\n\r\nIt is not likely that a significant part of the variation is due to vanadium abundance.\r\n\r\nGreenstein and Richardson have proposed that the lithuim in the solar surface has been depleted by convective mixing to hotter regions. It is suggested that this hypothesis may explain both the trend and the variations observed in the cooler stars.", "date": "1959", "date_type": "degree", "id_number": "CaltechETD:etd-01312006-133428", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01312006-133428", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-01-31", "doi": "10.7907/HAVA-YH31", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-01-31", "thesis_defense_date": "1959-01-01", "thesis_approved_date": "2006-01-31", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1959", "author_list": "Bonsack, Walter Karl" }, { "id": "/id/eprint/654", "eprint_id": 654, "rev_number": 10, "documents": [ { "id": "/id/document/969", "doc_id": 969, "rev_number": 2, "files": [ { "id": "/id/file/6111", "fileid": 6111, "datasetid": "document", "objectid": 969, "filename": "Melbourne_wg_1959.pdf", "mime_type": "application/pdf", "filesize": 15587577, "mtime": "2012-12-26 02:31:15", "url": "/654/1/Melbourne_wg_1959.pdf" } ], "eprint_id": 654, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Melbourne_wg_1959.pdf", "language": "en", "security": "public", "license": "other", "main": "Melbourne_wg_1959.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17771" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17771" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17771" } ] } }, { "id": "/id/document/17771", "doc_id": 17771, "rev_number": 2, "files": [ { "id": "/id/file/6109", "fileid": 6109, "datasetid": "document", "objectid": 17771, "filename": "preview.png", "mime_type": "image/png", "hash": "d769d8f7d31d44e714623cbae2292736", "hash_type": "MD5", "filesize": 8032, "mtime": "2012-12-26 02:31:15", "url": "/654/2/preview.png" } ], "eprint_id": 654, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/969" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/969" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/969" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/06/54", "datestamp": "2006-02-17", "lastmod": "2023-10-18 22:14:16", "status_changed": "2009-09-25 01:43:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Melbourne-William-Geary", "name": { "family": "Melbourne", "given": "William Geary" }, "show_email": "NO" } ] }, "title": "Line Blanketing Effects on Middle-Type Main-Sequence and Sub-Dwarf Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "The subject of line blanketing and its effect on the continuous radiation and measured colors of stars is reviewed. Observed energy distributions which have been corrected for blanketing are compared with theoretical flux distributions derived from model atmospheres. Reasonable agreement is found and the comparisons serve to establish a set of effective temperatures for the stars under study.\r\n\r\nThe UBV colors of the program stars are computed from observed energy distributions and the results are compared with the observed colors. The theoretical colors are also obtained. The effects of line blanketing with and without the hydrogen lines on the UBV colors are quantitatively assessed. A three dimensional (U-B) -- (B-V) -- effective temperature relationship is discussed. The above analysis leads to line-free UBV and color-magnitude main-sequence relationships.", "date": "1959", "date_type": "degree", "id_number": "CaltechETD:etd-02172006-090057", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-02172006-090057", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-02-17", "doi": "10.7907/EJ3Z-2917", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Code-A-D", "name": { "family": "Code", "given": "Arthur D." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-02-17", "thesis_defense_date": "1959-01-01", "thesis_approved_date": "2006-02-17", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1959", "author_list": "Melbourne, William Geary" }, { "id": "/id/eprint/255", "eprint_id": 255, "rev_number": 24, "documents": [ { "id": "/id/document/381", "doc_id": 381, "rev_number": 3, "files": [ { "id": "/id/file/2415", "fileid": 2415, "datasetid": "document", "objectid": 381, "filename": "Wallerstein_g_1958.pdf", "mime_type": "application/pdf", "filesize": 14180478, "mtime": "2012-12-26 02:28:25", "url": "/255/1/Wallerstein_g_1958.pdf" } ], "eprint_id": 255, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Wallerstein_g_1958.pdf", "language": "en", "security": "internal", "license": "other", "main": "Wallerstein_g_1958.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/106885" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/106885" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/106885" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/02/55", "datestamp": "2006-01-24", "lastmod": "2023-10-17 18:48:42", "status_changed": "2009-09-25 01:32:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wallerstein-George", "name": { "family": "Wallerstein", "given": "George" }, "orcid": "0000-0003-3416-8728", "show_email": "NO" } ] }, "title": "Spectra of Population II Cepheid Variable Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "The physical properties of the population II cepheids have been studied using the following material: photoelectric observations of Arp, low dispersion spectra of Joy, high dispersion spectra taken by Sanford and Abt, and numerous moderate dispersion spectra obtained by the author.
\r\n\r\nRadial velocity curves for ten cepheids are shown. It is shown that the velocity curves for all population II cepheids with periods greater than 15 days are probably discontinuous. The difference between the RV tauri star an the star whose velocity and light curves repeat well is shown to be due to a delay in the new outrush of gas during alternate cycles of the RV tauri star. Displacement curves are derived for eight cepheids that probably have discontinuous velocity curves.
\r\n\r\nThe photoelectric observations are interpreted to show that the surface temperature M5 No. 42 varies from 7200\u00b0K to 4800\u00b0K and of W Virginis from 6200\u00b0K to below 4800\u00b0K. The electron pressure for the two stars varies from 100 dynes/cm\u00b2 to 0.1 dynes/cm\u00b2 and 10 dynes/cm\u00b2 to less than 0.1 dynes/cm\u00b2 respectively. The changes in radii obtained applying Steffan's Law to the changes in temperature and luminosity agree reasonably well with integration of the velocity curve. Values of the surface gravity obtained from the colors at maximum radius and from the deceleration of the velocity curve yield masses in the vicinity of one to three solar masses. The use of the period density relation is consistent with masses between 1.2 and 2.0 solar masses.
\r\n\r\nThe spectra of the population II cepheids are generally of type A5 to F0 at earliest a F5 to G0 at latest. No correlation of spectral type with period can found. A correlation between spectral type and light curve seems to be present.
\r\n\r\nConsideration of the emission lines and of certain absorption lines that are effected by dilution leads to the conclusion that proper model for W Virginis must contain a shock wave moving out through the atmosphere of the star.
", "date": "1958", "date_type": "degree", "id_number": "CaltechETD:etd-01202006-142307", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01202006-142307", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-01-24", "doi": "10.7907/JGXJ-B131", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-01-20", "thesis_defense_date": "1958-01-01", "thesis_approved_date": "2006-01-24", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1958", "author_list": "Wallerstein, George" }, { "id": "/id/eprint/233", "eprint_id": 233, "rev_number": 9, "documents": [ { "id": "/id/document/336", "doc_id": 336, "rev_number": 2, "files": [ { "id": "/id/file/2148", "fileid": 2148, "datasetid": "document", "objectid": 336, "filename": "Tifft_wg_1958.pdf", "mime_type": "application/pdf", "filesize": 5571674, "mtime": "2012-12-26 02:28:11", "url": "/233/1/Tifft_wg_1958.pdf" } ], "eprint_id": 233, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Tifft_wg_1958.pdf", "language": "en", "security": "public", "license": "other", "main": "Tifft_wg_1958.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17161" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17161" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17161" } ] } }, { "id": "/id/document/17161", "doc_id": 17161, "rev_number": 2, "files": [ { "id": "/id/file/2146", "fileid": 2146, "datasetid": "document", "objectid": 17161, "filename": "preview.png", "mime_type": "image/png", "hash": "125fd8c67014db3829ccde4de8fa64d1", "hash_type": "MD5", "filesize": 7955, "mtime": "2012-12-26 02:28:10", "url": "/233/2/preview.png" } ], "eprint_id": 233, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/336" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/336" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/336" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/02/33", "datestamp": "2006-01-24", "lastmod": "2023-10-17 16:48:22", "status_changed": "2009-09-25 01:31:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tifft-William-Grant", "name": { "family": "Tifft", "given": "William Grant" }, "show_email": "NO" } ] }, "title": "Multicolor Photoelectric Photometry of Bright Extragalactic Systems", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "57 galaxies and 52 stars have been observed in four colors using a blue sensitive phototube. The response bands of the photometric system have effective reciprocal wave lengths of (micron units) 2.66, 2.39, 2.07, and 1.68. In addition to the blue measurements 8 galaxies and 19 stars have been observed in four colors using a red sensitive photocell. The effective reciprocal wave lengths of the red response bands are 1.55, 1.26, 1.14, and 1.00. From one to five different aperture sizes have been used in the photometry of each galaxy, with an average of three per galaxy. The entire eight color photometric system has been calibrated to place color index measurements on an absolute energy basis.\r\n\r\nCorrelations between nuclear color index and inclination, spectral class, and nebular type indicate that most of the observed galaxies fall into fairly distinct groups. Radial color variations are also found to correlate with group membership. The dominant characteristics of the groups are as follows: Spectral type A, spectral type F, spectral type FG, nebular type SA, nebular type E, nebular type SO, nebular type SB.\r\n\r\nThe correlation between nuclear color and inclination (axis ratio) is found to show a distinct separation of SA, SB, and elliptical galaxies, probably due in part to differences in internal absorption. The correlation of nuclear color and spectral type shows that FG galaxies, while later in spectral class than F galaxies, have nuclei bluer than those in F galaxies. A possible explanation is offered which interprets the inversion in terms of the relative numbers of normal and low metal abundance stars in each type of galaxy. Radial color investigation reveal the existence of blue nuclei in three galaxies.\r\n\r\nSynthetic models are given for five distinct types of extragalactic nuclei. K nuclei can be represented with a mixture of old population I and II stars. F, FG, and probably AF nuclei can be produced by adding various numbers of young blue stars to K galaxies. A type galaxies appear to be completely dominated by young stars.", "date": "1958", "date_type": "degree", "id_number": "CaltechETD:etd-01192006-093239", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01192006-093239", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2006-01-24", "doi": "10.7907/Q9G6-YA63", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Code-A-D", "name": { "family": "Code", "given": "Arthur D." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2006-01-19", "thesis_defense_date": "1958-01-01", "thesis_approved_date": "2006-01-24", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1958", "author_list": "Tifft, William Grant" }, { "id": "/id/eprint/1581", "eprint_id": 1581, "rev_number": 19, "documents": [ { "id": "/id/document/87107", "doc_id": 87107, "rev_number": 2, "files": [ { "id": "/id/file/246960", "fileid": 246960, "datasetid": "document", "objectid": 87107, "filename": "Abell_GO_1957.pdf", "mime_type": "application/pdf", "hash": "89581181e78ba4dcd5300c18757bd548", "hash_type": "MD5", "filesize": 61337040, "mtime": "2018-03-09 19:10:32", "url": "/1581/1/Abell_GO_1957.pdf" } ], "eprint_id": 1581, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Abell_GO_1957.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"archive", "userid": 2, "dir": "disk0/00/00/15/81", "datestamp": "2007-05-03", "lastmod": "2023-08-15 19:56:23", "status_changed": "2009-09-25 02:08:16", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abell-George-Ogden", "name": { "family": "Abell", "given": "George Ogden" }, "show_email": "NO" } ] }, "title": "The Distribution of Rich Clusters of Galaxies", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "A catalogue is prepared of 2712 rich clusters of galaxies found on the National Geographic Society--Palomar Observatory Sky Survey. From the catalogue, 1682 clusters are selected which meet specific criteria for inclusion in a homogeneous statistical sample.
\r\n\r\nAn investigation of the sample leads to the following conclusions: (i) The distribution function of clusters according to richness, N(n) increases rapidly as n decreases. (ii) The data allow no significant decision that the spatial density of cluster centers varies with distance. (iii) Galactic obscuration of the order of a few tenths of a magnitude (photored) exists at high northern galactic latitudes around galactic longitude 300\u00b0. (iv) There is a highly significant nonrandom distribution of clusters in direction, both when clusters at all distances and when clusters at various distances are considered. An analysis of the distribution yields strong evidence for the existence of second-order clusters, that is clusters of clusters of galaxies. A statistical test shows the observed distribution to be compatible with the assumption of complete second-order clustering of galaxies.
", "date": "1957", "date_type": "degree", "id_number": "CaltechETD:etd-05022007-092134", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05022007-092134", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-03", "doi": "10.7907/99X5-ZM38", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Osterbrock-D-E", "name": { "family": "Osterbrock", "given": "Donald E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-02", "thesis_defense_date": "1957-01-01", "thesis_approved_date": "2007-05-03", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1957", "author_list": "Abell, George Ogden" }, { "id": "/id/eprint/2493", "eprint_id": 2493, "rev_number": 10, "documents": [ { "id": "/id/document/4748", "doc_id": 4748, "rev_number": 2, "files": [ { "id": "/id/file/27368", "fileid": 27368, "datasetid": "document", "objectid": 4748, "filename": "Mathis_js_1956.pdf", "mime_type": "application/pdf", "filesize": 6165164, "mtime": "2012-12-26 02:52:07", "url": "/2493/1/Mathis_js_1956.pdf" } ], "eprint_id": 2493, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Mathis_js_1956.pdf", "language": "en", "security": "public", "license": "other", "main": "Mathis_js_1956.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/21303" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21303" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21303" } ] } }, { "id": "/id/document/21303", "doc_id": 21303, "rev_number": 2, "files": [ { "id": "/id/file/27366", "fileid": 27366, "datasetid": "document", "objectid": 21303, "filename": "preview.png", "mime_type": "image/png", "hash": "acb71e677f0f80e146d8e10b0ff45195", "hash_type": "MD5", "filesize": 8478, "mtime": "2012-12-26 02:52:07", "url": "/2493/2/preview.png" } ], "eprint_id": 2493, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/4748" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4748" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4748" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/24/93", "datestamp": "2004-06-08", "lastmod": "2023-07-13 22:47:59", "status_changed": "2009-09-25 02:39:10", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mathis-John-Samuel", "name": { "family": "Mathis", "given": "John Samuel" }, "show_email": "NO" } ] }, "title": "The Abundance of Helium Relative to Hydrogen in the Orion Nebula", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nSpectrograms were taken at two slit positions in the brighest portion of the Orion Nebula near the exciting star [...] Ori C. Four independent measurements were made in each slit position of the ratios of the He I lines [...], and [...] to the hydrogen lines H , H , and H , respectively. The ratios of the [OIII] lines [...] and [...] and of the [OII] lines [...] and [...] were also determined. Reddening by interstellar absorption was taken into account.\r\n\r\nThe electron density was found from the [OII] lines to be 3,800 [...]. The electron temperature was found from the [OIII] lines to be 10,000[degrees]K. The theory of statistical equilibrium was developed for neutral helium, and from the three helium lines the ratio of abundances of helium and hydrogen was found to be 0.128 by number. All three lines gave results within nineteen per cent of the average in both slit positions.\r\n\r\nIt was found that the absorption of the line of He I at [...] in the spectrum of [...] Ori, C could take place in only .025 parsec under the most favorable conditions.\r\n\r\nIn order to estimate the lifetime of the [...] level in helium the probability of two-photon emission was estimated. The estimate was [...].", "date": "1956", "date_type": "degree", "id_number": "CaltechETD:etd-06072004-163340", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-06072004-163340", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-06-08", "doi": "10.7907/CB4D-4026", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Osterbrock-D-E", "name": { "family": "Osterbrock", "given": "Donald E." }, "role": "advisor" }, { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-06-07", "thesis_defense_date": "1956-01-01", "thesis_approved_date": "2004-06-08", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1956", "author_list": "Mathis, John Samuel" }, { "id": "/id/eprint/451", "eprint_id": 451, "rev_number": 10, "documents": [ { "id": "/id/document/687", "doc_id": 687, "rev_number": 2, "files": [ { "id": "/id/file/4301", "fileid": 4301, "datasetid": "document", "objectid": 687, "filename": "Stewart_jc_1955.pdf", "mime_type": "application/pdf", "filesize": 4814998, "mtime": "2012-12-26 02:29:53", "url": "/451/1/Stewart_jc_1955.pdf" } ], "eprint_id": 451, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Stewart_jc_1955.pdf", "language": "en", "security": "public", "license": "other", "main": "Stewart_jc_1955.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17503" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17503" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17503" } ] } }, { "id": "/id/document/17503", "doc_id": 17503, "rev_number": 2, "files": [ { "id": "/id/file/4299", "fileid": 4299, "datasetid": "document", "objectid": 17503, "filename": "preview.png", "mime_type": "image/png", "hash": "58c39b1ea3b2024f25f3ea96bdb4bbbf", "hash_type": "MD5", "filesize": 9446, "mtime": "2012-12-26 02:29:53", "url": "/451/2/preview.png" } ], "eprint_id": 451, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/687" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/687" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/687" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/04/51", "datestamp": "2004-02-04", "lastmod": "2023-07-10 19:34:11", "status_changed": "2009-09-25 01:37:50", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Stewart-John-Charles", "name": { "family": "Stewart", "given": "John Charles" }, "show_email": "NO" } ] }, "title": "A Quantitative Analysis of the Atmospheres of Three Peculiar Low-Luminosity B Stars", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in Plain ACII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nHigh-dispersion spectra of HD 37058, HD 37129 and HD 135485, three B stars exhibiting spectral peculiarities, have been studied on the basis of model atmospheres, with a view to detecting abundance anomalies. An approximate theory of high-temperature model atmospheres, applicable to stars in the range of spectral type B 1 - B7 and luminosity classes IV and V, has been developed and applied to the prediction of Balmer line profiles and total intensities of other lines. Temperatures, surface gravities and helium abundances of the three peculiar stars and two standard B stars, [...] Peg and [...] Scl, have been determined. The abundances of other elements have been found from curves of growth using theoretical line strengths. The values of surface gravity derived imply luminosities lower than those of the standard stars. The helium abundance derived for HD 135485 is remarkably large; a sizable titanium excess and an oxygen deficiency were detected in HD 37058.", "date": "1955", "date_type": "degree", "id_number": "CaltechETD:etd-02022004-095522", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-02022004-095522", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-02-04", "doi": "10.7907/DWVS-1E46", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-02-02", "thesis_defense_date": "1955-01-01", "thesis_approved_date": "2004-02-04", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1955", "author_list": "Stewart, John Charles" }, { "id": "/id/eprint/136", "eprint_id": 136, "rev_number": 9, "documents": [ { "id": "/id/document/207", "doc_id": 207, "rev_number": 2, "files": [ { "id": "/id/file/1314", "fileid": 1314, "datasetid": "document", "objectid": 207, "filename": "Parker_jm_1954.pdf", "mime_type": "application/pdf", "filesize": 5717498, "mtime": "2012-12-26 02:27:32", "url": "/136/1/Parker_jm_1954.pdf" } ], "eprint_id": 136, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Parker_jm_1954.pdf", "language": "en", "security": "public", "license": "other", "main": "Parker_jm_1954.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/17032" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17032" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17032" } ] } }, { "id": "/id/document/17032", "doc_id": 17032, "rev_number": 2, "files": [ { "id": "/id/file/1312", "fileid": 1312, "datasetid": "document", "objectid": 17032, "filename": "preview.png", "mime_type": "image/png", "hash": "3d5c37d1012e368e78ed29535a4a8857", "hash_type": "MD5", "filesize": 8805, "mtime": "2012-12-26 02:27:32", "url": "/136/2/preview.png" } ], "eprint_id": 136, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/207" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/207" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/207" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/01/36", "datestamp": "2004-01-12", "lastmod": "2023-06-13 21:50:07", "status_changed": "2009-09-25 01:29:22", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Parker-James-Mervin", "name": { "family": "Parker", "given": "James Mervin" }, "show_email": "NO" } ] }, "title": "Profiles and Wavelength of Spectrum Lines in the Solar Chromosphere", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nObservations have been made of the spectrum of the solar chromosphere outside of eclipse. The spectral region covered extends from [...] to [...] and from [...] to [...]. In addition, The O I triplet at [...] was photographed. In all, 1882 emission lines were photographed, and measured for wavelengths. Photographic intensity profiles were found for 530 of the lines, through the use of a microdensitometer. 330 of these lines were due to the Swan hands of C2. These lines were measured for total intensity, and a rotational temperature of 4600[degrees]K derived. The other 200 lines were reduced using the method of Voigt profiles. The width of the lines as a function of atomic weight was examined in the light of several assumptions, and it was found that the best interpretation was that of low temperature, of the order of 5000[degrees]K to 6000[degrees]K and an overlying turbulent motion which varies with height in the chromosphere. The interpretation of the line contours on this basis was performed using the model chromosphere due to van de Hulst.", "date": "1954", "date_type": "degree", "id_number": "CaltechETD:etd-01122004-160233", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-01122004-160233", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2004-01-12", "doi": "10.7907/GC46-VM62", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Nicholson-S-B", "name": { "family": "Nicholson", "given": "Seth B." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2004-01-12", "thesis_defense_date": "1954-01-01", "thesis_approved_date": "2004-01-12", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1954", "author_list": "Parker, James Mervin" }, { "id": "/id/eprint/1616", "eprint_id": 1616, "rev_number": 10, "documents": [ { "id": "/id/document/2542", "doc_id": 2542, "rev_number": 2, "files": [ { "id": "/id/file/15652", "fileid": 15652, "datasetid": "document", "objectid": 2542, "filename": "Arp_hc_1953.pdf", "mime_type": "application/pdf", "filesize": 6233362, "mtime": "2012-12-26 02:39:58", "url": "/1616/1/Arp_hc_1953.pdf" } ], "eprint_id": 1616, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Arp_hc_1953.pdf", "language": "en", "security": "public", "license": "other", "main": "Arp_hc_1953.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19282" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19282" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19282" } ] } }, { "id": "/id/document/19282", "doc_id": 19282, "rev_number": 2, "files": [ { "id": "/id/file/15650", "fileid": 15650, "datasetid": "document", "objectid": 19282, "filename": "preview.png", "mime_type": "image/png", "hash": "1e280c2c4fcf8541b694191f3dca3695", "hash_type": "MD5", "filesize": 10583, "mtime": "2012-12-26 02:39:57", "url": "/1616/2/preview.png" } ], "eprint_id": 1616, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2542" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2542" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2542" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/16/16", "datestamp": "2003-05-06", "lastmod": "2023-05-17 22:25:20", "status_changed": "2009-09-25 02:10:03", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arp-Halton-Christian", "name": { "family": "Arp", "given": "Halton Christian" }, "show_email": "NO" } ] }, "title": "Variable Stars with Periods Greater than One Day in Globular Clusters", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "Nineteen variable stars with periods greater than one day were observed in six globular clusters. The observational techniques and the accuracy of the measurements are discussed and light curves for 15 variables are exhibited.\r\n\r\nColor-magnitude diagrams for six clusters are presented and the distance modulus to each is derived.\r\n\r\nThe resulting period-luminosity relation for type II cepheids indicates there are actually three separate lines in the period-luminosity diagram which these variables occupy. Means of identifying stars on these different lines are presented. The factor of two in the period which these lines are from each other is discussed from the standpoint of the nature of cepheid variation. Finally a hypothesis is advanced to explain the connection between type I and type II cepheids.", "date": "1953", "date_type": "degree", "id_number": "CaltechETD:etd-05052003-160207", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05052003-160207", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-05-06", "doi": "10.7907/SMXJ-NH60", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Baade-Walter", "name": { "family": "Baade", "given": "Walter" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2003-05-05", "thesis_defense_date": "1953-01-01", "thesis_approved_date": "2003-05-06", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1953", "author_list": "Arp, Halton Christian" }, { "id": "/id/eprint/4199", "eprint_id": 4199, "rev_number": 13, "documents": [ { "id": "/id/document/6910", "doc_id": 6910, "rev_number": 2, "files": [ { "id": "/id/file/41980", "fileid": 41980, "datasetid": "document", "objectid": 6910, "filename": "Sandage_ar_1953.pdf", "mime_type": "application/pdf", "filesize": 8340575, "mtime": "2012-12-26 03:06:20", "url": "/4199/1/Sandage_ar_1953.pdf" } ], "eprint_id": 4199, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Sandage_ar_1953.pdf", "language": "en", "security": "public", "license": "other", "main": "Sandage_ar_1953.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23441" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23441" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23441" } ] } }, { "id": "/id/document/23441", "doc_id": 23441, "rev_number": 2, "files": [ { "id": "/id/file/41978", "fileid": 41978, "datasetid": "document", "objectid": 23441, "filename": "preview.png", "mime_type": "image/png", "hash": "963caaf69c6e711525f67dc46237b9d4", "hash_type": "MD5", "filesize": 8004, "mtime": "2012-12-26 03:06:20", "url": "/4199/2/preview.png" } ], "eprint_id": 4199, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6910" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6910" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6910" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/41/99", "datestamp": "2002-10-22", "lastmod": "2023-05-25 21:38:06", "status_changed": "2009-09-25 03:13:26", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sandage-Allan-Rex", "name": { "family": "Sandage", "given": "Allan Rex" }, "show_email": "NO" } ] }, "title": "A Study of the Globular Cluster M3", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Astronomy and Physics)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nThe color-magnitude diagram for the globular cluster M3 has been obtained to absolute magnitude M[subscript v] = +6. The main sequence has been found, extending from M[subscript v] = +3.5 to the limit of the data. The photometric parallax of m - M = 15.63 is found by fitting the apparent magnitude diagram to O. J. Eggen's and H. L. Johnson's diagram for stars in the solar neighborhood. The absolute magnitude of the cluster type variables in M3 is calibrated by this method. The value M[subscript v]= 0.0 for these stars is correct within [...]. This value is of significance for a decision on a new distance scale for the extragalactic nebulae in the observable universe.\r\n\r\nThe luminosity function is obtained to M[subscript v] = 6.8 for M3. From M[subscript Bol]= +2 to +4 a linear relation between log [...] (M) and M[subsript Bol] exists. The results of Chapter 3 show that this relation is expected if the sequences of the color-magnitude diagram are evolutionary in origin.\r\n\r\nApplication of a theory of evolution to the color magnitude diagram gives an age of 5 x 10[superscript 9] years since the formation of the main sequence in M3 and M92.\r\n\r\nFurther consequences of an evolutionary interpretation of the data are discussed in Chapter 3 and it is concluded that all evidence now available lends support to the evolutionary explanation of the sequences in the color-magnitude diagram.", "date": "1953", "date_type": "degree", "id_number": "CaltechETD:etd-10212002-160549", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10212002-160549", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2002-10-22", "doi": "10.7907/06G7-RG84", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Baade-Walter", "name": { "family": "Baade", "given": "Walter" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2002-10-21", "thesis_defense_date": "1953-04-01", "thesis_approved_date": "2002-10-22", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained and attached hereto a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1953", "author_list": "Sandage, Allan Rex" }, { "id": "/id/eprint/4348", "eprint_id": 4348, "rev_number": 11, "documents": [ { "id": "/id/document/7106", "doc_id": 7106, "rev_number": 2, "files": [ { "id": "/id/file/43289", "fileid": 43289, "datasetid": "document", "objectid": 7106, "filename": "Young_rd_1952.pdf", "mime_type": "application/pdf", "filesize": 76694667, "mtime": "2012-12-26 03:07:45", "url": "/4348/1/Young_rd_1952.pdf" } ], "eprint_id": 4348, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Young_rd_1952.pdf", "language": "en", "security": "public", "license": "other", "main": "Young_rd_1952.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/23635" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23635" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23635" } ] } }, { "id": "/id/document/23635", "doc_id": 23635, "rev_number": 2, "files": [ { "id": "/id/file/43287", "fileid": 43287, "datasetid": "document", "objectid": 23635, "filename": "preview.png", "mime_type": "image/png", "hash": "67af55888e281678796860b3a9bc09ef", "hash_type": "MD5", "filesize": 6725, "mtime": "2012-12-26 03:07:45", "url": "/4348/2/preview.png" } ], "eprint_id": 4348, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/7106" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7106" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7106" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/43/48", "datestamp": "2008-11-04", "lastmod": "2023-05-17 16:45:13", "status_changed": "2009-09-25 03:16:34", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Young-Richard Davidson", "name": { "family": "Young", "given": "Richard Davidson" }, "show_email": "NO" } ] }, "title": "The R-F Thermal Radiation from the Sun", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics and Electrical Engineering)", "abstract": "The thermal component of the radio frequency radiation from the sun is derived from the laws of classical physics.\r\n\r\nWith the \"velocity distribution\" method of the kinetic theory of gas the mean number of collisions per second between the particles is found. From this the absorption coefficient for the radiation is obtained. For the intensity of the emitted radiation the equation of transfer is solved in a three dimensional medium. In the solution the emissivity is eliminated by means of a modified form of Kirchhoff's law of radiation where the index of refraction is generalized to include absorption as well. For the path of the rays the equation of the iconal of geometrical optics is considered in a refracting and absorbing medium. The solution does not exhibit the phenomenon of total reflection, present in purely refracting media.\r\n\r\nNumerical calculations give the distribution of the radiation across the solar disk from 30 mc through 3000 mc. At 3000 mc the sun is of nearly uniform brightness with a sharply defined limb. At the lower frequencies a small central portion becomes quite bright and the limb less distinct and darker.", "date": "1952", "date_type": "degree", "id_number": "CaltechETD:etd-10312008-112710", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10312008-112710", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-11-04", "doi": "10.7907/7084-7319", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Epstein-P-S", "name": { "family": "Epstein", "given": "Paul Sophus" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-10-31", "thesis_defense_date": "1952-01-01", "thesis_approved_date": "2008-11-04", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "option_minor": { "items": [ "eleceng" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1952", "author_list": "Young, Richard Davidson" }, { "id": "/id/eprint/1551", "eprint_id": 1551, "rev_number": 27, "documents": [ { "id": "/id/document/84242", "doc_id": 84242, "rev_number": 2, "files": [ { "id": "/id/file/238950", "fileid": 238950, "datasetid": "document", "objectid": 84242, "filename": "abt-helmut-arthur-thesis-1952.pdf", "mime_type": "application/pdf", "hash": "59148e0a1c8efd2dc87c2e8b4a5b6fc1", "hash_type": "MD5", "filesize": 2553206, "mtime": "2017-11-27 23:20:38", "url": "/1551/3/abt-helmut-arthur-thesis-1952.pdf" } ], "eprint_id": 1551, "pos": 3, "placement": 3, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "abt-helmut-arthur-thesis-1952.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", 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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/84242" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/84242" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/84242" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/51", "datestamp": "2008-04-29", "lastmod": "2023-05-10 21:14:32", "status_changed": "2009-09-25 02:07:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abt-Helmut-Arthur", "name": { "family": "Abt", "given": "Helmut Arthur" }, "orcid": "0000-0002-4531-7867", "show_email": "NO" } ] }, "title": "An Analysis of the Variable Star, W Virginis", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astronomy; Physics", "abstract": "W Virginis is a 17-day variable star which is considered to be the prototype of population II Cepheids. An analysis of the physical conditions in W Virginis during its cyclic variations has been made from the following data: High dispersion (10 \u00c5/mm.) Coude plates were measured for radial velocities (by R. F. Sanford) and lines intensities which yielded curves of growth. Also used were a light curve in one color (Gordon and Kron) and colors (Whitford and Code).
\r\n\r\nThe observations indicate an expansion of about 36 x 106 km. and then a subsequent contraction. The first indication of a new expansion wave is the appearance of hydrogen emission lines, formed deep in the atmosphere. Later the outward-moving region of gas produces absorption lines like that of an F-type star. These gain in strength until maximum expansion. This is also a time of minimum electron pressure and nearly minimum temperature. During the contraction the electron pressure, temperature, and opacity rapidly increase. Also just after maximum expansion the appearance of a new set of hydrogen emission lines from deep in the atmosphere indicates the start of a new outward-moving wave. There is a time of several days during which absorption lines are seen from the two masses of gas: the one falling downward and the other moving upward. As the spectral features of the downward-moving region fade, those of the upward-moving region increase toward maximum strength. Data derived from the two simultaneous sets of absorption lines indicate very different conditions in the two regions.
\r\n\r\nIt was found that relative radii derived from light and color curves could not be compared with displacements derived from the radial velocity curve, because, perhaps, the regions predominantly forming the continuous and line spectra have different motions. The extremely red colors and the large apparent temperature gradient, both particularly at maximum expansion, may be due to the presence of an extended atmosphere.
", "date": "1952", "date_type": "degree", "id_number": "CaltechETD:etd-04292008-114242", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04292008-114242", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-04-29", "doi": "10.7907/R3P7-KJ13", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Greenstein-J-L", "name": { "family": "Greenstein", "given": "Jesse L." }, "role": "chair" }, { "id": "Baade-W", "name": { "family": "Baade", "given": "Walter" }, "role": "member" }, { "id": "Fowler-W-A", "name": { "family": "Fowler", "given": "William A." }, "role": "member" }, { "id": "King-R-B", "name": { "family": "King", "given": "Robert Burnett" }, "role": "member" }, { "id": "M\u00fcnch-G", "name": { "family": "M\u00fcnch", "given": "Guido" }, "role": "member" }, { "id": "Wilson-O-C", "name": { "family": "Wilson", "given": "O. C." }, "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-04-29", "thesis_defense_date": "1952-01-01", "thesis_approved_date": "2008-04-29", "review_status": "approved", "option_major": { "items": [ "astronomy" ] }, "option_minor": { "items": [ "physics" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1952", "author_list": "Abt, Helmut Arthur" }, { "id": "/id/eprint/1587", "eprint_id": 1587, "rev_number": 11, "documents": [ { "id": "/id/document/2469", "doc_id": 2469, "rev_number": 2, "files": [ { "id": "/id/file/15254", "fileid": 15254, "datasetid": "document", "objectid": 2469, "filename": "Hill_aj_1950.pdf", "mime_type": "application/pdf", "filesize": 5941303, "mtime": "2012-12-26 02:39:34", "url": "/1587/1/Hill_aj_1950.pdf" } ], "eprint_id": 1587, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Hill_aj_1950.pdf", "language": "en", "security": "public", "license": "other", "main": "Hill_aj_1950.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/19209" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19209" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19209" } ] } }, { "id": "/id/document/19209", "doc_id": 19209, "rev_number": 2, "files": [ { "id": "/id/file/15252", "fileid": 15252, "datasetid": "document", "objectid": 19209, "filename": "preview.png", "mime_type": "image/png", "hash": "bf1b4816e125895c26db76af518f73be", "hash_type": "MD5", "filesize": 8430, "mtime": "2012-12-26 02:39:34", "url": "/1587/2/preview.png" } ], "eprint_id": 1587, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2469" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2469" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2469" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/15/87", "datestamp": "2008-05-16", "lastmod": "2023-03-31 18:37:14", "status_changed": "2009-09-25 02:08:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hill-Armin-John", "name": { "family": "Hill", "given": "Armin John" }, "show_email": "NO" } ] }, "title": "Relative f-Values of Selected lines in the Absorption Spectrum of Chromium I", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics and Astronomy)", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nRelative f- and gf-values for 410 lines in the spectrum of neutral chromium have been measured in electric furnace absorption spectra by the method developed by R. B. King for obtaining relative gf-values from the equivalent widths of weak absorption lines. Most of the transitions having lower excitation potentials less than 3.00 volts, in the wave length region [...] 3800 - 5500 have been measured. Some lines from terms as high as 3.45 volts are included, though most of these were too weak to permit accurate determination of their gf-values.\r\n\r\nSome information was obtained on three lines which have not as yet been classified, and is included with the hope that it may prove of assistance in the classification of these lines.\r\n\r\nWave lengths were found for two lines which did not agree with those which had previously been assigned. These were measured with reference to known lines and corrected values are suggested.\r\n\r\nThe methods used in these measurements are described in some detail and suggestions for improvement made. Sources of error are discussed and the measures taken to reduce error from these sources are described.", "date": "1950", "date_type": "degree", "id_number": "CaltechETD:etd-05022008-161551", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05022008-161551", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2008-05-16", "doi": "10.7907/16GH-E254", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "King-R-B", "name": { "family": "King", "given": "Robert Burnett" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2008-05-02", "thesis_defense_date": "1950-01-01", "thesis_approved_date": "2008-05-16", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "option_minor": { "items": [ "astronomy" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1950", "author_list": "Hill, Armin John" }, { "id": "/id/eprint/3465", "eprint_id": 3465, "rev_number": 12, "documents": [ { "id": "/id/document/6008", "doc_id": 6008, "rev_number": 2, "files": [ { "id": "/id/file/35813", "fileid": 35813, "datasetid": "document", "objectid": 6008, "filename": "Johnson_jj_1935.pdf", "mime_type": "application/pdf", "filesize": 2713490, "mtime": "2012-12-26 03:00:09", "url": "/3465/1/Johnson_jj_1935.pdf" } ], "eprint_id": 3465, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Johnson_jj_1935.pdf", "language": "en", "security": "public", "license": "other", "main": "Johnson_jj_1935.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final", "relation": { "items": [ { "type": "http://eprints.org/relation/hasVolatileVersion", "uri": "/id/document/22548" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22548" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22548" } ] } }, { "id": "/id/document/22548", "doc_id": 22548, "rev_number": 2, "files": [ { "id": "/id/file/35811", "fileid": 35811, "datasetid": "document", "objectid": 22548, "filename": "preview.png", "mime_type": "image/png", "hash": "c43cc784ca019f35fcb7eef5ec504e2e", "hash_type": "MD5", "filesize": 7613, "mtime": "2012-12-26 03:00:09", "url": "/3465/2/preview.png" } ], "eprint_id": 3465, "pos": 2, "placement": 2, "mime_type": "image/png", "format": "image/png", "language": "en", "security": "public", "license": "other", "main": "preview.png", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/6008" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6008" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6008" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/34/65", "datestamp": "2007-09-17", "lastmod": "2019-10-03 23:26:46", "status_changed": "2009-09-25 02:58:52", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Johnson-Josef-Jerome", "name": { "family": "Johnson", "given": "Josef Jerome" }, "show_email": "NO" } ] }, "title": "Visual Measurements of the Polarization of the Solar Corona", "ispublished": "unpub", "full_text_status": "public", "keywords": "Astrophysics", "abstract": "Visual polarization measurements were made at the eclipse of February 14, 1934, with a modified Lyot-type polarimeter attached to a four-inch equatorially-mounted refractor. The objective was stopped down to 1 1/2 inches to reduce polarization effects the instrument. Distances from the moon's limb were measured by means of a cross-wire reticle in the focal plane of the eyepiece.
\r\n\r\nFive different points of the corona were investigated, all lying directly off the east limb of the sun and ranging in distance from the limb from 1 to 8.5 minutes of arc. The observed polarization rose rapidly from 17% at 1' to 26% at 4', remaining sensibly constant from 4' outward.
\r\n\r\nThese values are considerably higher than those previously obtained by visual methods, but are lower than the values obtained photographically. Subject to confirmation at a future eclipse, these values will constitute important evidence in favor of Schwarzschild's theory that a large part of the light of the corona is due to the scattering of photospheric light by free electrons.
", "date": "1935", "date_type": "degree", "id_number": "CaltechETD:etd-09112007-075222", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09112007-075222", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Astronomy Department" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-09-17", "doi": "10.7907/FBFH-ER25", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Anderson-J-A", "name": { "family": "Anderson", "given": "John A." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-09-11", "thesis_defense_date": "1935-01-01", "thesis_approved_date": "2007-09-17", "review_status": "approved", "option_major": { "items": [ "astrophys" ] }, "copyright_statement": "I hereby certify that, if appropriate, I have obtained a written permission statement from the owner(s) of each third party copyrighted matter to be included in my thesis, dissertation, or project report, allowing distribution as specified below. I certify that the version I submitted is the same as that approved by my advisory committee.\n\nI hereby grant to California Institute of Technology or its agents the non-exclusive\nlicense to archive and make accessible, under the conditions specified below,\nmy thesis, dissertation, or project report in whole or in part in all forms of media, now or hereafter known. I retain all other ownership rights to the copyright of the thesis, dissertation or project report. I also retain the right to use in future works (such as articles or books) all or part of this thesis, dissertation, or project report.", "pub_year": "1935", "author_list": "Johnson, Josef Jerome" } ]