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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"thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "jsrankin@princeton.edu", "id": "Rankin-Jamie-Sue", "name": { "family": "Rankin", "given": "Jamie Sue" }, "orcid": "0000-0002-8111-1444", "show_email": "NO" } ] }, "title": "Voyager 1 Observations of Galactic Cosmic Ray Anisotropies in the Local Interstellar Medium", "ispublished": "unpub", "full_text_status": "public", "keywords": "Voyager 1; Voyager Mission; interstellar medium; galactic cosmic rays; solar physics; Cosmic Ray Subsystem; heliophysics; astro-particle physics; sun; interstellar space", "abstract": "Since crossing the heliopause on August 25, 2012, Voyager 1 has observed reductions in galactic cosmic ray counting rates caused by a time-varying depletion of particles with pitch angles near 90-deg, while intensities of particles with other pitch angles remain unchanged. Between late 2012 and mid-2017, three large-scale, durable events occurred, lasting roughly 100 to 630 days. Omnidirectional and directional data from the Cosmic Ray Subsystem's high energy telescopes are used to report observations of the cosmic ray intensity variations. Omnidirectional (>20 MeV) proton-dominated measurements show up to a ~3.8% intensity reduction. Bi-directional (>70 MeV) and unidirectional (~18 to ~70 MeV) proton-dominated measurements are analyzed using data taken from various spacecraft orientations, including during magnetometer roll calibrations and 70-deg-offset maneuvers. The anisotropy is characterized as a \"notch\" in an otherwise uniform pitch-angle distribution of varying depth and width centered about 90-deg in pitch angle space. The notch averages ~22-deg wide and ~15% deep -- signifying a depletion region that is broad and shallow. However, electron observations reveal that there is only a weak, at most, evidence of pitch angle anisotropy in cosmic-ray electrons with energies of ~3 to ~105 MeV, indicating that the generation of the notch or its evolution differs between electrons and protons, or varies with rigidity. There are indications that the anisotropy is formed by a combination of magnetic trapping and adiabatic cooling in associated shocks or compression regions.\r\n", "date": "2019", "date_type": "degree", "id_number": "CaltechTHESIS:09022018-124448728", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09022018-124448728", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNN12AA01C" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Jamie Rankin", "deposited_on": "2018-09-06 22:27:35", "doi": "10.7907/WX3S-1D86", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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": "gh@astro.caltech.edu", "id": "Hallinan-G-W", "name": { "family": "Hallinan", "given": "Gregg W." }, "orcid": "0000-0002-7083-4049", "role": "member" }, { "email": "phopkins@caltech.edu", "id": "Hopkins-P-F", "name": { "family": "Hopkins", "given": "Philip F." }, "orcid": "0000-0003-3729-1684", "role": "member" }, { "email": "rbpatter@caltech.edu", "id": "Patterson-R-B", "name": { "family": "Patterson", "given": "Ryan B." }, "orcid": "0000-0002-5787-9517", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "2018-08-23", "gradofc_approval_date": "2018-09-06", "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": "2019", "author_list": "Rankin, Jamie Sue" }, { "id": "/id/eprint/10294", "eprint_id": 10294, "rev_number": 28, "documents": [ { "id": "/id/document/80696", "doc_id": 80696, "rev_number": 3, "files": [ { "id": "/id/file/227795", "fileid": 227795, "datasetid": "document", "objectid": 80696, "filename": "Balokovic Doctoral Thesis 6-Month Embargo Request for Mislav Balokovic - Google Groups.pdf", "mime_type": "application/pdf", "hash": "827a6de38ee68acc51d912bbc6082de9", "hash_type": "MD5", "filesize": 68791, "mtime": "2017-06-06 18:51:14", "url": "/10294/7/Balokovic Doctoral Thesis 6-Month Embargo Request for Mislav Balokovic - Google Groups.pdf" } ], "eprint_id": 10294, "pos": 7, "placement": 7, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "author 6-month embargo 6/6/2017", "language": "en", "security": 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"0", "media_sample_stop": "0", "relation": { "items": [ { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/80732" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/80732" }, { "type": "http://eprints.org/relation/issmallThumbnailVersionOf", "uri": "/id/document/80732" } ] } } ], "eprint_status": "archive", "userid": 10848, "dir": "disk0/00/01/02/94", "datestamp": "2017-06-07 17:34:01", "lastmod": "2021-11-05 22:43:59", "status_changed": "2017-06-07 17:34:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mislav.balokovic@gmail.com", "id": "Balokovic-Mislav", "name": { "family": "Balokovic", "given": "Mislav" }, "orcid": "0000-0003-0476-6647", "show_email": "NO" } ] }, "title": "Unveiling the Structure of Active Galactic Nuclei with Hard X-ray Spectroscopy", "ispublished": "unpub", "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. I also retain 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": "Balokovic, Mislav" }, { "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/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/159093", "doc_id": 159093, "rev_number": 1, "files": [ { "id": "/id/file/456608", "fileid": 456608, "datasetid": "document", "objectid": 159093, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "767bc482481493850ce778f6087b2865", "hash_type": "MD5", "filesize": 42382, "mtime": "2024-10-10 18:28:16", "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/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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"uri": "/id/document/18923" } ] } }, { "id": "/id/document/15766", "doc_id": 15766, "rev_number": 3, "files": [ { "id": "/id/file/201334", "fileid": 201334, "datasetid": "document", "objectid": 15766, "filename": "Chen_Chi_Ming_Hubert_2008.PDF", "mime_type": "application/pdf", "filesize": 44133, "mtime": "2016-08-22 21:14:52", "url": "/1428/4/Chen_Chi_Ming_Hubert_2008.PDF" } ], "eprint_id": 1428, "pos": 4, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Chen_Chi_Ming_Hubert_2008.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/18923", "doc_id": 18923, "rev_number": 2, "files": [ { "id": "/id/file/13525", "fileid": 13525, "datasetid": "document", "objectid": 18923, "filename": "preview.png", "mime_type": "image/png", "hash": "1e7b51a7c6c48390264582ae6add2b88", "hash_type": "MD5", "filesize": 16254, "mtime": "2012-12-26 02:38:00", "url": "/1428/5/preview.png" } ], "eprint_id": 1428, "pos": 5, "placement": 5, "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/2167" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2167" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2167" } ] } }, { "id": "/id/document/156657", "doc_id": 156657, "rev_number": 1, "files": [ { "id": "/id/file/454164", "fileid": 454164, "datasetid": "document", "objectid": 156657, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "b3f121582a14318cb58799e00d45cf1c", "hash_type": "MD5", "filesize": 46679, "mtime": "2024-10-10 17:42:29", "url": "/1428/6/indexcodes.txt" } ], "eprint_id": 1428, "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/2167" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/2167" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/2167" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/14/28", "datestamp": "2008-05-20", "lastmod": "2020-03-10 19:28:43", "status_changed": "2009-09-25 02:03:49", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "hubert@srl.caltech.edu", "id": "Chen-Chi-Ming-Hubert", "name": { "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/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/158950", "doc_id": 158950, "rev_number": 1, "files": [ { "id": "/id/file/456465", "fileid": 456465, "datasetid": "document", "objectid": 158950, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "81c56ab2ac3bfa4a848dcb26709fcfde", "hash_type": "MD5", "filesize": 53207, "mtime": "2024-10-10 18:23:48", "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/559", "eprint_id": 559, "rev_number": 15, "documents": [ { "id": "/id/document/818", "doc_id": 818, "rev_number": 2, "files": [ { "id": "/id/file/5211", "fileid": 5211, "datasetid": "document", "objectid": 818, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 9853721, "mtime": "2012-12-26 02:30:31", "url": "/559/1/thesis.pdf" } ], "eprint_id": 559, "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/17633" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/17633" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/17633" } ] } }, { "id": "/id/document/16340", "doc_id": 16340, "rev_number": 3, "files": [ { "id": "/id/file/200244", "fileid": 200244, "datasetid": "document", "objectid": 16340, "filename": "Ogliore_Ryan_Christopher_2007.PDF", "mime_type": "application/pdf", "filesize": 41689, "mtime": "2016-08-22 21:14:10", "url": "/559/2/Ogliore_Ryan_Christopher_2007.PDF" } ], "eprint_id": 559, "pos": 2, "format": "application/pdf", "language": "en", "security": "internal", "license": "other", "main": "Ogliore_Ryan_Christopher_2007.PDF", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "approvalform" }, { "id": "/id/document/17633", "doc_id": 17633, "rev_number": 2, "files": [ { "id": "/id/file/5209", "fileid": 5209, "datasetid": "document", "objectid": 17633, "filename": "preview.png", "mime_type": "image/png", "hash": "f9ac983853359ce9140c912d4f33136d", "hash_type": "MD5", "filesize": 17165, "mtime": "2012-12-26 02:30:30", "url": "/559/3/preview.png" } ], "eprint_id": 559, "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/818" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/818" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/818" } ] } }, { "id": "/id/document/155885", "doc_id": 155885, "rev_number": 1, "files": [ { "id": "/id/file/453392", "fileid": 453392, "datasetid": "document", "objectid": 155885, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "b4546dd466c9443651df0617e27f1c71", "hash_type": "MD5", "filesize": 13924, "mtime": "2024-10-10 17:24:44", "url": "/559/4/indexcodes.txt" } ], "eprint_id": 559, "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/818" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/818" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/818" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/05/59", "datestamp": "2007-02-12", "lastmod": "2024-06-24 20:21:20", "status_changed": "2009-09-25 01:40:14", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "ogliore@gmail.com", "id": "Ogliore-Ryan-Christopher", "name": { "family": "Ogliore", "given": "Ryan Christopher" }, "orcid": "0000-0001-8165-6252", "show_email": "YES" } ] }, "title": "The Sulfur, Argon, and Calcium Isotopic Composition of the Galactic Cosmic Ray Source", "ispublished": "unpub", "full_text_status": "public", "keywords": "astrophysics; cosmic rays", "abstract": "Galactic cosmic ray measurements of the sulfur, argon, and calcium isotopes made by the Cosmic Ray Isotope Spectrometer on the NASA Advanced Composition Explorer are reported over the energy range from 100 to 400 MeV/nucleon. The propagation of cosmic rays through the Galaxy and heliosphere is modeled with observational constraints imposed by measurements. Source abundance ratios of the sulfur, argon, and calcium isotopes are deduced from this model. Cosmic rays are thought to originate in the cores of superbubbles which contain stellar ejecta mixed with the surrounding interstellar medium. The composition of the superbubble core should reflect the composition of the cosmic rays at their source. Based on the derived isotopic source ratios of sulfur, argon, and calcium, the superbubble material at the cosmic ray source is constrained to be 18%+26%-14% supernova and wind ejecta, with the remainder interstellar medium material. This mix of metal-rich ejecta and interstellar medium in the superbubble core corresponds to a cosmic ray source metallicity of 2.7+3.9-2.1 times solar metallicity.", "date": "2007", "date_type": "degree", "id_number": "CaltechETD:etd-02082007-175902", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-02082007-175902", "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" ] }, "suggestions": "ROGLIORE@WUSTL.EDU", "deposited_by": "Imported from ETD-db", "deposited_on": "2007-02-12", "doi": "10.7907/ZKDE-TE09", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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": "ajw@caltech.edu", "id": "Weinstein-Alan-J-Physics", "name": { "family": "Weinstein", "given": "Alan Jay" }, "orcid": "0000-0002-0928-6784", "role": "member" }, { "email": "jimh@lobach.jsd.claremont.edu", "id": "Higdon-James", "name": { "family": "Higdon", "given": "James" }, "orcid": "0009-0000-1441-2872", "role": "member" }, { "email": "bmck@caltech.edu", "id": "McKeown-R-D", "name": { "family": "McKeown", "given": "Robert D." }, "role": "member" }, { "email": "rmewaldt@srl.caltech.edu", "id": "Mewaldt-R-A", "name": { "family": "Mewaldt", "given": "Richard A." }, "orcid": "0000-0003-2178-9111", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-02-08", "thesis_defense_date": "2006-12-18", "thesis_approved_date": "2007-02-12", "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": "Ogliore, Ryan Christopher" }, { "id": "/id/eprint/3760", "eprint_id": 3760, "rev_number": 12, "documents": [ { "id": "/id/document/6384", "doc_id": 6384, "rev_number": 3, "files": [ { "id": "/id/file/38329", "fileid": 38329, "datasetid": "document", "objectid": 6384, "filename": "thesis.pdf", "mime_type": "application/pdf", "filesize": 2559790, "mtime": "2012-12-26 03:02:45", "url": "/3760/1/thesis.pdf" } ], "eprint_id": 3760, "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/22922" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/22922" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/22922" } ] } }, { "id": "/id/document/16690", "doc_id": 16690, "rev_number": 3, "files": [ { "id": "/id/file/204152", "fileid": 204152, "datasetid": "document", "objectid": 16690, "filename": "Yost_Sarah_Anne_2004.txt", "mime_type": "text/plain", "filesize": 1857, "mtime": "2016-08-22 21:16:56", "url": "/3760/2/Yost_Sarah_Anne_2004.txt" } ], "eprint_id": 3760, "pos": 2, "format": "text/plain", "language": "en", "security": "internal", "license": "other", "main": "Yost_Sarah_Anne_2004.txt", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/22922", "doc_id": 22922, "rev_number": 2, "files": [ { "id": "/id/file/38327", "fileid": 38327, "datasetid": "document", "objectid": 22922, "filename": "preview.png", "mime_type": 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"indexcodes.txt", "mime_type": "text/plain", "hash": "2e6fd1fe93b3e784ce5c75df7ad1aa08", "hash_type": "MD5", "filesize": 788, "mtime": "2024-10-10 18:47:02", "url": "/3760/5/indexcodes.txt" } ], "eprint_id": 3760, "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/16690" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/16690" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/16690" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/37/60", "datestamp": "2003-09-29", "lastmod": "2021-01-22 01:47:24", "status_changed": "2009-09-25 03:04:55", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "syost@csbsju.edu", "id": "Yost-Sarah-Anne", "name": { "family": "Yost", "given": "Sarah Anne" }, "show_email": "NO" } ] }, "title": "Gamma-Ray Burst Afterglows: Constraining Physical Parameters and Fireball Model Assumptions", "ispublished": "unpub", "full_text_status": "public", "keywords": "fireball model; gamma-ray bursts", "abstract": "Gamma-ray bursts (GRBs) are the most luminous events in the high-energy sky. Occurring at cosmological distances, they are cataclysmic events presumed to be associated with the endpoints of massive stars' lives. They are produced by relativistic ejecta. As the ejecta encounters the surrounding medium it slows and emits lower-energy emission known as the GRB afterglow. The evolution of the shock in this phase depends upon the medium encountered as well as on such basic parameters of the event as energy and collimation. Afterglow studies can shed light upon the physics of relativistic shocks and the GRB environment(s), providing indirect clues to the progenitors. These parameters can be determined by fitting afterglow data sets to a model of the event, here, the fireball model. If the model assumptions are correct, the parameters providing a good fit will correspond to those of the event.
\r\n\r\nWe develop a fireball model starting from its analytic, asymptotic behaviour parameterized by its fundamental parameters (energy, collimation, density, and microphysics). We find good fits to four of the best-sampled broadband afterglow data sets, with simple assumptions concerning the unknown microphysics and circumburst density profile. We present the resulting fit parameters, showing reasonable energies, densities similar to those of diffuse clouds, and a large spread in such microphysical parameters as the fraction of shock energy used to generate magnetic fields.
\r\n\r\nWe also present results where the model fit showed degeneracies and other data sets that are not well-fit by this model. Motivated to determine the model's inherent uncertainty from the adoption of physical assumption, we consider some changes to these. We present our results: that a range of magnetic energy fraction variation with shock strength is permissible, and that afterglow fits are not sensitive to steeply rising circumburst power law density profiles. We demonstrate that the fitted parameters change when the assumptions are changed; this may be by a small fraction, or up to an order of magnitude.
", "date": "2004", "date_type": "degree", "id_number": "CaltechETD:etd-09252003-152937", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-09252003-152937", "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" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2003-09-29", "doi": "10.7907/FHCW-2P04", "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": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "role": "member" }, { "email": "sari@tapir.caltech.edu", "id": "Sari-R", "name": { "family": "Sari", "given": "Re'em" }, "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": "2003-09-25", "thesis_defense_date": "2003-08-31", "thesis_approved_date": "2003-09-29", "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": "2004", "author_list": "Yost, Sarah Anne" }, { "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/159004", "doc_id": 159004, "rev_number": 1, "files": [ { "id": "/id/file/456519", "fileid": 456519, "datasetid": "document", "objectid": 159004, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "695ccbc708705f1af9f0b6f4a6f05965", "hash_type": "MD5", "filesize": 27389, "mtime": "2024-10-10 18:25:46", "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/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/159458", "doc_id": 159458, "rev_number": 1, "files": [ { "id": "/id/file/456973", "fileid": 456973, "datasetid": "document", "objectid": 159458, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "616c0cab16be01415660d6b685cb8beb", "hash_type": "MD5", "filesize": 920, "mtime": "2024-10-10 18:37:48", "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/4192", "eprint_id": 4192, "rev_number": 10, "documents": [ { "id": "/id/document/6903", "doc_id": 6903, "rev_number": 3, "files": [ { "id": "/id/file/41929", "fileid": 41929, "datasetid": "document", "objectid": 6903, "filename": "Williams_dl_1998.pdf", "mime_type": "application/pdf", "filesize": 13979902, "mtime": "2012-12-26 03:06:18", "url": "/4192/1/Williams_dl_1998.pdf" } ], "eprint_id": 4192, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Williams_dl_1998.pdf", "language": "en", "security": "public", "license": "other", "main": "Williams_dl_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/23434" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23434" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23434" } ] } }, { "id": "/id/document/23434", "doc_id": 23434, "rev_number": 3, "files": [ { "id": "/id/file/41927", "fileid": 41927, "datasetid": "document", "objectid": 23434, "filename": "preview.png", "mime_type": "image/png", "hash": "e2070064d7d5f87873b9373941e10721", "hash_type": "MD5", "filesize": 16086, "mtime": "2012-12-26 03:06:18", "url": "/4192/2/preview.png" } ], "eprint_id": 4192, "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/6903" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/6903" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/6903" } ] } }, { "id": "/id/document/59908", "doc_id": 59908, "rev_number": 3, "files": [ { "id": "/id/file/167859", "fileid": 167859, "datasetid": "document", "objectid": 59908, "filename": "Williams_dl_1998.docx", "mime_type": "application/vnd.openxmlformats-officedocument.wordprocessingml.document", "hash": "215ce9f25e809bf336759e934bb03dbc", "hash_type": "MD5", "filesize": 12182, "mtime": "2015-07-06 15:10:06", "url": "/4192/3/Williams_dl_1998.docx" } ], "eprint_id": 4192, "pos": 3, "placement": 3, "mime_type": "application/vnd.openxmlformats-officedocument.wordprocessingml.document", "format": "other", "format_desc": "Author OK 07/06/2015", "language": "en", "security": "internal", "license": "other", "main": "Williams_dl_1998.docx", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "release" }, { "id": "/id/document/160014", "doc_id": 160014, "rev_number": 1, "files": [ { "id": "/id/file/457529", "fileid": 457529, "datasetid": "document", "objectid": 160014, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "33b14d39f0ece17b2a54b697e9706cab", "hash_type": "MD5", "filesize": 557, "mtime": "2024-10-10 18:54:03", "url": "/4192/4/indexcodes.txt" } ], "eprint_id": 4192, "pos": 4, "placement": 4, "mime_type": "text/plain", "format": "other", "format_desc": "Generate index codes conversion from other 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/59908" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/59908" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/59908" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/41/92", "datestamp": "2005-10-20", "lastmod": "2019-12-21 04:50:14", "status_changed": "2009-09-25 03:13:17", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "dlwiii@gmail.com", "id": "Williams-D-L", "name": { "family": "Williams", "given": "Daniel LeRoy" }, "show_email": "YES" } ] }, "title": "Measurements of the isotopic composition of solar energetic particles with the MAST instrument aboard the SAMPEX spacecraft", "ispublished": "unpub", "full_text_status": "public", "keywords": "SAMPEX MAST Solar Isotopic Composition Isotope Neon", "abstract": "NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.\r\n\r\nWe report measurements of the isotopic composition of solar energetic particles (SEP) as observed in two gradual solar energetic particle events which began on 30 October and 2 November of 1992. These measurements were taken by the Mass Spectrometer Telescope (MAST), a charged-particle telescope on board the SAMPEX satellite in a polar, low-Earth orbit. The elements measured are carbon, nitrogen, oxygen, neon, magnesium and silicon, which are observed over an energy interval of ~15 to 70 MeV per nucleon. These are the first isotopic measurements of silicon, and only the second measurements of the other elements in individual SEP events.\r\n\r\nSAMPEX has access to interplanetary fluxes of energetic particles during the high latitude portions of its orbit. This access depends on the rigidity of the particles and therefore on their charge to mass ratio. Fortunately, the polar orbit of SAMPEX allows measurement of SEP charge states using the geomagnetic filtering technique, and a previous study reported measurements of the ionic charge states in the same two SEP events studied in this work. This was the first time that charge states of SEPs at these high energies have been measured, and it allows rigidity-dependent biases in the elemental and isotopic composition to be investigated in the present study. This is particularly important since acceleration/transport processes depend on rigidity, and because the observed composition is also affected by the Earth's magnetic field.\r\n\r\nThe MAST instrument measures both elemental and isotopic composition using the [...] technique, which resulted in a typical mass resolution of ~0.24 amu. It was found that during times of high counting rates, the measured mass distributions exhibited high-mass tails. Through computer simulation of the instrument and its particle environment, it was found that these tails are caused by [...] MeV protons which hit the instrument hodoscope in coincidence with the heavy ions of interest. By choosing only data which occurred during periods of low to moderate counting rates, the probability of such coincidences could be reduced, and these tails could be effectively removed. The elemental composition was used to find and correct for the bias introduced by these restrictions.\r\n\r\nThe energy spectra of the elements in each SEP event could be fit with exponentials in energy per nucleon, with a single, characteristic e-folding energy for each event. Such well-behaved spectra allowed elemental abundances to be calculated. These abundances exhibited a fractionation due to acceleration and propagation of the SEP source material, which could be ordered as a function of the charge to mass ratio of each element. The SEP source abundances exhibited a depletion of elements with a high first-ionization potential as compared to the composition of the solar photosphere, a phenomena which has been well-observed in SEP composition for many years. The depletion factor varied by a factor of ~2 between the two SEP events.\r\n\r\nThe isotopic ratios of [...], [...], [...], [...] and [...] were found to be in generally good agreement with the solar system values of isotopic composition as tabulated by Anders and Grevesse (1989) based on terrestrial and meteoritic measurements. Earlier measurements of SEP isotopes found a [...] ratio which was ~80% higher than the [...] ratio measured in the solar wind, but close to the neon-A component found in meteorites, which had been adopted as the solar system standard by Cameron (1982). Our measurements of [...], however, are consistent with the [...] ratio found in the solar wind. This leads us to conclude that the underlying isotopic composition of the SEP source material is closer to that of the solar wind.\r\n\r\nThere are only two cases in which the measured isotope ratios differ significantly from the Anders and Grevesse (1989) values, the [...] and the [...] ratio in the second SEP event, both of which are a factor of ~2 higher than the solar system value. There is no apparent pattern to these overabundances.\r\n\r\nWhile the isotopic ratios measured in the two SEP events generally support the assumption that SEPs and solar wind come from the same reservoir of material, and that SEP composition is consistent with the standard solar system abundances compiled by Anders and Grevesse (1989), SEP isotope measurements are still at an exploratory stage. The limited number of observations prevent us from making definite conclusions about the nature of event-to-event variations in SEP isotopic composition, or about possible differences between the coronal and solar system abundances.\r\n", "date": "1998", "date_type": "degree", "id_number": "CaltechETD:etd-10202005-144209", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10202005-144209", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-10-20", "doi": "10.7907/P5H0-EB69", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Mewaldt-R", "name": { "family": "Mewaldt", "given": "Richard" }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "role": "chair" }, { "id": "Zirin-H", "name": { "family": "Zirin", "given": "Harold" }, "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": "2005-10-20", "thesis_defense_date": "1998-04-30", "thesis_approved_date": "2005-10-20", "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": "Williams, Daniel LeRoy" }, { "id": "/id/eprint/8666", "eprint_id": 8666, "rev_number": 37, "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": 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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." }, "orcid": "0000-0002-8850-3627", "role": "advisor" }, { "email": "rmewaldt@caltech.edu", "id": "Mewaldt-R", "name": { "family": "Mewaldt", "given": "Richard" }, "orcid": "0000-0003-2178-9111", "role": "advisor" }, { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "prince@caltech.edu", "id": "Prince-T-A", "name": { "family": "Prince", "given": "Thomas A." }, "orcid": "0000-0002-8850-3627", "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." }, "orcid": "0000-0003-2178-9111", "role": "member" }, { "email": "newman@hep.caltech.edu", "id": "Newman-H-B", "name": { "family": "Newman", "given": "Harvey B." }, "orcid": "0000-0003-0964-1480", "role": "member" }, { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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/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": { 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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/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/7666", "eprint_id": 7666, "rev_number": 17, "documents": [ { "id": "/id/document/37964", "doc_id": 37964, "rev_number": 3, "files": [ { "id": "/id/file/117812", "fileid": 117812, "datasetid": "document", "objectid": 37964, "filename": "Heindl_wa_1994.pdf", "mime_type": "application/pdf", "hash": "09f58ac4199ed267baf8f9ee5db3a9db", "hash_type": "MD5", "filesize": 27058796, "mtime": "2013-05-07 15:53:35", "url": "/7666/1/Heindl_wa_1994.pdf" } ], "eprint_id": 7666, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Heindl_wa_1994.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": "disk0/00/00/76/66", "datestamp": "2013-05-07 16:19:17", "lastmod": "2022-11-09 19:19:59", "status_changed": "2013-05-07 16:19:17", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Heindl-W-A", "name": { "family": "Heindl", "given": "William Adams" }, "show_email": "NO" } ] }, "title": "Multiwavelength observations of the black hole candidate 1E 1740.7-2942", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics ", "abstract": "Observations of the Galactic center region black hole candidate\r\n1E 1740.7-2942 have been carried out using the Caltech Gamma-Ray Imaging Payload\r\n(GRIP), the R\u00f6ntgensatellit (ROSAT) and the Very Large Array (VLA). These\r\nmultiwavelength observations have helped to establish the association between a\r\nbright emitter of hard X-rays and soft \u03b3-rays, the compact core of a double radio jet\r\nsource, and the X-ray source, 1E 1740.7-2942. They have also provided information\r\non the X-ray and hard X-ray spectrum.
\r\n\r\nThe Galactic center region was observed by GRIP during balloon flights from\r\nAlice Springs, NT, Australia on 1988 April 12 and 1989 April 3. These observations\r\nrevealed that 1E 1740.7-2942 was the strongest source of hard X-rays within ~10\u00b0\r\nof the Galactic center. The source spectrum from each flight is well fit by a single\r\npower law in the energy range 35-200 keV. The best-fit photon indices and 100 keV\r\nnormalizations are: \u03b3 = (2.05 \u00b1 0.15) and K_(100) = (8.5 \u00b1 0.5) x 10^(-5) cm^(-2) s^(-1) keV^(-1)\r\nand \u03b3 = (2.2 \u00b1 0.3) and K_(100) = (7.0 \u00b1 0.7) x 10^(-5) cm^(-2) s^(-1) keV^(-1) for the 1988 and\r\n1989 observations respectively. No flux above 200 keV was detected during either\r\nobservation. These values are consistent with a constant spectrum and indicate that\r\n1E 1740.7-2942 was in its normal hard X-ray emission state. A search on one hour\r\ntime scales showed no evidence for variability.
\r\n\r\nThe ROSAT HRI observed 1E 1740.7-2942 during the period 1991 March\r\n20-24. An improved source location has been derived from this observation. The\r\nbest fit coordinates (J2000) are: Right Ascension = 17^h43^m54^s.9, Declination =\r\n -29\u00b044'45\".3, with a 90% confidence error circle of radius 8\".5. The PSPC observation\r\nwas split between periods from 1992 September 28- October 4 and 1993 March\r\n23-28. A thermal bremsstrahlung model fit to the data yields a column density of\r\nN_H = 1.12^(+1.51)_(0.18) x cm^(-2) , consistent with earlier X- ray measurements.
\r\n\r\nWe observed the region of the Einstein IPC error circle for 1E 1740.7-2942\r\nwith the VLA at 1.5 and 4.9 GHz on 1989 March 2. The 4.9 GHz observation revealed\r\ntwo sources. Source 'A', which is the core of a double aligned radio jet source (Mirabel\r\net al. 1992), lies within our ROSAT error circle, further strengthening its identification\r\nwith 1E 1740.7-2942.
", "date": "1994", "date_type": "degree", "id_number": "CaltechTHESIS:05072013-085136174", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05072013-085136174", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Tony Diaz", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2013-05-07 16:19:17", "doi": "10.7907/485k-vs32", "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_defense_date": "1994-02-08", "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": "1994", "author_list": "Heindl, William Adams" }, { "id": "/id/eprint/3261", "eprint_id": 3261, "rev_number": 11, "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": "2025-08-05 23:49:44", "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" }, "orcid": "0000-0003-2219-9383", "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/7329", "eprint_id": 7329, "rev_number": 20, "documents": [ { "id": "/id/document/16762", "doc_id": 16762, "rev_number": 5, "files": [ { "id": "/id/file/102192", "fileid": 102192, "datasetid": "document", "objectid": 16762, "filename": "Looper_md_1993.pdf", "mime_type": "application/pdf", "filesize": 22811454, "mtime": "2012-12-26 04:46:29", "url": "/7329/1/Looper_md_1993.pdf" } ], "eprint_id": 7329, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Looper_md_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": 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"datestamp": "2012-12-12 17:18:42", "lastmod": "2024-06-24 20:24:16", "status_changed": "2012-12-12 17:18:42", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mark.d.looper@aero.org", "id": "Looper-Mark-Dixon", "name": { "family": "Looper", "given": "Mark Dixon" }, "orcid": "0000-0001-8223-1598", "show_email": "NO" } ] }, "title": "Energetic Protons in the Magnetosphere of Neptune", "ispublished": "unpub", "full_text_status": "public", "keywords": "Voyager ; Neptune ; radiation ; magnetosphere", "abstract": "The Cosmic Ray Subsystem aboard Voyager 2 measured large fluxes of trapped energetic\r\nprotons and electrons in the inner magnetosphere of Neptune during the 1989 flyby; the\r\nprotons above 1.9 MeV observed by the Low Energy Telescopes are analyzed in this thesis.\r\nProton events are extracted from pulse-height distributions dominated by low-energy electron\r\npileup noise, and fluxes are calculated with corrections for discriminator deadtime. Theoretical\r\nmodels for satellite absorption of charged particles are adapted to the large gyroradii of\r\nenergetic protons, and model magnetospheres are constructed that involve diffusion of particles\r\nin the presence of this absorption; parameters of these model magnetospheres are\r\nadjusted to reproduce the observations. The inward-diffusing proton flux is limited by\r\nabsorption due to the moon 1989N1 (Proteus), with absorption at high magnetic latitudes\r\n(whence high Ls) proving to be most important. The proton radial diffusion coefficient is an\r\norder of magnitude less than that inferred elsewhere for the electrons; this prevents protons\r\nfrom diffusing inward past 1989N1 before they are absorbed, and in fact the proton flux\r\nreturns to background levels within a limit well outside the minimum L-shell of 1989N1,\r\nwhile electrons can diffuse past this satellite so that their flux recovers before they are\r\nabsorbed by the other moons and rings closer to the planet. The rate of proton radial\r\ndiffusion, in comparison with that for electrons, is consistent with the diffusion being driven\r\nby electric fields from wind fluctuations in the ionosphere of Neptune. Radial diffusion\r\nalone, however, produces too much pitch-angle anisotropy as particles with mild anisotropy\r\nin the outer magnetosphere are transported inward, and pitch-angle diffusion must be invoked\r\nto reduce the excess anisotropy and reproduce the observations. The pitch-angle distributions\r\nat different Ls are consistent with the diffusion coefficient for this process being comparable\r\nin magnitude to that for radial diffusion inside L of about 6.8, though still much less than the\r\nstrong-diffusion limit, and negligible outside that L.\r\n", "date": "1993", "date_type": "degree", "id_number": "CaltechTHESIS:12122012-085110897", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:12122012-085110897", "related_url": { "items": [ { "description": "Some observations presented in published article in Science: \"Energetic Charged Particles in the Magnetosphere of Neptune\"", "type": "related", "url": "https://doi.org/10.1126/science.246.4936.1489" } ] }, "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" ] }, "deposited_on": "2012-12-12 17:18:42", "doi": "10.7907/QEPK-4523", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1993-01-08", "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": "1993", "author_list": "Looper, Mark Dixon" }, { "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/162986", "doc_id": 162986, "rev_number": 1, "files": [ { "id": "/id/file/460501", "fileid": 460501, "datasetid": "document", "objectid": 162986, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "2fc0b1f9ed10bf6e5c2580b753af42a6", "hash_type": "MD5", "filesize": 29322, "mtime": "2024-10-10 20:00:11", "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/6650", "eprint_id": 6650, "rev_number": 15, "documents": [ { "id": "/id/document/13577", "doc_id": 13577, "rev_number": 4, "files": [ { "id": "/id/file/88122", "fileid": 88122, "datasetid": "document", "objectid": 13577, "filename": "Gibner_ps_1992.pdf", "mime_type": "application/pdf", "filesize": 50491752, "mtime": "2012-12-26 04:38:42", "url": "/6650/1/Gibner_ps_1992.pdf" } ], "eprint_id": 6650, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Gibner_ps_1992.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/13578", "doc_id": 13578, "rev_number": 3, "files": [ { "id": "/id/file/207499", "fileid": 207499, "datasetid": "document", "objectid": 13578, "filename": "Gibner_ps_1992.zip", "mime_type": "application/zip", "filesize": 126308452, "mtime": "2016-08-22 21:23:12", "url": "/6650/2/Gibner_ps_1992.zip" } ], "eprint_id": 6650, "pos": 2, "format": "application/zip", "format_desc": "TIFF", "language": "en", "security": "internal", "license": "other", "main": "Gibner_ps_1992.zip", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/162995", "doc_id": 162995, "rev_number": 1, "files": [ { "id": "/id/file/460510", "fileid": 460510, "datasetid": "document", "objectid": 162995, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "3e5958e14d23b4378399283012772bbf", "hash_type": "MD5", "filesize": 25563, "mtime": "2024-10-10 20:00:26", "url": "/6650/3/indexcodes.txt" } ], "eprint_id": 6650, "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/13577" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/13577" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/13577" } ] } } ], "eprint_status": "archive", "userid": 51, "dir": "disk0/00/00/66/50", "datestamp": "2011-09-08 20:44:31", "lastmod": "2024-06-24 20:24:39", "status_changed": "2011-09-08 20:44:31", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gibner-P-S", "name": { "family": "Gibner", "given": "Peyton Stinson" }, "show_email": "NO" } ] }, "title": "Isotopic composition of galactic cosmic ray boron, carbon, nitrogen, and oxygen", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "Relative abundances of the isotopes of galactic cosmic ray B, C, N, and O nuclei have been measured using the balloon-borne High Energy Isotope Spectrometer Telescope (HEIST). Analysis of data collected during the 1988 HEIST flight from Prince Albert, Saskatchewan, has resulted in mass histograms containing ~890 boron, ~3100 carbon, ~910 nitrogen, and ~3300 oxygen nuclei. Masses were derived using both the Cerenkov-Energy and \u0394E-E' techniques, achieving a resulting rms mass resolution of ~0.26 amu. These isotopic composition measurements correspond to energy intervals at the top of the atmosphere of ~400-650 MeV/nucleon for boron, 430-670 MeV/nucleon for carbon, 440-680 MeV/nucleon for nitrogen, and 450-780 MeV/nucleon for oxygen, higher than previous direct isotope measurements for these elements.
\r\n\r\nThe abundance ratios of carbon, nitrogen, and oxygen at the top of the atmosphere have been interpreted using an interstellar propagation model that includes improved fragmentation cross sections. Because cosmic ray boron is used as a \"secondary tracer,\" the calculated isotope ratios of interest are insensitive to the value chosen for the solar modulation parameter, \u00f8. The resulting abundance ratios for cosmic ray source material include ^(14)N/O = 0.042 \u00b1 0.014 and ^(15)N/O \u2264 0.040, favoring no ^(15)N at the source. The carbon and oxygen isotopes at the cosmic ray source are ^(13)C/^(12)C = 0.005 \u00b1 .011 and ^(18)O/^(16)O = 0.0115 \u00b1 .0038, compared to solar system values of ^(13)C/^(12)C = 0.011 and ^(18)O/^(16)O = 0.0020. The derived cosmic ray source abundances show a possible enhancement of ^(18)O/^(16)O over the solar system value and a ^(13)C/^(12)C ratio consistent with solar system material. Taking a weighted average of our result with previous high resolution measurements of oxygen results in ^(18)O/^(16)O = 0.0075 \u00b1 0.0024, an enhancement in ^(18)O of 3.75 times the solar system value.
\r\n\r\nCurrent isotope results are compared with models of cosmic ray origin. Both the supermetallicity model and the \"anomalous\" solar system model predict an ^(18)O excess in cosmic rays, however, the \"anomalous\" solar system model also predicts an excess in ^(13)C. The Wolf-Rayet model fits many of the currently observed isotopic excesses in cosmic rays, but the predictions for ^(18)O/^(16)O and the elemental N/O ratio are still in question. We conclude that although further refinements in the Wolf-Rayet model may explain ^(18)O and N/O, none of the presently available models account quantitatively for all of the observed differences in composition between cosmic rays and solar system material.
\r\n", "date": "1992", "date_type": "degree", "id_number": "CaltechTHESIS:09062011-105435728", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:09062011-105435728", "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" ] }, "deposited_by": "Tony Diaz", "deposited_on": "2011-09-08 20:44:31", "doi": "10.7907/m2hn-q437", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1992-03-23", "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": "1992", "author_list": "Gibner, Peyton Stinson" }, { "id": "/id/eprint/2338", "eprint_id": 2338, "rev_number": 14, "documents": [ { "id": "/id/document/4432", "doc_id": 4432, "rev_number": 4, "files": [ { "id": "/id/file/25556", "fileid": 25556, "datasetid": "document", "objectid": 4432, "filename": "Grove_JE_1989.pdf", "mime_type": "application/pdf", "filesize": 9493627, "mtime": "2012-12-26 02:50:14", "url": "/2338/1/Grove_JE_1989.pdf" } ], "eprint_id": 2338, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Grove_JE_1989.pdf", "language": "en", "security": "internal", "license": "other", "main": "Grove_JE_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/21000" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/21000" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/21000" } ] } }, { "id": "/id/document/21000", "doc_id": 21000, "rev_number": 3, "files": [ { "id": "/id/file/25554", "fileid": 25554, "datasetid": "document", "objectid": 21000, "filename": "preview.png", "mime_type": "image/png", "hash": "e81b0c5eca61d12a217e7b4ac4e38f82", "hash_type": "MD5", "filesize": 7654, "mtime": "2012-12-26 02:50:14", "url": "/2338/2/preview.png" } ], "eprint_id": 2338, "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/4432" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4432" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4432" } ] } }, { "id": "/id/document/134568", "doc_id": 134568, "rev_number": 2, "files": [ { "id": "/id/file/380805", "fileid": 380805, "datasetid": "document", "objectid": 134568, "filename": "grove_JE_1989.pdf", "mime_type": "application/pdf", "hash": "b883ccdb93179a263e1f0fe4808813cc", "hash_type": "MD5", "filesize": 7669338, "mtime": "2021-07-15 19:12:45", "url": "/2338/3/grove_JE_1989.pdf" } ], "eprint_id": 2338, "pos": 3, "placement": 3, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "grove_JE_1989.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/158634", "doc_id": 158634, "rev_number": 1, "files": [ { "id": "/id/file/456149", "fileid": 456149, "datasetid": "document", "objectid": 158634, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "54aee86eb4d2f275941810752c52c458", "hash_type": "MD5", "filesize": 29154, "mtime": "2024-10-10 18:17:16", "url": "/2338/4/indexcodes.txt" } ], "eprint_id": 2338, "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/134568" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/134568" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/134568" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/23/38", "datestamp": "2007-05-31", "lastmod": "2021-07-15 20:28:33", "status_changed": "2009-09-25 02:34:59", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Grove-Jon-Eric", "name": { "family": "Grove", "given": "Jon Eric" }, "show_email": "NO" } ] }, "title": "A Balloon Measurement of the Isotopic Composition of Galactic Cosmic Ray Iron", "ispublished": "unpub", "full_text_status": "public", "keywords": "Physics", "abstract": "We have measured the isotopic composition of galactic cosmic ray iron in the energy interval ~1550-2200 MeV/nucleon using a balloon-borne mass spectrometer. The instrument was flown from Palestine, Texas, in May 1984 for >35 hours at an atmospheric depth of ~6 g/cm\u00b2. Masses were derived by the Cerenkov-Energy technique. The Cerenkov counter employed a silica aerogel radiator with index of refraction n = 1.1. Particle energies were measured in a stack of NaI(Tl) scintillators, which also provided particle trajectories. The calibration of the detectors is discussed, along with the algorithms we have used to calculate velocities, energies, and masses. The limitations of aerogels as Cerenkov radiators, particularly the stability of their light yield, are considered. A detailed discussion of the sources of mass uncertainty is presented, including an analytic model of the contribution from fluctuations in the Cerenkov yield from knock-on electrons. The achieved mass resolution is ~0.65 amu, which is consistent with the theoretical estimate. We report an \u2075\u2074Fe/\u2075\u2076Fe abundance ratio of 0.14+0.18-0.11 and an 84% confidence upper limit of \u2075\u2078Fe/\u2075\u2076Fe \u2264 0.07 at the top of the atmosphere. Combining our data with those of previous measurements of the composition of iron at lower energies, and using a model of the galactic propagation, we derive cosmic-ray source abundance ratios of \u2075\u2074Fe/\u2075\u2076Fe = 0.064+0.032-0.027 and \u2075\u2078Fe/\u2075\u2076Fe \u2264 0.062. These values are consistent with the composition of solar-system iron and place restrictions on the conditions under which cosmic-ray iron is synthesized.
", "date": "1989", "date_type": "degree", "id_number": "CaltechETD:etd-05312007-121425", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05312007-121425", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "other_numbering_system": { "items": [ { "id": "89-02", "name": "Space Radiation Laboratory (SRL)" } ] }, "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-31", "doi": "10.7907/3cr8-jv31", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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" }, { "id": "Kavanagh-R-W", "name": { "family": "Kavanagh", "given": "Ralph William" }, "role": "member" }, { "id": "Gomez-R", "name": { "family": "Gomez", "given": "Ricardo" }, "role": "member" }, { "email": "kip@caltech.edu", "id": "Thorne-K-S", "name": { "family": "Thorne", "given": "Kip S." }, "role": "member" }, { "email": "rmewaldt@caltech.edu", "id": "Mewaldt-R-A", "name": { "family": "Mewaldt", "given": "Richard A." }, "orcid": "0000-0003-2178-9111", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2007-05-31", "thesis_defense_date": "1989-04-21", "thesis_approved_date": "2007-05-31", "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": "1989", "author_list": "Grove, Jon Eric" }, { "id": "/id/eprint/2309", "eprint_id": 2309, "rev_number": 17, "documents": [ { "id": "/id/document/4360", "doc_id": 4360, "rev_number": 3, "files": [ { "id": "/id/file/25195", "fileid": 25195, "datasetid": "document", "objectid": 4360, "filename": "Christian_er_1989.pdf", "mime_type": "application/pdf", "filesize": 3996921, "mtime": "2012-12-26 02:49:55", "url": "/2309/1/Christian_er_1989.pdf" } ], "eprint_id": 2309, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Original (no OCR) Christian_er_1989.pdf", "language": "en", "security": "internal", "license": "other", "main": "Christian_er_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/20946" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/20946" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/20946" } ] } }, { "id": "/id/document/20946", "doc_id": 20946, "rev_number": 2, "files": [ { "id": "/id/file/25193", "fileid": 25193, "datasetid": "document", "objectid": 20946, "filename": "preview.png", "mime_type": "image/png", "hash": "e937d485845d727f6b22577d4800835b", "hash_type": "MD5", "filesize": 8089, "mtime": "2012-12-26 02:49:55", "url": "/2309/2/preview.png" } ], "eprint_id": 2309, "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/4360" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/4360" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/4360" } ] } }, { "id": "/id/document/134338", "doc_id": 134338, "rev_number": 2, "files": [ { "id": "/id/file/380037", "fileid": 380037, "datasetid": "document", "objectid": 134338, "filename": "christian-er_1989.pdf", "mime_type": "application/pdf", "hash": "7f10e506bfea58be33cd19fea4eb8222", "hash_type": "MD5", "filesize": 3412913, "mtime": "2021-07-06 23:56:52", "url": "/2309/3/christian-er_1989.pdf" } ], "eprint_id": 2309, "pos": 3, "placement": 3, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "christian-er_1989.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": "/id/document/158558", "doc_id": 158558, "rev_number": 1, "files": [ { "id": "/id/file/456073", "fileid": 456073, "datasetid": "document", "objectid": 158558, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "a744137bc089a35965ca1a77b214b602", "hash_type": "MD5", "filesize": 16676, "mtime": "2024-10-10 18:16:01", "url": "/2309/4/indexcodes.txt" } ], "eprint_id": 2309, "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/134338" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/134338" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/134338" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/23/09", "datestamp": "2007-05-31", "lastmod": "2021-07-07 00:09:13", "status_changed": "2009-09-25 02:34:04", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "eric.r.christian@nasa.gov", "id": "Christian-Eric-Richard", "name": { "family": "Christian", "given": "Eric Richard" }, "orcid": "0000-0003-2134-3937", "show_email": "NO" } ] }, "title": "Evidence for Anomalous Cosmic Ray Hydrogen", "ispublished": "unpub", "full_text_status": "public", "keywords": "Cosmic ray hydrogen", "abstract": "The High Energy Telescopes on the Voyager 1 and Voyager 2 spacecraft are used to measure the differential energy spectra of hydrogen and other elements. During the period of minimum solar modulation in 1987, changes in the shape of the hydrogen energy spectra are observed. It is shown that these changes are difficult to explain in the framework of current modulation theory, and are consistent with the emergence of an anomalous cosmic ray (ACR) hydrogen component. ACR hydrogen is predicted by the current theories of anomalous cosmic rays, but this is the first evidence that ACR hydrogen is actually present. Several different estimates of the contribution of ACR hydrogen are used to obtain peak fluxes of 0.33 \u00b1 0.12 particles/m2s sr MeV and 0.67 \u00b1 0.18 particles/m2s sr MeV for Voyager 1 and Voyager 2 respectively during the time period 1987/209-313.
\r\n\r\nUsing a model developed by Cummings and Stone (1987), we relate these fluxes of ACR hydrogen and the peak fluxes of ACR helium to the relative abundance of hydrogen and helium, n(H I)/n(He I), in the neutral gas flowing into the solar system from the local interstellar medium. For two different choices of parameters, we obtain values of 3 \u00b1 1 and 5 \u00b1 3 for n(H I)/n(He I), which should be compared to the cosmic relative abundance of ~ 10. Our values are consistent with previous results obtained from solar ultraviolet backscatter experiments, and support the hypothesis that hydrogen is substantially ionized in the very local interstellar medium.
", "date": "1989", "date_type": "degree", "id_number": "CaltechETD:etd-05302007-091830", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05302007-091830", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NGR 05-002-160" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Melissa Ray", "other_numbering_system": { "items": [ { "id": "89-01", "name": "Space Radiation Laboratory" } ] }, "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2007-05-31", "doi": "10.7907/AQ34-AJ87", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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": "bradf@caltech.edu", "id": "Filippone-B-W", "name": { "family": "Filippone", "given": "Bradley W." }, "orcid": "0000-0002-2618-2688", "role": "member" }, { "email": "newman@hep.caltech.edu", "id": "Newman-H-B", "name": { "family": "Newman", "given": "Harvey B." }, "orcid": "0000-0003-0964-1480", "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": "2007-05-30", "thesis_defense_date": "1989-02-15", "thesis_approved_date": "2007-05-31", "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": "1989", "author_list": "Christian, Eric Richard" }, { "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/163032", "doc_id": 163032, "rev_number": 1, "files": [ { "id": "/id/file/460547", "fileid": 460547, "datasetid": "document", "objectid": 163032, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "7ab08f6a2d14f5dc3b9479822bd055b0", "hash_type": "MD5", "filesize": 32192, "mtime": "2024-10-10 20:02:08", "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. I also retain 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": "Finger, Mark Harold" }, { "id": "/id/eprint/8688", "eprint_id": 8688, "rev_number": 33, "documents": [ { "id": "/id/document/52564", "doc_id": 52564, "rev_number": 4, "files": [ { "id": "/id/file/151879", "fileid": 151879, "datasetid": "document", "objectid": 52564, "filename": "Newport 1986.pdf", "mime_type": "application/pdf", "hash": "b87ba3ea44735bd6136169e369727149", "hash_type": "MD5", "filesize": 21657540, "mtime": "2014-10-09 21:54:16", "url": "/8688/2/Newport 1986.pdf" } ], "eprint_id": 8688, "pos": 2, "placement": 2, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Newport 1986.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": 50, "dir": "disk0/00/00/86/88", "datestamp": "2014-10-09 22:07:21", "lastmod": "2026-01-28 01:07:40", "status_changed": "2014-10-09 22:07:21", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Newport-Brian-John", "name": { "family": "Newport", "given": "Brian John" }, "show_email": "NO" } ] }, "title": "The Abundances of Ultraheavy Elements in the Cosmic Radiation", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "Analysis of the data from the Heavy Nuclei Experiment on the HEAO-3 spacecraft has yielded the cosmic ray abundances of odd-even element pairs with atomic number, Z, in the range 33 \u2264 Z \u2264 60, and the abundances of broad element groups in the range 62 \u2264 Z \u2264 83, relative to iron. These data show that the cosmic ray source composition in this charge range is quite similar to that of the solar system provided an allowance is made for a source fractionation based on first ionization potential. The observations are inconsistent with a source composition which is dominated by either r-process or s-process material, whether or not an allowance is made for first ionization potential. Although the observations do not exclude a source containing the same mixture of r- and s-process material as in the solar system. the data are best fit by a source having an r- to s-process ratio of 1.22+0.25-0.21, relative to the solar system The abundances of secondary elements are consistent with the leaky box model of galactic propagation, implying a pathlength distribution similar to that which explains the abundances of nuclei with Z < 29.
\r\n\r\nThe energy spectra of the even elements in the range 38 \u2264 Z \u2264 60 are found to have a deficiency of particles in the range ~1.5 to 3 GeV/amu, compared to iron. This deficiency may result from ionization energy loss in the interstellar medium, and is not predicted by propagation models which ignore such losses. ln addition, the energy spectra of secondary elements are found to be different to those of the primary elements. Such effects are consistent with observations of lighter nuclei, and are in qualitative agreement with galactic propagation models using a rigidity dependent escape length. The energy spectra of secondaries arising from the platinum group are found to be much steeper than those of lower Z. This effect may result from energy dependent fragmentation cross sections.
\r\n\r\n", "date": "1986", "date_type": "degree", "id_number": "CaltechTHESIS:10092014-143512211", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10092014-143512211", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Caltech" }, { "agency": "NASA", "grant_number": "NAG8-502" }, { "agency": "NASA", "grant_number": "NGR05-002-160" }, { "agency": "NASA", "grant_number": "NAS8-27978" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_on": "2014-10-09 22:07:21", "doi": "10.7907/2bfw-r090", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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": "scf@theory.caltech.edu", "id": "Frautschi-S-C", "name": { "family": "Frautschi", "given": "Steven C." }, "role": "member" }, { "id": "Barnes-C-A", "name": { "family": "Barnes", "given": "Charles A." }, "role": "member" }, { "email": "newman@hep.caltech.edu", "id": "Newman-H-B", "name": { "family": "Newman", "given": "Harvey B." }, "orcid": "0000-0003-0964-1480", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1986-05-21", "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": "1986", "author_list": "Newport, Brian John" }, { "id": "/id/eprint/8692", "eprint_id": 8692, "rev_number": 29, "documents": [ { "id": "/id/document/52584", "doc_id": 52584, "rev_number": 4, "files": [ { "id": "/id/file/151948", "fileid": 151948, "datasetid": "document", "objectid": 52584, "filename": "Lau_KH_1985.pdf", "mime_type": "application/pdf", "hash": "8c5bdd9cd987ac2336a93e9c57d125b4", "hash_type": "MD5", "filesize": 36109480, "mtime": "2014-10-14 17:27:46", "url": "/8692/1/Lau_KH_1985.pdf" } ], "eprint_id": 8692, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Lau_KH_1985.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": "disk0/00/00/86/92", "datestamp": "2014-10-15 16:17:01", "lastmod": "2025-11-20 22:34:13", "status_changed": "2014-10-15 16:17:01", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lau-Koon-Hang", "name": { "family": "Lau", "given": "Koon Hang" }, "show_email": "NO" } ] }, "title": "A Cerenkov-\u0394\u0395-Cerenkov Detector for High Energy Cosmic Ray Isotopes and an Accelerator Study of \u2074\u2070Ar & \u2075\u2076Fe Fragmentation", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "This thesis has two major parts. The first part of the thesis will describe a high energy cosmic ray detector -- the High Energy Isotope Spectrometer Telescope (HEIST). HEIST is a large area (0.25 m2sr) balloon-borne isotope spectrometer designed to make high-resolution measurements of isotopes in the element range from neon to nickel (10 \u2264 Z \u2264 28) at energies of about 2 GeV/nucleon. The instrument consists of a stack of 12 NaI(Tl) scintilla tors, two Cerenkov counters, and two plastic scintillators. Each of the 2-cm thick NaI disks is viewed by six 1.5-inch photomultipliers whose combined outputs measure the energy deposition in that layer. In addition, the six outputs from each disk are compared to determine the position at which incident nuclei traverse each layer to an accuracy of ~2 mm. The Cerenkov counters, which measure particle velocity, are each viewed by twelve 5-inch photomultipliers using light integration boxes.
\r\n\r\nHEIST-2 determines the mass of individual nuclei by measuring both the change in the Lorentz factor (\u0394\u03b3) that results from traversing the NaI stack, and the energy loss (\u0394\u0395) in the stack. Since the total energy of an isotope is given by \u0395 = \u03b3M, the mass M can be determined by M = \u0394\u0395/\u0394\u03b3. The instrument is designed to achieve a typical mass resolution of 0.2 amu.
\r\n\r\nThe second part of this thesis presents an experimental measurement of the isotopic composition of the fragments from the breakup of high energy 40Ar and 56Fe nuclei. Cosmic ray composition studies rely heavily on semi-empirical estimates of the cross-sections for the nuclear fragmentation reactions which alter the composition during propagation through the interstellar medium. Experimentally measured yields of isotopes from the fragmentation of 40Ar and 56Fe are compared with calculated yields based on semi-empirical cross-section formulae. There are two sets of measurements. The first set of measurements, made at the Lawrence Berkeley Laboratory Bevalac using a beam of 287 MeV/nucleon 40Ar incident on a CH2 target, achieves excellent mass resolution (\u03c3m \u2264 0.2 amu) for isotopes of Mg through K using a Si(Li) detector telescope. The second set of measurements, also made at the Lawrence Berkeley Laboratory Bevalac, using a beam of 583 MeV/nucleon 56Fe incident on a CH2 target, resolved Cr, Mn, and Fe fragments with a typical mass resolution of ~ 0.25 amu, through the use of the Heavy Isotope Spectrometer Telescope (HIST) which was later carried into space on ISEE-3 in 1978. The general agreement between calculation and experiment is good, but some significant differences are reported here.
\r\n", "date": "1985", "date_type": "degree", "id_number": "CaltechTHESIS:10142014-102314134", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10142014-102314134", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NGR 05-002-160" }, { "agency": "NASA", "grant_number": "NAG 5-308" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Bianca Rios", "deposited_on": "2014-10-15 16:17:01", "doi": "10.7907/m2gd-r904", "alt_title": { "items": [ "Cerenkov-Delta\u0395-Cerenkov Detector for High Energy Cosmic Ray Isotopes and an Accelerator Study of 40Ar and 56Fe Fragmentation" ] }, "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "politzer@theory.caltech.edu", "id": "Politzer-H-D", "name": { "family": "Politzer", "given": "Hugh David" }, "orcid": "0000-0002-4983-6621", "role": "chair" }, { "id": "Barnes-C-A", "name": { "family": "Barnes", "given": "Charles A." }, "role": "member" }, { "email": "barish@ligo.caltech.edu", "id": "Barish-B-C", "name": { "family": "Barish", "given": "Barry C." }, "orcid": "0000-0001-6386-7371", "role": "member" }, { "email": "rmewaldt@caltech.edu", "id": "Mewaldt-R-A", "name": { "family": "Mewaldt", "given": "Richard A." }, "orcid": "0000-0003-2178-9111", "role": "member" }, { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1985-05-31", "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": "1985", "author_list": "Lau, Koon Hang" }, { "id": "/id/eprint/8686", "eprint_id": 8686, "rev_number": 26, "documents": [ { "id": "/id/document/52537", "doc_id": 52537, "rev_number": 3, "files": [ { "id": "/id/file/151790", "fileid": 151790, "datasetid": "document", "objectid": 52537, "filename": "Berneman 1985.pdf", "mime_type": "application/pdf", "hash": "c264ded5f7386d01ad6a16f31fcc43dd", "hash_type": "MD5", "filesize": 29380421, "mtime": "2014-10-09 18:18:47", "url": "/8686/2/Berneman 1985.pdf" } ], "eprint_id": 8686, "pos": 2, "placement": 2, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Berneman 1985.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"files": [ { "id": "/id/file/462873", "fileid": 462873, "datasetid": "document", "objectid": 165358, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "fdc4fd1253d79801a0ca502c355402b6", "hash_type": "MD5", "filesize": 34439, "mtime": "2024-10-11 01:11:22", "url": "/8686/9/indexcodes.txt" } ], "eprint_id": 8686, "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/52537" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/52537" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/52537" } ] } } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/86/86", "datestamp": "2014-10-09 19:42:11", "lastmod": "2025-11-06 19:16:42", "status_changed": "2014-10-09 19:42:11", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Breneman-Hugh-Herbert-III", "name": { "family": "Breneman", "given": "Hugh Herbert, III" }, "show_email": "NO" } ] }, "title": "Solar Photospheric and Coronal Abundances from Solar Energetic Particle Measurements", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "Observations of solar energetic particles (SEPs) from 22 solar flares in the 1977-1982 time period are reported. The observations were made by the Cosmic Ray Subsystem on board the Voyager 1 and 2 spacecraft. SEP abundances have been obtained for all elements with 3 \u2264 Z \u2264 30 except Li, Be, B, F, Sc, V, Co and Cu, for which upper limits have been obtained. Statistically meaningful abundances of several rare elements (e.g., P, Cl, K, Ti, Mn) have been determined for the first time, and the average abundances of the more abundant elements have been determined with improved precision, typically a factor of three better than the best previous determinations.
\r\n\r\nPreviously reported results concerning the dependence of the fractionation of SEPs relative to photosphere on first ionization potential (FIP) have been confirmed and amplified upon with the new data. The monotonic Z-dependence of the variation between flares noted by earlier studies was found to be interpretable as a fractionation, produced by acceleration of the particles from the corona and their propagation through interplanetary space, which is ordered by the ionic charge-to-mass ratio Q/ M of the species making up the SEPs. It was found that Q/M is the primary organizing parameter of acceleration and propagation effects in SEPs, as evidenced by the dependence on Q/M of time, spatial and energy dependence within flares and of the abundance variability from flare to flare.
\r\n\r\nAn unfractionated coronal composition was derived by applying a simple Q/M fractionation correction to the observed average SEP composition, to simultaneously correct for all Q/M-correlated acceleration/propagation fractionation of SEPs. The resulting coronal composition agrees well with current XUV/X-ray spectroscopic measurements of coronal composition but is of much higher precision and is available for a much larger set of elements. Compared to spectroscopic photospheric abundances, the SEP-derived corona appears depleted in C and somewhat enriched in Cr (and possibly Ca and Ti).
\r\n\r\nAn unfractionated photospheric composition was derived by applying a simple FIP fractionation correction to the derived coronal composition, to correct for the FIP-associated fractionation of the corona during its formation from photospheric material. The resulting composition agrees well with the photospheric abundance tabulation of Grevesse (1984) except for an at least ~50% lower abundance of C and a significantly greater abundance of Cr and possibly Ti. The results support the Grevesse photospheric Fe abundance, about 50% higher than meteoritic and earlier solar values. The SEP-derived photospheric composition is not generally of higher precision than the available spectroscopic data, but it relies on fewer physical parameters and is available for some elements (C, N, Ne, Ar) which cannot be measured spectroscopically in the photosphere.
", "date": "1985", "date_type": "degree", "id_number": "CaltechTHESIS:10092014-111031305", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10092014-111031305", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS7-918" }, { "agency": "NASA", "grant_number": "NGR 05-002-160" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_on": "2014-10-09 19:42:11", "doi": "10.7907/4mma-e885", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "wnw@caltech.edu", "id": "Whaling-W", "name": { "family": "Whaling", "given": "Ward" }, "role": "member" }, { "id": "McKeown-R-D", "name": { "family": "McKeown", "given": "Robert D." }, "role": "member" }, { "email": "burnett@gps.caltech.edu", "id": "Burnett-D-S", "name": { "family": "Burnett", "given": "Donald S." }, "orcid": "0000-0001-9521-8675", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1985-05-24", "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": "Breneman, Hugh Herbert, III" }, { "id": "/id/eprint/8687", "eprint_id": 8687, "rev_number": 29, "documents": [ { "id": "/id/document/52555", "doc_id": 52555, "rev_number": 3, "files": [ { "id": "/id/file/151841", "fileid": 151841, "datasetid": "document", "objectid": 52555, "filename": "Spalding_j_1983.pdf", "mime_type": "application/pdf", "hash": "884340edc9e6870dd8122f3452687392", "hash_type": "MD5", "filesize": 24748901, "mtime": "2014-10-09 20:53:57", "url": "/8687/1/Spalding_j_1983.pdf" } ], "eprint_id": 8687, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Spalding_j_1983.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"archive", "userid": 87, "dir": "disk0/00/00/86/87", "datestamp": "2014-10-09 21:27:55", "lastmod": "2025-08-07 20:20:58", "status_changed": "2014-10-09 21:27:55", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Spalding-John-David", "name": { "family": "Spalding", "given": "John David" }, "show_email": "NO" } ] }, "title": "The Isotopic Composition of Energetic Particles Emitted from a Large Solar Flare", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "We report measurements of isotope abundance ratios for 5-50 MeV/nuc nuclei from a large solar flare that occurred on September 23, 1978. The measurements were made by the Heavy Isotope Spectrometer Telescope (HIST) on the ISEE-3 satellite orbiting the Sun near an Earth-Sun libration point approximately one million miles sunward of the Earth. We report finite values for the isotope abundance ratios 13C/12C, 15N/14N, 18O/16O, 22Ne/ 20Ne, 25Mg/24Mg, and 26Mg/24Mg, and upper limits for the isotope abundance ratios 3He/4He, 14C/12C, 17O/16O, and 21Ne/20Ne.
\r\n\r\nWe measured element abundances and spectra to compare the September 23, 1978 flare with other flares reported in the literature. The flare is a typical large flare with \"low\" Fe/O abundance (\u2264 0.1).
\r\n\r\nFor 13C/12C, 15N/14N, 18O/16O, 25Mg/ 24Mg, and 26Mg/24Mg, our measured isotope abundance ratios agree with the solar system abundance ratios of Cameron (1981). For neon we measure 22Ne/20Ne = 0.109 + 0.026 - 0.019, a value that is different with confidence 97.5% from the abundance measured in the solar wind by Geiss at al. (1972) of 22Ne/20Ne = 0.073 \u00b1 0.001. Our measurement for 22Ne/20Ne agrees with the isotopic composition of the meteoritic component neon-A.
\r\n\r\nSeparate arguments appear to rule out simple mass fractionation in the solar wind and in our solar energetic particle measurements as the cause of the discrepancy in the comparison of the apparent compositions of these two sources of solar material.
", "date": "1983", "date_type": "degree", "id_number": "CaltechTHESIS:10092014-135300222", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10092014-135300222", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS5-20721" }, { "agency": "NASA", "grant_number": "NGR 05-002-160" }, { "agency": "Caltech" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2014-10-09 21:27:55", "doi": "10.7907/dt5j-0t88", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "email": "rmewaldt@caltech.edu", "id": "Mewaldt-R-A", "name": { "family": "Mewaldt", "given": "Richard A." }, "orcid": "0000-0003-2178-9111", "role": "chair" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "hitlin@caltech.edu", "id": "Hitlin-D-G", "name": { "family": "Hitlin", "given": "David G." }, "orcid": "0000-0003-4028-6982", "role": "member" }, { "id": "Kavanagh-R-W", "name": { "family": "Kavanagh", "given": "Ralph William" }, "role": "member" }, { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1982-11-23", "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. 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"archive", "userid": 87, "dir": "disk0/00/00/86/85", "datestamp": "2014-10-09 19:48:32", "lastmod": "2025-08-01 18:53:19", "status_changed": "2014-10-09 19:48:32", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Krombel-Keith-E", "name": { "family": "Krombel", "given": "Keith E." }, "show_email": "NO" } ] }, "title": "The Relative Abundances of Sn, Te, Xe, Ba, and Ce in the Cosmic Radiation", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "Elements with even atomic number (Z) in the interval 50 \u2264 Z \u2264 58 have been resolved in the cosmic radiation using the Heavy Nuclei Experiment on the HEAO-3 satellite. Their relative abundances have been compared with the results expected from pure r-process material, pure s-process material, and solar system material, both with and without a modification due to possible first ionization potential effects. Such effects may be the result of the preferential acceleration, and hence enhancement in the cosmic rays, or those elements having low first ionization potentials. We find that our measurements are inconsistent with pure r-process material at the greater than 98% confidence level whether or not the first ionization potential adjustments are made.
\r\n\r\nIn addition, we have compared our results with mixtures having varying ratios of pure r-process material to pure s-process material. We find that, if no first ionization potential effects are included,
\r\n\r\n(r/s)CRS/(r/s)SS = 0.20+0.18-0.14
\r\n\r\nwhere CRS refers to the cosmic ray source and SS refers to the solar system, consistent with having an almost pure s-process source. If the first ionization potential adjustments are applied
\r\n\r\n(r/s)CRS/(r/s)SS = 1.5+1.1-0.7
\r\n\r\nconsistent with a solar system mixture.
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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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"http://eprints.org/relation/isVersionOf", "uri": "/id/document/108127" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/108127" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/108127" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/13/89", "datestamp": "2009-04-15", "lastmod": "2025-04-28 22:00:10", "status_changed": "2009-09-25 02:02:54", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "neil.gehrels@nasa.gov", "id": "Gehrels-Neil", "name": { "family": "Gehrels", "given": "Neil" }, "show_email": "NO" } ] }, "title": "Energetic Oxygen and Sulfur Ions in the Jovian Magnetosphere", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics) ; Jupiter; Magnetosphere", "abstract": "Observations of 1 to 20 MeV/nuc oxygen, sodium, and sulfur ions in the Jovian magnetosphere are reported. Measurements made by the Cosmic Ray Subsystem on Voyager 1 and 2 are used to calculate abundances and energy spectra in the region from 5 to 20 Jovian radii (RJ). The phase space density of the oxygen ions calculated from the spectra has a positive radial gradient between 6 and 17 RJ, indicating an inward diffusive flow. The diffusion coefficient upper limit at 9 RJ is ~10-5s-1. This limit, combined with the analysis of Voyager plasma observations by Siscoe et al. [1981], implies an upper limit to the mass loading rate near Io of ~1028 ions/s.
\r\n\r\nThe energetic oxygen lifetime is within an order of magnitude of the strong pitch-angle diffusion lifetime in this region, with the largest total number of particles lost between 7.5 and 12.5 RJ. It is shown that the losses are not due to geometric absorption by Io, absorption by dust grains, or energy loss in the plasma of the inner magnetosphere, and it is therefore postulated that the primary loss mechanism is pitch-angle scattering into the loss cone.
\r\n\r\nThe power delivered to the Jovian atmosphere by oxygen and sulfur ions with magnetic moments greater than 70 MeV/nuc-G (E\u22730.3 MeV/nuc at 10 RJ, scattered into the loss cone between 6 and 17 RJ, is ~5x1012 W; a power comparable to the ~1.2x1013 W required to produce the auroral emission observed by the ultraviolet spectrometer on Voyager [Broadfoot et al., 1981]. The measured dependence of the input power on magnetic moment threshold indicates that additional power is contributed by oxygen and sulfur ions with magnetic moments less than 70 MeV/nuc-G. Since most of the particles are lost between 7.5 and 12.5 RJ, the latitudinal zone in which the most energy is deposited in the atmosphere is ~67\u00b0 to ~71\u00b0.
\r\n", "date": "1982", "date_type": "degree", "id_number": "CaltechETD:etd-04142009-144756", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-04142009-144756", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAGW-200" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory", "Caltech Distinguished Alumni Award" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2009-04-15", "doi": "10.7907/QBH7-KH81", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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" }, { "id": "Pine-J", "name": { "family": "Pine", "given": "Jerome" }, "role": "member" }, { "id": "Barnes-C-A", "name": { "family": "Barnes", "given": "Charles A." }, "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": "2009-04-14", "thesis_defense_date": "1981-09-11", "thesis_approved_date": "2009-04-15", "thesis_awards": "Caltech Distinguished Alumni Award, 2016", "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": "1982", "author_list": "Gehrels, Neil" }, { "id": "/id/eprint/8689", "eprint_id": 8689, "rev_number": 38, "documents": [ { "id": "/id/document/52570", "doc_id": 52570, "rev_number": 4, "files": [ { "id": "/id/file/151902", "fileid": 151902, "datasetid": "document", "objectid": 52570, "filename": "Zumberge_JF_1981.pdf", "mime_type": "application/pdf", "hash": "b9fde28c8cba0add2c982485ae449c46", "hash_type": "MD5", "filesize": 15101550, "mtime": "2014-10-09 22:59:18", "url": "/8689/1/Zumberge_JF_1981.pdf" } ], "eprint_id": 8689, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Zumberge_JF_1981.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": 635, "dir": "disk0/00/00/86/89", "datestamp": "2014-10-09 23:14:29", "lastmod": "2025-02-26 22:34:20", "status_changed": "2014-10-09 23:14:29", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zumberge-James-Frederick", "name": { "family": "Zumberge", "given": "James Frederick" }, "show_email": "NO" } ] }, "title": "A Balloon Measurement of the Isotopic Composition of Galactic Cosmic Ray Boron, Carbon, and Nitrogen", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "The isotopic compositions of galactic cosmic ray boron, carbon, and nitrogen have been measured at energies near 300 MeV amu-1, using a balloon-borne instrument at an atmospheric depth of ~ 5 g cm-2. The calibrations of the detectors comprising the instrument are described. The saturation properties of the cesium iodide scintilla tors used for measurement of particle energy are studied in the context of analyzing the data for mass. The achieved rms mass resolution varies from ~ 0.3 amu at boron to ~ 0.5 amu at nitrogen, consistent with a theoretical analysis of the contributing factors. Corrected for detector interactions and the effects of the residual atmosphere, the results are 10B/B = 0.33+0.17-0.11, 13C/C = 0.06+0.13-0.01, and 15N/N = 0.42+0.19-0.17. A model of galactic propagation and solar modulation is described. Assuming a cosmic ray source composition of solar-like isotopic abundances, the model predicts abundances near earth consistent with the measurements.
\r\n", "date": "1981", "date_type": "degree", "id_number": "CaltechTHESIS:10092014-153207228", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10092014-153207228", "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": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Ignis Nguyen", "deposited_on": "2014-10-09 23:14:29", "doi": "10.7907/22yw-v483", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "email": "ecs@srl.caltech.edu", "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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" }, { "id": "Tombrello-T-A", "name": { "family": "Tombrello", "given": "Thomas A." }, "role": "member" }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "Roger D." }, "role": "member" }, { "email": "burnett@gps.caltech.edu", "id": "Burnett-D-S", "name": { "family": "Burnett", "given": "Donald S." }, "orcid": "0000-0001-9521-8675", "role": "member" } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1981-02-25", "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": "1981", "author_list": "Zumberge, James Frederick" }, { "id": "/id/eprint/8682", "eprint_id": 8682, "rev_number": 36, "documents": [ { "id": "/id/document/52495", "doc_id": 52495, "rev_number": 3, "files": [ { "id": "/id/file/151668", "fileid": 151668, "datasetid": "document", "objectid": 52495, "filename": "Hartman_sr_1979.pdf", "mime_type": "application/pdf", "hash": "283775c8ab6d1177a32aa5ee1f79116e", "hash_type": "MD5", "filesize": 27388238, "mtime": "2014-10-09 16:55:47", "url": "/8682/1/Hartman_sr_1979.pdf" } ], "eprint_id": 8682, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Hartman_sr_1979.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"/id/file/462869", "fileid": 462869, "datasetid": "document", "objectid": 165354, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "c623afceb0564bc08d1e09570e827991", "hash_type": "MD5", "filesize": 19364, "mtime": "2024-10-11 01:11:14", "url": "/8682/7/indexcodes.txt" } ], "eprint_id": 8682, "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/52495" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/52495" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/52495" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/00/86/82", "datestamp": "2014-10-09 17:22:22", "lastmod": "2024-11-27 20:26:23", "status_changed": "2014-10-09 17:22:22", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hartman-Steward-Russell", "name": { "family": "Hartman", "given": "Steward Russell" }, "show_email": "NO" } ] }, "title": "Observations of 1-6 MeV Jovian Electrons at 1 AU and a Study of Their Propogation", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "The 1-6 MeV electron flux at 1 AU has been measured for the\r\ntime period October 1972 to December 1977 by the Caltech\r\nElectron/Isotope Spectrometers on the IMP-7 and IMP-8 satellites.\r\nThe non-solar interplanetary electron flux reported here covered\r\nparts of five synodic periods. The 88 Jovian increases identified\r\nin these five synodic periods were classified by their time profiles.\r\nThe fall time profiles were consistent with an exponential fall\r\nwith \u03c4 \u2248 4-9 days. The rise time profiles displayed a systematic\r\nvariation over the synodic period. Exponential rise time profiles\r\nwith \u03c4 \u2248 1-3 days tended to occur in the time period before nominal\r\nconnection, diffusive profiles predicted by the convection-diffusion\r\nmodel around nominal connection, and abrupt profiles after nominal\r\nconnection.
\r\n\r\nThe times of enhancements in the magnetic field, \u2502B\u2502, at 1 AU\r\nshowed a better correlation than corotating interaction regions (CIR's)\r\nwith Jovian increases and other changes in the electron flux at 1 AU,\r\nsuggesting that \u2502B\u2502 enhancements indicate the times that barriers to\r\nelectron propagation pass Earth. Time sequences of the increases and\r\ndecreases in the electron flux at 1 AU were qualitatively modeled by\r\nusing the times that CIR's passed Jupiter and the times that \u2502B\u2502\r\nenhancements passed Earth.
\r\n\r\nThe electron data observed at 1 AU were modeled by using a\r\nconvection-diffusion model of Jovian electron propagation. The\r\nsynodic envelope formed by the maxima of the Jovian increases was\r\nmodeled by the envelope formed by the predicted intensities at a\r\ntime less than that needed to reach equilibrium. Even though the\r\nenvelope shape calculated in this way was similar to the observed\r\nenvelope, the required diffusion coefficients were not consistent\r\nwith a diffusive process.
\r\n\r\nThree Jovian electron increases at 1 AU for the 1974 synodic\r\nperiod were fit with rise time profiles calculated from the\r\nconvection-diffusion model. For the fits without an ambient\r\nelectron background flux, the values for the diffusion coefficients\r\nthat were consistent with the data were kx = 1.0 - 2.5 x 1021 cm2/sec\r\nand ky = 1.6 - 2.0 x 1022 cm2/sec. For the fits that included the\r\nambient electron background flux, the values for the diffusion\r\ncoefficients that were consistent with the data were\r\nkx = 0.4 - 1.0 x 1021 cm2/sec and ky = 0.8 - 1.3 x 1022 cm2/sec.
\r\n\r\n", "date": "1979", "date_type": "degree", "id_number": "CaltechTHESIS:10092014-094710787", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10092014-094710787", "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" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2014-10-09 17:22:22", "doi": "10.7907/8spt-ea51", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1979-05-14", "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": "Hartman, Steward Russell" }, { "id": "/id/eprint/8674", "eprint_id": 8674, "rev_number": 22, "documents": [ { "id": "/id/document/52436", "doc_id": 52436, "rev_number": 2, "files": [ { "id": "/id/file/151511", "fileid": 151511, "datasetid": "document", "objectid": 52436, "filename": "Wiedenbeck 1978.pdf", "mime_type": "application/pdf", "hash": "63dfa9290ae5c8efc302ff99e4869efd", "hash_type": "MD5", "filesize": 29662959, "mtime": "2014-10-07 18:48:04", "url": "/8674/1/Wiedenbeck 1978.pdf" } ], "eprint_id": 8674, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Wiedenbeck 1978.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"objectid": 165346, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "a958b5ab55b20671397eae121023eec4", "hash_type": "MD5", "filesize": 32340, "mtime": "2024-10-11 01:10:59", "url": "/8674/13/indexcodes.txt" } ], "eprint_id": 8674, "pos": 13, "placement": 13, "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/52436" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/52436" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/52436" } ] } }, { "id": "/id/document/165347", "doc_id": 165347, "rev_number": 1, "files": [ { "id": "/id/file/462862", "fileid": 462862, "datasetid": "document", "objectid": 165347, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "eeba1f459dc135a9281150dced6e33f7", "hash_type": "MD5", "filesize": 688, "mtime": "2024-10-11 01:10:59", "url": "/8674/14/indexcodes.txt" } ], "eprint_id": 8674, "pos": 14, "placement": 14, "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/52443" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/52443" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/52443" } ] } } ], "eprint_status": "archive", "userid": 50, "dir": "disk0/00/00/86/74", "datestamp": "2014-10-07 20:11:34", "lastmod": "2024-11-14 19:47:53", "status_changed": "2014-10-07 20:11:34", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "email": "mark.e.wiedenbeck@jpl.nasa.gov", "id": "Wiedenbeck-Mark-Edward", "name": { "family": "Wiedenbeck", "given": "Mark Edward" }, "show_email": "NO" } ] }, "title": "An Investigation of Techniques for the Measurement and Interpretation of Cosmic Ray Isotopic Abundances", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "An instrument, the Caltech High Energy Isotope\r\nSpectrometer Telescope (HEIST), has been developed to\r\nmeasure isotopic abundances of cosmic ray nuclei in the\r\ncharge range 3 \u2264 Z \u2264 28 and the energy range between 30 and\r\n800 MeV/nuc by employing an energy loss -- residual energy\r\ntechnique. Measurements of particle trajectories and\r\nenergy losses are made using a multiwire proportional\r\ncounter hodoscope and a stack of CsI(TI) crystal\r\nscintillators, respectively. A detailed analysis has been\r\nmade of the mass resolution capabilities of this\r\ninstrument.
\r\n\r\nLandau fluctuations set a fundamental limit on the\r\nattainable mass resolution, which for this instrument\r\nranges between ~.07 AMU for z~3 and ~.2 AMU for z~2b.\r\nContributions to the mass resolution due to uncertainties\r\nin measuring the path-length and energy losses of the\r\ndetected particles are shown to degrade the overall mass\r\nresolution to between ~.1 AMU (z~3) and ~.3 AMU\r\n(z~2b).
\r\n\r\nA formalism, based on the leaky box model of cosmic\r\nray propagation, is developed for obtaining isotopic\r\nabundance ratios at the cosmic ray sources from abundances\r\nmeasured in local interstellar space for elements having\r\nthree or more stable isotopes, one of which is believed to\r\nbe absent at the cosmic ray sources. This purely\r\nsecondary isotope is used as a tracer of secondary\r\nproduction during propagation. This technique is\r\nillustrated for the isotopes of the elements O, Ne, S, Ar\r\nand Ca.
\r\n\r\nThe uncertainties in the derived source ratios due to\r\nerrors in fragmentation and total inelastic cross\r\nsections, in observed spectral shapes, and in measured\r\nabundances are evaluated. It is shown that the dominant\r\nsources of uncertainty are uncorrelated errors in the\r\nfragmentation cross sections and statistical uncertainties\r\nin measuring local interstellar abundances.
\r\n\r\nThese results are applied to estimate the extent to\r\nwhich uncertainties must be reduced in order to\r\ndistinguish between cosmic ray production in a solar-like\r\nenvironment and in various environments with greater\r\nneutron enrichments.
\r\n", "date": "1978", "date_type": "degree", "id_number": "CaltechTHESIS:10072014-112144047", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10072014-112144047", "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" ] }, "deposited_on": "2014-10-07 20:11:34", "doi": "10.7907/TXRP-JV20", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" }, { "id": "Vogt-R-E", "name": { "family": "Vogt", "given": "Rochus E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1977-12-09", "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": "1978", "author_list": "Wiedenbeck, Mark Edward" }, { "id": "/id/eprint/8673", "eprint_id": 8673, "rev_number": 23, "documents": [ { "id": "/id/document/52422", "doc_id": 52422, "rev_number": 2, "files": [ { "id": "/id/file/151470", "fileid": 151470, "datasetid": "document", "objectid": 52422, "filename": "Marshall-fe-1977.pdf", "mime_type": "application/pdf", "hash": "9998475ca8b39de79f5863e689dec9c2", "hash_type": "MD5", "filesize": 29171443, "mtime": "2014-10-07 17:57:03", "url": "/8673/1/Marshall-fe-1977.pdf" } ], "eprint_id": 8673, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Marshall-fe-1977.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { 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"files": [ { "id": "/id/file/462860", "fileid": 462860, "datasetid": "document", "objectid": 165345, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "9b323806925bb3b356d23b986d0e558f", "hash_type": "MD5", "filesize": 19484, "mtime": "2024-10-11 01:10:56", "url": "/8673/8/indexcodes.txt" } ], "eprint_id": 8673, "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/52422" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/52422" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/52422" } ] } } ], "eprint_status": "archive", "userid": 104, "dir": "disk0/00/00/86/73", "datestamp": "2014-10-07 18:09:41", "lastmod": "2024-10-30 01:20:19", "status_changed": "2014-10-07 18:09:41", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Marshall-Francis-E", "name": { "family": "Marshall", "given": "Francis E." }, "show_email": "NO" } ] }, "title": "The Streaming of 1.3-2.3 MeV Cosmic-Ray Protons During Periods Between Prompt Solar Particle Events", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics) ; cosmic-ray, protons", "abstract": "The anisotropy of 1.3 - 2.3 MeV protons in interplanetary space has been measured using the Caltech Electron/Isotope Spectrometer aboard IMP-7 for 317 6-hour periods from 72/273 to 74/2. Periods dominated by prompt solar particle events are not included. The convective and diffusive anisotropies are determined from the\r\nobserved anisotropy using concurrent solar wind speed measurements and observed energy spectra. The diffusive flow of particles is found to be typically toward the sun, indicating a positive radial gradient in the particle density. This anisotropy is inconsistent with previously proposed sources of low-energy proton increases seen at 1 AU which involve continual solar acceleration.
\r\n\r\nThe typical properties of this new component of low-energy cosmic rays have been determine d for this period which is near solar minimum. The particles have a median intensity of 0.06 protons/ cm^(2)-sec-sr-MeV and a mean spectral index of -3.15.The amplitude of the diffusive anisotropy is approximately proportional to\r\nthe solar wind speed. The rate at which particles are diffusing toward the sun is larger than the rate at which the solar wind is convecting the particles away from the sun. The 20 to 1 proton to alpha ratio typical of this new component has been reported by Mewaldt, et al. (1975b).
\r\n\r\nA propagation model with \u03ba_(rr) assumed independent of radius and energy is used to show that the anisotropy could be due to increases similar to those found by McDonald, et al. (1975) at ~3 AU. The interplanetary Fermi-acceleration model proposed by Fisk (1976) to explain the increases seen near 3 AU is not consistent with the ~12 per cent diffusive anisotropy found.
\r\n\r\nThe dependence of the diffusive anisotropy on various parameters is shown. A strong dependence of the direction of the diffusive anisotropy on the concurrently measured magnetic field direction is found, indicating a \u03ba_\u22a5 less than \u03ba_\u2225 to be typical for this large data set.
\r\n", "date": "1977", "date_type": "degree", "id_number": "CaltechTHESIS:10072014-104228753", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10072014-104228753", "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" ] }, "deposited_by": "Dan Anguka", "deposited_on": "2014-10-07 18:09:41", "doi": "10.7907/X1Z0-0M25", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" }, { "id": "Vogt-R-E", "name": { "family": "Vogt", "given": "Rochus E." }, "role": "co-advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1976-09-14", "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": "Marshall, Francis E." }, { "id": "/id/eprint/8679", "eprint_id": 8679, "rev_number": 28, "documents": [ { "id": "/id/document/52468", "doc_id": 52468, "rev_number": 2, "files": [ { "id": "/id/file/151585", "fileid": 151585, "datasetid": "document", "objectid": 52468, "filename": "Hurford_gj_1975.pdf", "mime_type": "application/pdf", "hash": "5c8b22cbb5998fdc947a8b48da06ae40", "hash_type": "MD5", "filesize": 17688002, "mtime": "2014-10-09 14:59:57", "url": "/8679/1/Hurford_gj_1975.pdf" } ], "eprint_id": 8679, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Hurford_gj_1975.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"files": [ { "id": "/id/file/462867", "fileid": 462867, "datasetid": "document", "objectid": 165352, "filename": "indexcodes.txt", "mime_type": "text/plain", "hash": "b12da5b46d772552d8d1f821c56573e2", "hash_type": "MD5", "filesize": 20967, "mtime": "2024-10-11 01:11:09", "url": "/8679/8/indexcodes.txt" } ], "eprint_id": 8679, "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/52468" }, { "type": "http://eprints.org/relation/isVolatileVersionOf", "uri": "/id/document/52468" }, { "type": "http://eprints.org/relation/isIndexCodesVersionOf", "uri": "/id/document/52468" } ] } } ], "eprint_status": "archive", "userid": 87, "dir": "disk0/00/00/86/79", "datestamp": "2014-10-09 15:48:02", "lastmod": "2024-08-05 21:36:04", "status_changed": "2014-10-09 15:48:02", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hurford-Gordon-James", "name": { "family": "Hurford", "given": "Gordon James" }, "show_email": "NO" } ] }, "title": "Observations of Hydrogen and Helium Isotopes in Solar Cosmic Rays", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "The isotopic composition of hydrogen and helium in solar cosmic\r\nrays provides a means of studying solar flare particle acceleration\r\nmechanisms since the enhanced relative abundance of rare isotopes, such\r\nas 2H, 3H and 3He, is due to their production by inelastic nuclear\r\ncollisions in the solar atmosphere during the flare. In this work the\r\nCaltech Electron/Isotope Spectrometer on the IMP-7 spacecraft has been\r\nused to measure this isotopic composition. The response of the dE/dx-E\r\nparticle telescope is discussed and alpha particle channeling in thin\r\ndetectors is identified as an important background source affecting\r\nmeasurement of low values of (3He/4He).
\r\n\r\nThe following flare-averaged results are obtained for the\r\nperiod, October, 1972 - November, 1973: (2H/1H) = 7+10-6 X 10-6 \r\n(1.6 - 8.6 MeV/nuc), (3H/1H) less than 3.4 x 10-6 (1.2 - 6.8 MeV/nuc),\r\n(3He/4He) = (9 \u00b1 4) x 10-3, (3He/1H) = (1.7 \u00b1 0.7) x 10-4\r\n(3.1 - 15.0 MeV/nuc). The deuterium and tritium ratios are significantly\r\nlower than the same ratios at higher energies, suggesting that the\r\ndeuterium and tritium spectra are harder than that of the protons. They\r\nare, however, consistent with the same thin target model relativistic\r\npath length of ~ 1 g/cm2 (or equivalently ~ 0.3 g/cm2 at 30 MeV/nuc) which\r\nis implied by the higher energy results. The 3He results, consistent with\r\nprevious observations, would imply a path length at least 3 times as long,\r\nbut the observations may be contaminated by small 3He rich solar events.
\r\n\r\nDuring 1973 three \"3He rich events,\" containing much more\r\n3He than 2H or 3H were observed on 14 February, 29 June and 5 September.\r\nAlthough the total production cross sections for 2H,3H and 3He are\r\ncomparable, an upper limit to (2H/3He) and (3H/3He) was 0.053\r\n(2.9-6.8 MeV/nuc), summing over the three events. This upper limit\r\nis marginally consistent with Ramaty and Kozlovsky's thick target model\r\nwhich accounts for such events by the nuclear reaction kinematics and\r\ndirectional properties of the flare acceleration process. The 5\r\nSeptember event was particularly significant in that much more 3He was\r\nobserved than 4He and the fluxes of 3He and 1H were about equal. The\r\nrange of (3He/4He) for such events reported to date is 0.2 to ~ 6 while\r\n(3He/1H) extends from 10-3 to ~ 1. The role of backscattered and \r\nmirroring protons and alphas in accounting for such variations is\r\ndiscussed.
", "date": "1975", "date_type": "degree", "id_number": "CaltechTHESIS:10092014-075936061", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10092014-075936061", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-11066" }, { "agency": "NASA", "grant_number": "NGR-05-002-160" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Benjamin Perez", "deposited_on": "2014-10-09 15:48:02", "doi": "10.7907/WGAQ-5D56", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" }, { "id": "Vogt-R-E", "name": { "family": "Vogt", "given": "Rochus E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1974-10-01", "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": "1975", "author_list": "Hurford, Gordon James" }, { "id": "/id/eprint/8680", "eprint_id": 8680, "rev_number": 19, "documents": [ { "id": "/id/document/52476", "doc_id": 52476, "rev_number": 2, "files": [ { "id": "/id/file/151624", "fileid": 151624, "datasetid": "document", "objectid": 52476, "filename": "Vidor thesis.pdf", "mime_type": "application/pdf", "hash": "ede87411354b9f0460f11b37c03fd199", "hash_type": "MD5", "filesize": 17347519, "mtime": "2014-10-09 16:10:46", "url": "/8680/1/Vidor thesis.pdf" } ], "eprint_id": 8680, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Vidor thesis.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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"userid": 50, "dir": "disk0/00/00/86/80", "datestamp": "2014-10-09 16:18:00", "lastmod": "2024-08-07 19:12:53", "status_changed": "2014-10-09 16:18:00", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vidor-Solomon-Benjamin", "name": { "family": "Vidor", "given": "Solomon Benjamin" }, "show_email": "NO" } ] }, "title": "Observations of Nitrogen and Oxygen Isotopes in the Low Energy Cosmic Rays", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "The isotopic composition of the enhanced low energy nitrogen\r\nand oxygen cosmic rays can provide information regarding the source\r\nof these particles. Using the Caltech Electron/Isotope Spectrometer\r\naboard the IMP-7 satellite, a measurement of this isotopic composition\r\nwas made. To determine the isotope response of the instrument, a\r\ncalibration was performed, and it was determined that the standard\r\nrange-energy tables were inadequate to calculate the isotope response.\r\nFrom the calibration, corrections to the standard range-energy tables\r\nwere obtained which can be used to calculate the isotope response of\r\nthis and similar instruments.
\r\n\r\nThe low energy nitrogen and oxygen cosmic rays were determined\r\nto be primarily ^(14)N and ^(16)O. Upper limits were obtained for the\r\nabundances of the other stable nitrogen and oxygen isotopes. To the\r\n84% confidence level the isotopic abundances are: ^(15)N/N \u2264 0.26\r\n(5.6- 12.7 MeV/nucleon), ^(17)0/0 \u2264 0.13 (7.0- 11.8 MeV/nucleon),\r\n(18)0/0 \u2264 0.12 (7.0 - 11.2 MeV/nucleon). The nitrogen composition\r\ndiffers from higher energy measurements which indicate that ^(15)N, which\r\nis thought to be secondary, is the dominant isotope. This implies that\r\nthe low energy enhanced cosmic rays are not part of the same population\r\nas the higher energy cosmic rays and that they have not passed through\r\nenough material to produce a large fraction of ^(15)N. The isotopic composition of the low energy enhanced nitrogen and oxygen is consistent\r\nwith the local acceleration theory of Fisk, Kozlovsky, and\r\nRamaty, in which interstellar material is accelerated to several\r\nMeV/nucleon. If, on the other hand, the low energy nitrogen and\r\noxygen result from nucleosynthesis in a galactic source, then the\r\nnucleosynthesis processes which produce an enhancement of nitrogen\r\nand oxygen and a depletion of carbon are restricted to producing\r\npredominantly ^(14)N and ^(16)O.
\r\n", "date": "1975", "date_type": "degree", "id_number": "CaltechTHESIS:10092014-085716916", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10092014-085716916", "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" ] }, "deposited_on": "2014-10-09 16:18:00", "doi": "10.7907/Y2TW-4412", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" }, { "id": "Vogt-R-E", "name": { "family": "Vogt", "given": "Rochus E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1975-05-29", "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. I also retain 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": "Vidor, Solomon Benjamin" }, { "id": "/id/eprint/4279", "eprint_id": 4279, "rev_number": 11, "documents": [ { "id": "/id/document/7021", "doc_id": 7021, "rev_number": 2, "files": [ { "id": "/id/file/42693", "fileid": 42693, "datasetid": "document", "objectid": 7021, "filename": "Brown_jw_1974.pdf", "mime_type": "application/pdf", "filesize": 4137195, "mtime": "2012-12-26 03:07:09", "url": "/4279/1/Brown_jw_1974.pdf" } ], "eprint_id": 4279, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Brown_jw_1974.pdf", "language": "en", "security": "public", "license": "other", "main": "Brown_jw_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/23550" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/23550" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/23550" } ] } }, { "id": "/id/document/23550", "doc_id": 23550, "rev_number": 2, "files": [ { "id": "/id/file/42691", "fileid": 42691, "datasetid": "document", "objectid": 23550, "filename": "preview.png", "mime_type": "image/png", "hash": "1e5382d54389061f319ba546996c42a5", "hash_type": "MD5", "filesize": 9768, "mtime": "2012-12-26 03:07:09", "url": "/4279/2/preview.png" } ], "eprint_id": 4279, "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/7021" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/7021" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/7021" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/42/79", "datestamp": "2005-11-01", "lastmod": "2024-07-19 17:45:33", "status_changed": "2009-09-25 03:15:24", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brown-James-William", "name": { "family": "Brown", "given": "James William" }, "show_email": "NO" } ] }, "title": "A Satellite Measurement of Cosmic-Ray Abundances and Spectra in the Charge Range 2 \u2264 Z \u2264 10", "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 composition of the nuclear component of the cosmic radiation has been under study for some time, because it can yield information concerning the source, propagation, and confinement of cosmic rays within the galaxy. We present here the first comprehensive satellite measurement of cosmic-ray composition and spectra in the charge range 2 <= Z <= 10 using the geomagnetic field as a rigidity analyzer through the entire range of vertical cutoffs. The results indicate that the spectra of all the elements in the observed range are similar, and thus that various ratios of elemental abundances are nearly independent of rigidity over the range 2 <= P <= 15 GV. Calculations of the propagation of cosmic rays through the interstellar and interplanetary media predict that there should be a variation with rigidity of ratios of various elements, because of the charge-dependent effects of ionization of the interstellar gas by the cosmic rays. The absence of this variation can be explained by assuming a rigidity-dependent confinement of the cosmic rays in the galaxy. From the ratios Be/0 and B/0 we obtain a leakage mean free path decreasing from [...] at ~2 GV to [...] at 10-15 GV, assuming that the interstellar gas is composed of hydrogen and helium in a 10:1 ratio. Ratios of other cosmic-ray elements are consistent with such a decreasing path length. The confinement time of the cosmic rays in the galaxy can be estimated from the ratio Be/B, because of the radioactive decay of [...] to [...]. The data indicate a confinement time of [...] years, which may be rigidity-dependent.", "date": "1974", "date_type": "degree", "id_number": "CaltechETD:etd-10282005-124729", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-10282005-124729", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "other_numbering_system": { "items": [ { "id": "1973-02", "name": "Space Radiation Laboratory" } ] }, "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-11-01", "doi": "10.7907/16Z7-5A26", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "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": "1973-06-12", "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": "Brown, James William" }, { "id": "/id/eprint/8697", "eprint_id": 8697, "rev_number": 27, "documents": [ { "id": "/id/document/52603", "doc_id": 52603, "rev_number": 2, "files": [ { "id": "/id/file/152007", "fileid": 152007, "datasetid": "document", "objectid": 52603, "filename": "Garrard_TL_1973.pdf", "mime_type": "application/pdf", "hash": "e22622781e6ce546ba3a1664371c97c7", "hash_type": "MD5", "filesize": 24844344, "mtime": "2014-10-15 17:31:20", "url": "/8697/1/Garrard_TL_1973.pdf" } ], "eprint_id": 8697, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Garrard_TL_1973.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": 51, "dir": "disk0/00/00/86/97", "datestamp": "2014-10-16 23:05:37", "lastmod": "2024-07-16 21:40:29", "status_changed": "2014-10-16 23:05:37", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Garrard-Thomas-Lee", "name": { "family": "Garrard", "given": "Thomas Lee" }, "show_email": "NO" } ] }, "title": "A Quantitative Investigation of the Solar Modulation of Cosmic-Ray Protons and Helium Nuclei", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "The differential energy spectra of cosmic-ray protons and He nuclei have been measured at energies up to 315 MeV/nucleon using balloon- and satellite-borne instruments. These spectra are presented for solar quiet times for the years 1966 through 1970. The data analysis is verified by extensive accelerator calibrations of the detector systems and by calculations and measurements of the production of secondary protons in the atmosphere.
\r\n\r\nThe spectra of protons and He nuclei in this energy range are dominated by the solar modulation of the local interstellar spectra. The transport equation governing this process includes as parameters the solar-wind velocity, V, and a diffusion coefficient, K(r,R), which is assumed to be a scalar function of heliocentric radius, r, and magnetic rigidity, R. The interstellar spectra, jD, enter as boundary conditions on the solutions to the transport equation. Solutions to the transport equation have been calculated for a broad range of assumed values for K(r,R) and jD and have been compared with the measured spectra.
\r\n\r\nIt is found that the solutions may be characterized in terms of a dimensionless parameter, \r\n\u03c8(r,R) = \u221e\u222br V dr'/(K(r',R). \r\nThe amount of modulation is roughly proportional to \u03c8. At high energies or far from the Sun, where the modulation is weak, the solution is determined primarily by the value of \u03c8 (and the interstellar spectrum) and is not sensitive to the radial dependence of the diffusion coefficient. At low energies and for small r, where the effects of adiabatic deceleration are found to be large, the spectra are largely determined by the radial dependence of the diffusion coefficient and are not very sensitive to the magnitude of \u03c8 or to the interstellar spectra. This lack of sensitivity to jD implies that the shape of the spectra at Earth cannot be used to determine the interstellar intensities at low energies.
\r\n\r\nValues of \u03c8 determined from electron data were used to calculate the spectra of protons and He nuclei near Earth. Interstellar spectra of the form jD \u03b1 (W - 0.25m)-2.65 for both protons and He nuclei were found to yield the best fits to the measured spectra for these values of \u03c8, where W is the total energy and m is the rest energy. A simple model for the diffusion coefficient was used in which the radial and rigidity dependence are separable and K is independent of radius inside a modulation region which has a boundary at a distance D. Good agreement was found between the measured and calculated spectra for the years 1965 through 1968, using typical boundary distances of 2.7 and 6.1 A.U. The proton spectra observed in 1969 and 1970 were flatter than in previous years. This flattening could be explained in part by an increase in D, but also seemed to require that a noticeable fraction of the observed protons at energies as high at 50 to 100 MeV be attributed to quiet-time solar emission. The turnup in the spectra at low energies observed in all years was also attributed to solar emission. The diffusion coefficient used to fit the 1965 spectra is in reasonable agreement with that determined from the power spectra of the interplanetary magnetic field (Jokipii and Coleman, 1968). We find a factor of roughly 3 increase in \u03c8 from 1965 to 1970, corresponding to the roughly order of magnitude decrease in the proton intensity at 250 MeV. The change in \u03c8 might be attributed to a decrease in the diffusion coefficient, or, if the diffusion coefficient is essentially unchanged over that period (Mathews et al., 1971), might be\r\nattributed to an increase in the boundary distance, D.
\r\n", "date": "1973", "date_type": "degree", "id_number": "CaltechTHESIS:10152014-102825697", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10152014-102825697", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Traineeship" }, { "agency": "NSF Traineeship" }, { "agency": "NASA", "grant_number": "NGR-05-002-160" }, { "agency": "NASA", "grant_number": "NAS5-9312" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Tony Diaz", "deposited_on": "2014-10-16 23:05:37", "doi": "10.7907/Q0NJ-4D68", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Vogt-R-E", "name": { "family": "Vogt", "given": "Rochus E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1972-06-19", "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": "1973", "author_list": "Garrard, Thomas Lee" }, { "id": "/id/eprint/1652", "eprint_id": 1652, "rev_number": 12, "documents": [ { "id": "/id/document/2585", "doc_id": 2585, "rev_number": 2, "files": [ { "id": "/id/file/15941", "fileid": 15941, "datasetid": "document", "objectid": 2585, "filename": "Cummings_ac_1973.pdf", "mime_type": "application/pdf", "filesize": 9211472, "mtime": "2012-12-26 02:40:12", "url": "/1652/1/Cummings_ac_1973.pdf" } ], "eprint_id": 1652, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Cummings_ac_1973.pdf", "language": "en", "security": "public", "license": "other", "main": "Cummings_ac_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/19324" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19324" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19324" } ] } }, { "id": "/id/document/19324", "doc_id": 19324, "rev_number": 2, "files": [ { "id": "/id/file/15939", "fileid": 15939, "datasetid": "document", "objectid": 19324, "filename": "preview.png", "mime_type": "image/png", "hash": "6496919e875e1400aa7012d98afe1778", "hash_type": "MD5", "filesize": 10621, "mtime": "2012-12-26 02:40:12", "url": "/1652/2/preview.png" } ], "eprint_id": 1652, "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/2585" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2585" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2585" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/16/52", "datestamp": "2005-05-09", "lastmod": "2024-07-16 20:20:11", "status_changed": "2009-09-25 02:10:55", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cummings-Alan-Coffman", "name": { "family": "Cummings", "given": "Alan Coffman" }, "show_email": "NO" } ] }, "title": "A Study of Cosmic-Ray Positron and Electron Spectra in Interplanetary and Interstellar Space and the Solar Modulation of Cosmic Rays", "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 measured the differential energy spectra of cosmic-ray positrons and negatrons with energies between ~11 and 1500 MeV during the period 1968-1971 using a balloon-borne magnetic spectrometer. These measurements fill a gap in the previously existing data and permit us to determine, within quantitative limits, the interstellar spectra of cosmic-ray positrons and electrons [...]. Knowledge of these spectra provides a crucial tool for studies of the distribution and density of matter and magnetic fields in the interstellar medium and the origin and dynamics of energetic particles contained in the fields.\r\n\r\nFrom a study of the near-Earth electron spectra and their relationship to the interstellar spectrum derived from the galactic non-thermal-radio-background emission, and from a study of the near-Earth positron spectra and their relationship to the interstellar positron spectrum calculated from collisions of cosmic-ray nuclei with the interstellar matter, we have found that the differential energy spectrum of interstellar electrons may be represented as a power-law, [...] for 100 MeV [...] GeV, but must flatten considerably at lower energies. From the measured electron charge composition, which we find to be little affected by solar modulation, we have concluded that the majority of cosmic-ray electrons with energies above ~10 MeV are not the result of nuclear collisions in the galaxy but presumably originate in \"primary\" sources.\r\n\r\nIn the energy range of our measurements the near-Earth intensities of cosmic-ray positrons and electrons, as well as the intensity of cosmic-ray nuclei, are significantly lower than their interstellar intensities because the particles are scattered by magnetic irregularities imbedded in the outward-flowing plasma of the solar wind. Long-term changes in the scattering properties of the interplanetary medium, i.e. in the cosmic-ray diffusion coefficient, [...], are responsible for the observed long-term variations in the near-Earth cosmic-ray intensities which are as large as a factor of 10 from \"solar minimum\" to \"solar maximum\". We have used the cosmic-ray positron and electron spectra as tools to study the solar modulation mechanism. By using numerical solutions of the cosmic-ray transport equation to relate the near-Earth electron spectra to the interstellar electron spectrum, we have found that the magnetic rigidity dependence of the interplanetary cosmic-ray diffusion coefficient at rigidities from ~100 MV to ~10 GV may be represented as [...] with b increasing from 0 to ~1-2 with increasing rigidity. However, from a comparison of the near-Earth and interstellar positron spectra we find that below ~60 MV the diffusion coefficient must increase with decreasing rigidity.\r\n\r\nThe magnitude of the diffusion coefficient at 1 AU derived from the electron and positron modulation studies depends on the assumed radial dependence of [...]. In order to place limits on this radial dependence and to make estimates of the size of the solar modulation region, we have also evaluated diffusion coefficients from measurements of the power spectrum of the interplanetary magnetic field near 1 AU. Assuming [...], we have found that [...] in order that the calculated modulation beyond 1 AU agrees with the observed modulation. For K independent of radius, we obtained consistency between the diffusion coefficients derived by the two methods for boundary distances of the solar modulation region in the range of 6-25 AU.\r\n\r\nThese diffusion coefficients derived from the electron modulation study must also apply to the cosmic-ray nuclei. As a consistency check, we have used the electron diffusion coefficients to calculate solutions of the transport equation for cosmic-ray protons and He nuclei for four different time periods from 1965 to 1970. Assuming a particular, time-independent form for the interstellar spectra of these particles, we have derived spectra at l AU which are consistent with the observations over the full range of intensity variations observed during this solar half cycle.", "date": "1973", "date_type": "degree", "id_number": "CaltechETD:etd-05062005-131722", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05062005-131722", "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" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-05-09", "doi": "10.7907/HM9B-QK62", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Vogt-R-E", "name": { "family": "Vogt", "given": "Rochus E." }, "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-05-06", "thesis_defense_date": "1973-03-26", "thesis_approved_date": "2005-05-09", "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": "Cummings, Alan Coffman" }, { "id": "/id/eprint/8691", "eprint_id": 8691, "rev_number": 19, "documents": [ { "id": "/id/document/52577", "doc_id": 52577, "rev_number": 4, "files": [ { "id": "/id/file/151928", "fileid": 151928, "datasetid": "document", "objectid": 52577, "filename": "Evans_LC_1972.pdf", "mime_type": "application/pdf", "hash": "f49b16bafc7ef09c6199a7304a30a304", "hash_type": "MD5", "filesize": 28147553, "mtime": "2014-10-13 21:59:19", "url": "/8691/1/Evans_LC_1972.pdf" } ], "eprint_id": 8691, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Evans_LC_1972.pdf", "media_duration": "0", "media_aspect_ratio": "0", "media_sample_start": "0", "media_sample_stop": "0", "content": "final" }, { "id": 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635, "dir": "disk0/00/00/86/91", "datestamp": "2014-10-14 16:51:33", "lastmod": "2024-07-01 16:44:31", "status_changed": "2014-10-14 16:51:33", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Evans-Lawrence-Curtis", "name": { "family": "Evans", "given": "Lawrence Curtis" }, "show_email": "NO" } ] }, "title": "Magnetospheric Access of Solar Particles and the Configuration of the Distant Geomagnetic Field", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics, Geophysics, Applied Mathematics and Business\r\nEconomics)", "abstract": "The access of 1.2-40 MeV protons and 0.4-1.0 MeV electrons from\r\ninterplanetary space to the polar cap regions has been investigated with\r\nan experiment on board a low altitude, polar orbiting satellite (OG0-4).
\r\nA total of 333 quiet time observations of the electron polar cap\r\nboundary give a mapping of the boundary between open and closed geomagnetic\r\nfield lines which is an order of magnitude more comprehensive than\r\npreviously available.
\r\n\r\nPersistent features (north/south asymmetries) in the polar cap proton\r\nflux, which are established as normal during solar proton events,\r\nare shown to be associated with different flux levels on open geomagnetic\r\nfield lines than on closed field lines. The pole in which these persistent\r\nfeatures are observed is strongly correlated to the sector structure\r\nof the interplanetary magnetic field and uncorrelated to the north/south\r\ncomponent of this field. The features were observed in the north (south)\r\npole during a negative (positive) sector 91% of the time, while the\r\nsolar field had a southward component only 54% of the time. In addition,\r\nchanges in the north/south component have no observable effect on the\r\npersistent features.
\r\n\r\nObservations of events associated with co-rotating regions of enhanced\r\nproton flux in interplanetary space are used to establish the\r\ncharacteristics of the 1.2 - 40 MeV proton access windows: the access window\r\nfor low polar latitudes is near the earth, that for one high polar\r\nlatitude region is ~250 R\u2295 behind the earth, while that for the other\r\nhigh polar latitude region is ~1750 R\u2295 behind the earth. All of the\r\naccess windows are of approximately the same extent (~120 R\u2295). The following\r\nphenomena contribute to persistent polar cap features: limited\r\ninterplanetary regions of enhanced flux propagating past the earth,\r\nradial gradients in the interplanetary flux, and anisotropies in the\r\ninterplanetary flux.
\r\n\r\nThese results are compared to the particle access predictions of\r\nthe distant geomagnetic tail configurations proposed by Michel and Dessler,\r\nDungey, and Frank. The data are consistent with neither the model of\r\nMichel and Dessler nor that of Dungey. The model of Frank can yield a\r\nconsistent access window configuration provided the following constraints\r\nare satisfied: the merging rate for open field lines at one polar neutral\r\npoint must be ~5 times that at the other polar neutral point, related\r\nto the solar magnetic field configuration in a consistent fashion,\r\nthe migration time for open field lines to move across the polar cap\r\nregion must be the same in both poles, and the open field line merging\r\nrate at one of the polar neutral points must be at least as large as\r\nthat required for almost all the open field lines to have merged in\r\n0 (one hour). The possibility of satisfying these constraints is investigated\r\nin some detail.
\r\n\r\nThe role played by interplanetary anisotropies in the observation\r\nof persistent polar cap features is discussed. Special emphasis is given\r\nto the problem of non-adiabatic particle entry through regions where the\r\nmagnetic field is changing direction. The degree to which such particle\r\nentry can be assumed to be nearly adiabatic is related to the particle\r\nrigidity, the angle through which the field turns, and the rate at which\r\nthe field changes direction; this relationship is established for the\r\ncase of polar cap observations.
\r\n", "date": "1972", "date_type": "degree", "id_number": "CaltechTHESIS:10132014-144759243", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:10132014-144759243", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAS 5-3095" }, { "agency": "NASA", "grant_number": "NGL 05-002-007" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Ignis Nguyen", "deposited_on": "2014-10-14 16:51:33", "doi": "10.7907/vzsp-g414", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1971-09-22", "review_status": "approved", "option_major": { "items": [ "physics" ] }, "option_minor": { "items": [ "appmath", "busecon", "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": "1972", "author_list": "Evans, Lawrence Curtis" }, { "id": "/id/eprint/9707", "eprint_id": 9707, "rev_number": 23, "documents": [ { "id": "/id/document/66071", "doc_id": 66071, "rev_number": 2, "files": [ { "id": "/id/file/183974", "fileid": 183974, "datasetid": "document", "objectid": 66071, "filename": "Lupton_je_1972.pdf", "mime_type": "application/pdf", "hash": "47031eb0391b25d4fe488767a1f6b78b", "hash_type": "MD5", "filesize": 45502833, "mtime": "2016-05-09 17:58:11", "url": "/9707/1/Lupton_je_1972.pdf" } ], "eprint_id": 9707, "pos": 1, "placement": 1, "mime_type": "application/pdf", "format": "application/pdf", "language": "en", "security": "public", "license": "other", "main": "Lupton_je_1972.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": 10575, "dir": "disk0/00/00/97/07", "datestamp": "2016-05-09 18:41:28", "lastmod": "2024-07-01 22:05:22", "status_changed": "2016-05-09 18:41:28", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lupton-John-Edward", "name": { "family": "Lupton", "given": "John Edward" }, "show_email": "NO" } ] }, "title": "Solar Flare Particle Propagation: Comparison of a New Analytical Solution with Spacecraft Measurements", "ispublished": "unpub", "full_text_status": "public", "keywords": "(Physics)", "abstract": "A new analytic solution has been obtained to the complete Fokker-Planck equation for solar flare particle propagation including the effects of convection, energy-change, corotation, and diffusion with \u0138r = constant and \u0138\u019f \u221d r2. It is assumed that the particles are injected impulsively at a single point in space, and that a boundary exists beyond which the particles are free to escape. Several solar flare particle events have been observed with the Caltech Solar and Galactic Cosmic Ray Experiment aboard OGO-6. Detailed comparisons of the predictions of the new solution with these observations of 1-70 MeV protons show that the model adequately describes both the rise and decay times, indicating that \u0138r = constant is a better description of conditions inside 1 AU than is \u0138r \u221d r. With an outer boundary at 2.7 AU, a solar wind velocity of 400 km/sec, and a radial diffusion coefficient \u0138r \u2248 2-8 x 1020 cm2/sec, the model gives reasonable fits to the time-profile of 1-10 MeV protons from \"classical\" flare-associated events. It is not necessary to invoke a scatter-free region near the sun in order to reproduce the fast rise times observed for directly-connected events. The new solution also yields a time-evolution for the vector anisotropy which agrees well with previously reported observations.
\r\n\r\nIn addition, the new solution predicts that, during the decay phase, a typical convex spectral feature initially at energy To will move to lower energies at an exponential rate given by TKINK = Toexp(-t/\u01acKINK). Assuming adiabatic deceleration and a boundary at 2.7 AU, the solution yields \u01acKINK \u2248 100h, which is faster than the measured ~200h time constant and slower than the adiabatic rate of ~78h at 1 AU. Two possible explanations are that the boundary is at ~5 AU or that some other energy-change process is operative.
\r\n", "date": "1972", "date_type": "degree", "id_number": "CaltechTHESIS:05092016-095858999", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechTHESIS:05092016-095858999", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NDEA" }, { "agency": "NASA" }, { "agency": "NASA", "grant_number": "NAS5-9312" }, { "agency": "NASA", "grant_number": "NGR-05-002-160" }, { "agency": "NASA", "grant_number": "NGL-05-002-007" } ] }, "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_on": "2016-05-09 18:41:28", "doi": "10.7907/RP79-C621", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_defense_date": "1971-12-02", "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": "1972", "author_list": "Lupton, John Edward" }, { "id": "/id/eprint/1752", "eprint_id": 1752, "rev_number": 13, "documents": [ { "id": "/id/document/2844", "doc_id": 2844, "rev_number": 2, "files": [ { "id": "/id/file/17321", "fileid": 17321, "datasetid": "document", "objectid": 2844, "filename": "Murray_ss_1971.pdf", "mime_type": "application/pdf", "filesize": 5258391, "mtime": "2012-12-26 02:41:38", "url": "/1752/1/Murray_ss_1971.pdf" } ], "eprint_id": 1752, "pos": 1, "mime_type": "application/pdf", "format": "application/pdf", "format_desc": "Murray_ss_1971.pdf", "language": "en", "security": "public", "license": "other", "main": "Murray_ss_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/19568" }, { "type": "http://eprints.org/relation/haspreviewThumbnailVersion", "uri": "/id/document/19568" }, { "type": "http://eprints.org/relation/hasVersion", "uri": "/id/document/19568" } ] } }, { "id": "/id/document/19568", "doc_id": 19568, "rev_number": 2, "files": [ { "id": "/id/file/17319", "fileid": 17319, "datasetid": "document", "objectid": 19568, "filename": "preview.png", "mime_type": "image/png", "hash": "a1c8a71b7d363f80987cbfac036a815c", "hash_type": "MD5", "filesize": 6794, "mtime": "2012-12-26 02:41:38", "url": "/1752/2/preview.png" } ], "eprint_id": 1752, "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/2844" }, { "type": "http://eprints.org/relation/ispreviewThumbnailVersionOf", "uri": "/id/document/2844" }, { "type": "http://eprints.org/relation/isVersionOf", "uri": "/id/document/2844" } ] } } ], "eprint_status": "archive", "userid": 2, "dir": "disk0/00/00/17/52", "datestamp": "2005-05-13", "lastmod": "2024-06-24 20:16:42", "status_changed": "2009-09-25 02:14:36", "type": "thesis", "metadata_visibility": "show", "creators": { "items": [ { "id": "Murray-Stephen-S", "name": { "family": "Murray", "given": "Stephen S." }, "show_email": "NO" } ] }, "title": "Propagation of 1-10 MeV Solar Flare Protons in Interplanetary Space", "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\nObservations of 1-10 MeV solar flare protons associated with the 7 June 1969 solar event are used in an investigation of the physical processes affecting particle propagation in interplanetary space. The observations were made with the Caltech Solar and Galactic Cosmic Ray Experiment on board OGO-VI, a low altitude polar orbiting satellite. We find during the decay of the event that the physical processes of diffusion, convection and energy change must all be considered to obtain satisfactory agreement between the observations and theoretical predictions. In particular we find that for this event, there is clear evidence for energy change processes occurring in interplanetary space. We find in fact that the observed energy change is not simply due to adiabatic deceleration in a uniformly expanding solar wind. We also find that during the decay of this event the effects of diffusion are consistent with an energy independent diffusion coefficient [...] for 1-10 MeV with a value of approximately 5 x [...].", "date": "1971", "date_type": "degree", "id_number": "CaltechETD:etd-05122005-142607", "refereed": "FALSE", "official_url": "https://resolver.caltech.edu/CaltechETD:etd-05122005-142607", "projects": { "items": [ "OGO54 GRANT48 GRANT" ] }, "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "collection": "CaltechTHESIS", "reviewer": "Kathy Johnson", "other_numbering_system": { "items": [ { "id": "1970-01", "name": "Space Radiation Laboratory" } ] }, "local_group": { "items": [ "Space Radiation Laboratory" ] }, "deposited_by": "Imported from ETD-db", "deposited_on": "2005-05-13", "doi": "10.7907/0752-B996", "divisions": { "items": [ "div_pma" ] }, "institution": "California Institute of Technology", "thesis_type": "phd", "thesis_advisor": { "items": [ { "id": "Stone-E-C", "name": { "family": "Stone", "given": "Edward C." }, "orcid": "0000-0002-2010-5462", "role": "advisor" } ] }, "thesis_committee": { "items": [ { "name": { "family": "Unknown", "given": "Unknown" } } ] }, "thesis_degree": "PHD", "thesis_degree_grantor": "California Institute of Technology", "thesis_submitted_date": "2005-05-12", "thesis_defense_date": "1970-12-28", "thesis_approved_date": "2005-05-13", "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": "1971", "author_list": "Murray, Stephen S." } ]