[ { "id": "authors:se7fn-5j718", "collection": "authors", "collection_id": "se7fn-5j718", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141022-162035331", "type": "book_section", "title": "An Experiment to Measure the Elemental Abundances of Ultra-Heavy Cosmic Rays", "author": [ { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Hink", "given_name": "P. L.", "clpid": "Hink-P-L" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Mewaldt", "given_name": "R. A.", "orcid": "0000-0003-2178-9111", "clpid": "Mewaldt-R-A" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Leske", "given_name": "R. A.", "orcid": "0000-0002-0156-2414", "clpid": "Leske-R-A" }, { "family_name": "Schindler", "given_name": "R. H.", "clpid": "Schindler-R-H" }, { "family_name": "Wiedenbeck", "given_name": "M. E.", "orcid": "0000-0002-2825-3128", "clpid": "Wiedenbeck-M-E" }, { "family_name": "Streitmatter", "given_name": "R. E.", "clpid": "Streitmatter-R-E" }, { "family_name": "Barbier", "given_name": "L. M.", "clpid": "Barbier-L-M" }, { "family_name": "Christian", "given_name": "E. R.", "orcid": "0000-0003-2134-3937", "clpid": "Christian-E-R" }, { "family_name": "Mitchell", "given_name": "J. W.", "clpid": "Mitchell-J-W" }, { "family_name": "Ormes", "given_name": "J. F.", "clpid": "Ormes-J-F" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Potgieter", "given_name": "M. S.", "clpid": "Potgieter-M-S" }, { "family_name": "Raubenheimer", "given_name": "C.", "clpid": "Raubenheimer-C" }, { "family_name": "van der Walt", "given_name": "D. J.", "clpid": "van-der-Walt-D-J" } ], "abstract": "Measurements of the elemental abundances of galactic cosmic ray nuclei with charge 26\u2264z\u226492 can provide important information that should help to resolve the question of cosmic-ray origin; i.e. whether cosmic rays originate from the acceleration of interstellar grain material or from preferential selection and acceleration of nuclei from stellar photosphere-chromosphere regions with T-10^4\nbased on first ionization potential. They will also refine tests of whether freshly synthesized rprocess material is a significant component in cosmic rays. The detector concept described utilizes an array of silicon detectors for dF/dx measurements, two Cherenkov counters with radiators of\ndifferent refractive index for velocity determination (one using aerogel and one using a novel waveshifter readout approach), and scintillating fibers for a hodoscope/time-of-flight detector. The numbers of particles which can be collected with this approach and the expected charge resolution are discussed.", "publisher": "Potchefstroom University, Space Research Unit", "publication_date": "1997" }, { "id": "authors:9194s-nqv11", "collection": "authors", "collection_id": "9194s-nqv11", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140717-163218909", "type": "book_section", "title": "The Advanced Composition Explorer Mission", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Christian", "given_name": "E. R.", "orcid": "0000-0003-2134-3937", "clpid": "Christian-E-R" }, { "family_name": "Mewaldt", "given_name": "R. A.", "orcid": "0000-0003-2178-9111", "clpid": "Mewaldt-R-A" }, { "family_name": "Ormes", "given_name": "J. F.", "clpid": "Ormes-J-F" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "contributor": [ { "family_name": "Potgeiter", "given_name": "M. S.", "clpid": "Potgeiter-M-S" } ], "abstract": "The Advanced Composition Explorer, to be launched in August of 1997, will include six high\nresolution spectrometers that will measure the composition of interplanetary nuclei with 2\u2264Z\u226428 from < 1 keV/nuc to ~500 MeV/nuc. Three additional instruments will provide the interplanetary context for these measurements. We give a brief introduction to the ACE mission, its\ninstrumentation, and its goals.", "publisher": "Potchefstroom University, Space Research Unit", "publication_date": "1997" }, { "id": "authors:9aefz-ren60", "collection": "authors", "collection_id": "9aefz-ren60", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140717-154827635", "type": "book_section", "title": "Propagation of the Heaviest UH-Cosmic Ray Nuclei", "author": [ { "family_name": "Waddington", "given_name": "I.", "clpid": "Waddington-I" }, { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Hink", "given_name": "P.", "clpid": "Hink-P-L" }, { "family_name": "Nilsen", "given_name": "B. S.", "clpid": "Nilsen-B-S" } ], "contributor": [ { "family_name": "Potgieter", "given_name": "M. S.", "clpid": "Potgieter-M-S" } ], "abstract": "Our previous studies showed that the fragmentation cross sections of gold nuclei interacting in\nhydrogen have large variations between the values measured at 0.9 and 10.6 GeV/n, which has very\nsignificant implications on calculations of the propagation of the heaviest UH cosmic ray nuclei,\nsuch as Pb and Pt We have now completed a series of runs at the Brookhaven AGS using beams of\ngold nuclei of intermediate energy. The data from these runs will allow us to establish the excitation\nfunctions for these cross sections in a wide range of targets and hence model propagation more\naccurately than hitherto. In addition we will be able to study the energy dependence of nuclear\ncharge pickup, electromagnetic dissociation and fission. Beams of gold nuclei with seven energies\nbetween 4.0 and 0.9 Ge V /n were studied interacting in targets ranging in mass from hydrogen to lead. We will present data on the cross sections derived from several of these beams and discuss\nsome of the implications.", "publisher": "Potchefstroom University, Space Research Unit", "publication_date": "1997" }, { "id": "authors:e5bf7-vdp80", "collection": "authors", "collection_id": "e5bf7-vdp80", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140717-162349735", "type": "book_section", "title": "The Response of Particle Detectors to Gold Nuclei at 11 GeV/nucleon", "author": [ { "family_name": "Wiedenbeck", "given_name": "M. E.", "orcid": "0000-0002-2825-3128", "clpid": "Wiedenbeck-M-E" }, { "family_name": "Barbier", "given_name": "L. M.", "clpid": "Barbier-L-M" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Christian", "given_name": "E. R.", "orcid": "0000-0003-2134-3937", "clpid": "Christian-E-R" }, { "family_name": "Dougherty", "given_name": "B. L.", "clpid": "Dougherty-B-L" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Hink", "given_name": "P. L.", "clpid": "Hink-P-L" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Leske", "given_name": "R. A.", "orcid": "0000-0002-0156-2414", "clpid": "Leske-R-A" }, { "family_name": "Mewaldt", "given_name": "R. A.", "orcid": "0000-0003-2178-9111", "clpid": "Mewaldt-R-A" }, { "family_name": "Mitchell", "given_name": "J. W.", "clpid": "Mitchell-J-W" }, { "family_name": "Sposato", "given_name": "S. H.", "clpid": "Sposato-S-H" }, { "family_name": "Streitmatter", "given_name": "R. E.", "clpid": "Streitmatter-R-E" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Potgieter", "given_name": "M. S.", "clpid": "Potgieter-M-S" } ], "abstract": "A set of particle detectors has been exposed to beams of _(79)Au nuclei at ~ 11 Ge V /nucleon from\nthe Alternating Gradient Synchrotron (AGS) at Brookhaven National Laboratory (BNL). We report\npreliminary results on the responses obtained from silicon solid state detectors and from Cerenkov\ncounters utilizing total internal reflection with waveshifter bars for readout.", "publisher": "Potchefstroom University, Space Research Unit", "publication_date": "1997" }, { "id": "authors:80rzg-crx66", "collection": "authors", "collection_id": "80rzg-crx66", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141022-162931350", "type": "book_section", "title": "A Science Center for the Advanced Composition Explorer", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Hammond", "given_name": "J. S.", "clpid": "Hammond-J-S" } ], "contributor": [ { "family_name": "Potgieter", "given_name": "M. S.", "clpid": "Potgieter-M-S" }, { "family_name": "Raubenheimer", "given_name": "C.", "clpid": "Raubenheimer-C" }, { "family_name": "van der Walt", "given_name": "D. J.", "clpid": "van-der-Walt-D-J" } ], "abstract": "The Advanced Composition Explorer (ACE) mission is supported by an ACE Science Center for the purposes of facilitating collaborative work. It is intended that coordinated use of a centralized science facility by the ACE team will ensure appropriate use of data formatting standards, thus easing access to the data; will improve communications within and to the ACE science working team; and will reduce redundant effort in data processing.", "publisher": "Potchefstroom University, Space Research Unit", "publication_date": "1997" }, { "id": "authors:r13c0-cn125", "collection": "authors", "collection_id": "r13c0-cn125", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-221959133", "type": "book_section", "title": "Enhancing the ACE Control Center for the Multiple uses of Spacecraft Integration and Test and Mission and Science Operations", "author": [ { "family_name": "Snow", "given_name": "Frank", "clpid": "Snow-F" }, { "family_name": "Garrard", "given_name": "Thomas L.", "clpid": "Garrard-T-L" }, { "family_name": "Steck", "given_name": "Jane A.", "clpid": "Steck-J-A" }, { "family_name": "Maury", "given_name": "Jesse L.", "clpid": "Maury-J-L" } ], "contributor": [ { "family_name": "Guyenne", "given_name": "T.-D.", "clpid": "Guyenne-T-D" } ], "abstract": "NASA, at the direction of its Administrator, is undertaking a grand challenge of change for \"faster, better, cheaper; strong emphasis is now being placed on staying within cost\nprojections while still meeting schedule and performance goals. This led NASA to mandate fixed-price, capped-cost programs. The Advanced Composition Explorer (ACE) is the first mission to be funded in this manner. Consequently, the ACE Project has sought novel approaches and techniques to constrain costs without compromising schedule or science goals. A key approach that has been adopted is novel, multiple reusage of the ACE control center subsystem.\n\nACE will use a version of the Transportable Payload Operations Control Center (TPOCC) for its mission operations. It was determined in Phase 8 of the ACE Project that a potential existed for substantial savings if the adaptation of the TPOCC for ACE Mission Operations could include adapting it as well for use as the primary component in the Ground Support Equipment for\nIntegration and Testing of the ACE Spacecraft and, at the same time, also adapting it be the basic component in the ACE Science Center; thus, realizing three separate uses for essentially the same system. Implementing this approach required enhancing the TPOCC requirements, significant\nchanges in its development schedule, and changes in the allocation and activities of personnel responsible for development of ACE operations. This paper discusses how these issues were addressed, the unforeseen problems that have been encountered, how these problems have been\nresolved, and an evaluation of what this approach portends for application to future missions.", "publisher": "European Space Agency", "publication_date": "1996-09" }, { "id": "authors:vkz17-wk666", "collection": "authors", "collection_id": "vkz17-wk666", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140703-222609991", "type": "book_section", "title": "ENergetic Trans-Iron Composition Explorer (ENTICE): A mission concept", "author": [ { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Hink", "given_name": "P. L.", "clpid": "Hink-P-L" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Leske", "given_name": "R. A.", "orcid": "0000-0002-0156-2414", "clpid": "Leske-R-A" }, { "family_name": "Mewaldt", "given_name": "R. A.", "orcid": "0000-0003-2178-9111", "clpid": "Mewaldt-R-A" }, { "family_name": "Schindler", "given_name": "S. M.", "clpid": "Schindler-S-M" }, { "family_name": "Barbier", "given_name": "L. M.", "clpid": "Barbier-L-M" }, { "family_name": "Christian", "given_name": "E. R.", "orcid": "0000-0003-2134-3937", "clpid": "Christian-E-R" }, { "family_name": "Mitchell", "given_name": "J. W.", "clpid": "Mitchell-J-W" }, { "family_name": "Ormes", "given_name": "J. R.", "clpid": "Ormes-J-R" }, { "family_name": "Streitmatter", "given_name": "R. E.", "clpid": "Streitmatter-R-E" }, { "family_name": "Wiedenbeck", "given_name": "M. E.", "orcid": "0000-0002-2825-3128", "clpid": "Wiedenbeck-M-E" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Ramsey", "given_name": "B. D.", "clpid": "Ramsey-B-D" }, { "family_name": "Parnell", "given_name": "T. A.", "clpid": "Parnell-T-A" } ], "abstract": "We describe a mission concept which has as its primary objective the measurement of the elemental abundances of galactic and solar energetic nuclei over the charge range of 14 less than or equal to Z less than or equal to 92. The instruments would have sufficient collecting power to improve the number of particles collected over that of previous measurements by more than an order of magnitude and, more important, will have the capability to clearly distinguish individual elements. These measurements are of fundamental importance to an understanding of the origin, nucleosynthesis, and acceleration of energetic galactic and solar particles.", "doi": "10.1117/12.253969", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "publication_date": "1996" }, { "id": "authors:34cwm-f6a32", "collection": "authors", "collection_id": "34cwm-f6a32", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140619-144509681", "type": "book_section", "title": "Nuclear Interaction Cross Sections for UltraHeavy Nuclei", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "family_name": "Geer", "given_name": "L. Y.", "clpid": "Geer-L-Y" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Nilsen", "given_name": "B. S.", "clpid": "Nilsen-B-S" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "abstract": "We summarize additions to our data base of charge-changing cross\nsections for relativistic ultraheavy nuclei interacting in targets ranging\nfrom H to Pb. We have improved parametric fits to those cross sections\nas functions of energy and of projectile, target, and fragment charge. At\nhigh energies, we have determined cross sections for Au projectiles at 10.6\nGeV /nucleon in targets of H, CH_2, C, Al, Cu, Sn, and Pb. Compared\nwith cross sections at 1 GeV /n, fragment production is substantially\nchanged, especially for the H target. These changes have important implications\nfor calculations of interstellar propagation of ultraheavy nuclei.\nAt lower energies, we have added Kr and Ag to our list of projectiles.\nAnalysis of these data has led to a better understanding of the systematics\nof these cross sections, hence more physically meaningful parameterizations\nfor fragmentation at high energies and for charge pickup.", "publisher": "International Union of Pure and Applied Physics", "publication_date": "1995" }, { "id": "authors:96x3m-djr05", "collection": "authors", "collection_id": "96x3m-djr05", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-144700326", "type": "book_section", "title": "Composition of energetic particles from solar flares", "book_title": "Life sciences and space research XXV (2): radiation biology", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "contributor": [ { "family_name": "Horneck", "given_name": "G.", "clpid": "Horneck-G" } ], "abstract": "We present a model for composition of heavy ions in the solar energetic particles (SEP). The SEP composition in a typical large solar particle event reflects the composition of the Sun, with adjustments due to fractionation effects which depend on the first ionization potential (FIP) of the ion and on the ratio of ionic charge to mass (Q/M). Flare-to-flare variations in composition are represented by parameters describing these fractionation effects and the distributions of these parameters are presented.", "doi": "10.1016/0273-1177(94)90514-2", "isbn": "0-08-042487-2", "publisher": "Pergamon Press", "place_of_publication": "Oxford", "publication_date": "1994-10", "pages": "589-598" }, { "id": "authors:62qfx-zte83", "collection": "authors", "collection_id": "62qfx-zte83", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140520-111256410", "type": "book_section", "title": "TENNIS: A Standard for Data Formatting, Input, and Output", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" } ], "abstract": "A technique for documenting, formatting, and storing data is introduced and briefly described. The documentation standard, now labeled the tennis standard, allows creation of function libraries and utilities to gain access to the data, greatly facilitating input and output; these functions and utilities are described. A comparison of this standard with the better known HDF and CDF standards is made.", "doi": "10.1063/1.44476", "publisher": "American Instittue of Physics", "publication_date": "1993-08-01" }, { "id": "authors:wfgda-emk59", "collection": "authors", "collection_id": "wfgda-emk59", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-100928259", "type": "book_section", "title": "New SEP-Based Solar Abundances", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "contributor": [ { "family_name": "Leahy", "given_name": "D. A.", "clpid": "Leahy-D-A" }, { "family_name": "Hickws", "given_name": "R. B.", "clpid": "Hickws-R-B" }, { "family_name": "Venkatesan", "given_name": "D.", "clpid": "Venkatesan-D" } ], "abstract": "The relative abundances of various elements in the solar photosphere and\nthe solar corona are re-determined from relative abundances of solar\nenergetic particles (SEP) in the light of revised solar spectroscopic\nabundances. We find excellent correlation between SEP-based\nabundances and spectroscopic abundances, after correcting for\nfractionation due to ionic charge-to-mass ratio and first ionization\npotential.", "publisher": "University of Calgary", "publication_date": "1993-07" }, { "id": "authors:nmm7v-ref30", "collection": "authors", "collection_id": "nmm7v-ref30", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141021-163711864", "type": "book_section", "title": "Energy Dependence of the Fragmentation of UH-Nuclei", "author": [ { "family_name": "Geer", "given_name": "L. Y.", "clpid": "Geer-L-Y" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Nilsen", "given_name": "B. S.", "clpid": "Nilsen-B-S" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" } ], "contributor": [ { "family_name": "Leahy", "given_name": "D. A.", "clpid": "Leahy-D-A" }, { "family_name": "Hickws", "given_name": "R. B.", "clpid": "Hickws-R-B" }, { "family_name": "Venkatesan", "given_name": "D.", "clpid": "Venkatesan-D" } ], "abstract": "The fragmentation of 10.6 GeV/n Au in CH_2. C, Al, Cu, Sn, and Pb targets has been studied using an array of ion chambers, multi-wire proportional counters (MWPC), \nand Cherenkov counters. Total charge-changing cross sections were found to be monotonically increasing with target charge over cross sections measured and\nderived from lower energy data. Partial charge-changing cross sections yielding charge changes less than 1O were depressed from those measured at lower energy.", "publisher": "World Scientific", "publication_date": "1993" }, { "id": "authors:3jm4g-wtn89", "collection": "authors", "collection_id": "3jm4g-wtn89", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141022-094729368", "type": "book_section", "title": "Fragmentation of Relativistic Krypton and Silver Nuclei", "author": [ { "family_name": "Nilsen", "given_name": "B. S.", "clpid": "Nilsen-B-S" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" } ], "contributor": [ { "family_name": "Leahy", "given_name": "D. A.", "clpid": "Leahy-D-A" }, { "family_name": "Hickws", "given_name": "R. B.", "clpid": "Hickws-R-B" }, { "family_name": "Venkatesan", "given_name": "D.", "clpid": "Venkatesan-D" } ], "abstract": "In 1990 we exposed a wide range of targets to beams of relativistic krypton and silver nuclei at the LBL Bevalac at energies from 0.5 to 1.5 GeV/nucleon. Incoming and fragmented nuclei were detected in an array of ion chambers,\nCherenkov detectors, and multiwire proportional chambers. The total and partial cross sections for charge-changing interactions have been measured, with emphasis on those of cosmic ray interest. These cross sections are compared to those from parametric fits.", "publisher": "World Scientific", "publication_date": "1993" }, { "id": "authors:jsgbj-fha39", "collection": "authors", "collection_id": "jsgbj-fha39", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141007-135031932", "type": "book_section", "title": "UHCR: A Cosmic Ray Mission to Study Nuclei in the Charge Range From 20 \u2264Z \u2264100", "author": [ { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Geer", "given_name": "L. Y.", "clpid": "Geer-L-Y" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Mewaldt", "given_name": "R. A.", "orcid": "0000-0003-2178-9111", "clpid": "Mewaldt-R-A" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "abstract": "A definitive study of the elemental abundances of nuclei over the charge range of 20 \u2264 Z \u2264 100 requires a satellite mission capable of obtaining high statistics and excellent charge resolution over the full charge range. Such a mission, utilizing an electronic instrument which is an evolution of the HEA0-3 Heavy Nuclei Experiment, is described here.", "publisher": "International Union of Pure and Applied Physics", "publication_date": "1991" }, { "id": "authors:1rqq6-j2a97", "collection": "authors", "collection_id": "1rqq6-j2a97", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141007-110101824", "type": "book_section", "title": "Fragmentation of UH Nuclei", "author": [ { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Nilsen", "given_name": "B. S.", "clpid": "Nilsen-B-S" } ], "abstract": "We have measured the total charge changing cross sections as a function of energy for projectile _(36)Kr nuclei in a wide range of targets ranging from polyethylene to lead. These cross sections are energy dependent and the dependence increases as the target mass increases.", "publisher": "International Union of Pure and Applied Physics", "publication_date": "1991" }, { "id": "authors:dy7km-tp355", "collection": "authors", "collection_id": "dy7km-tp355", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140924-110740661", "type": "book_section", "title": "Heavy Ions in the October 1989 Solar Flares Observed on the Galileo Spacecraft", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "abstract": "Composition measurements were made of the energetic\nparticles produced in the series of large flares which began on 19 October 1989, using the Galileo Heavy Ion Counter which is sensitive to nuclei ranging from carbon (Z=6) to nickel (Z=28) over an energy range from about 5 MeV/nucleon to >70 MeV/nucleon. The observations are unique in that clean, statistically well-measured abundances are available for heavy ions for an unusually large flare. For elements with low First Ionization Potential (FIP), these results show the same correlation of relative abundances\nwith the ion charge to mass ratio as the earlier Voyager observations of solar energetic particles 1 . After correction for selection on the basis of this charge to mass ratio, the abundances of all the elements measured\nshow the expected step-function correlation with FIP, when compared to the spectroscopic photspheric abundances.", "publisher": "Institute for Advanced Studies", "publication_date": "1991" }, { "id": "authors:khmgq-ttx14", "collection": "authors", "collection_id": "khmgq-ttx14", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141007-134028845", "type": "book_section", "title": "Response of Scintillators to UH Nuclei", "author": [ { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Nilsen", "given_name": "B. S.", "clpid": "Nilsen-B-S" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "abstract": "In order to evaluate the performance of plastic scintillators for the detection\nof Ultra-Heavy cosmic ray nuclei, as envisaged in paper OG 10.1.14P,\nwe have conducted experiments at the LBL Bevalac in which we exposed\nNE-114 and acrylic scintillators to beams of 47Ag ions and its interaction\nfragments. As a result we have calibrated these scintillators over the charge\nrange 31 \u2264 Z \u2264 47. Our results show that a combination of Cherenkov and\nscintillator detectors can resolve individual charges over this charge range.\nThe resolution obtained in scintillator was 0.24 and 0.28 cu for NE-114 and\nacrylic scintillator respectively. In addition the light emission is shown to be\nlinear to a good approximation with dE/dx over this charge range.", "publisher": "International Union of Pure and Applied Physics", "publication_date": "1991" }, { "id": "authors:tvvy8-p1109", "collection": "authors", "collection_id": "tvvy8-p1109", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140505-092241472", "type": "book_section", "title": "Large Isotope Spectrometer for Astromag", "author": [ { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Mewaldt", "given_name": "R. A.", "orcid": "0000-0003-2178-9111", "clpid": "Mewaldt-R-A" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Ormes", "given_name": "J. F.", "clpid": "Ormes-J-F" }, { "family_name": "Streitmatter", "given_name": "R. E.", "clpid": "Streitmatter-R-E" }, { "family_name": "Rasmussen", "given_name": "I. L.", "clpid": "Rasmussen-I-L" }, { "family_name": "Wiedenbeck", "given_name": "M. E.", "orcid": "0000-0002-2825-3128", "clpid": "Wiedenbeck-M-E" } ], "abstract": "The Large Isotope Spectrometer for Astromag (LISA) is an experiment designed to measure the isotopic composition and energy spectra of cosmic rays for elements extending from beryllum through zinc. The overall objectives of this investigation are to study the origin and evolution of galactic matter; the acceleration, transport, and time scales of comsic rays in the galaxy; and search for heavy antinuclei in the cosmic radiation.\nTo achieve these objectives the LISA experiment will make the first identifications of individual heavy cosmic ray isotopes in the energy range from about 2.5 to 4 GeV/n where relativistic time dilation effects enhance the abundances of radioactive clocks and where the effects of solar modulation and cross\u2010section variations are minimized. It will extend high resolution measurements of individual element abundances and their energy spectra to energies of nearly 1 TeV/n, and has the potential for discovering heavy anti\u2010nuclei which could not have been formed except in extra\u2010galactic sources.", "doi": "10.1063/1.39145", "publisher": "American Institute of Physics", "publication_date": "1990-03-20" }, { "id": "authors:wadp3-4qn61", "collection": "authors", "collection_id": "wadp3-4qn61", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140507-142954825", "type": "book_section", "title": "Response of Ionization Chambers and Cherenkov Counters to Relativistic Ultraheavy Nuclei", "author": [ { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Vylet", "given_name": "V.", "clpid": "Vylet-V" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" } ], "contributor": [ { "family_name": "Protheroe", "given_name": "R. J.", "clpid": "Protheroe-R-J" } ], "abstract": "We have exposed a detector, similar to the one used on the HEAO Heavy\nNuclei Experiment {Binns, et al., 1981) to beams of _(26)Fe, _(57)La, _(61)Ho and\n_(79)Au at the LBL Bevalac. We will report on the deviations from z2\nscaling for the signals in the ion chambers and the Cherenkov counters\nas a function of energy and Z. These deviations are definitely small and\nimply an error of less than one charge unit in the charge\ndeterminations used in the Heavy Nuclei Experiment (Binns, et al.,\n1989).", "publisher": "University of Adelaide", "publication_date": "1990" }, { "id": "authors:35ybe-wr972", "collection": "authors", "collection_id": "35ybe-wr972", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-111300538", "type": "book_section", "title": "Energy Spectra Between 10 and Several Hundred GeV/Nucleon for Elements from _(18)Ar to _(23)V: Results from HEAO-3", "author": [ { "family_name": "Vylet", "given_name": "V.", "clpid": "Vylet-V" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Metzger", "given_name": "M.", "clpid": "Metzger-M" } ], "contributor": [ { "family_name": "Protheroe", "given_name": "R. J.", "clpid": "Protheroe-R-J" } ], "abstract": "We report updates of recently published results on cosmic ray energy spectra of the sub-iron\nnuclei. This paper is based on the following analysis and improvements : a) a better analysis of\nthe charge resolution of the instrument, b) availability of more recent charge-changing cross\nsections necessary to correct the abundances for interactions inside the detector, and c) a recent revision of the results from the French-Danish C2 experiment on HEA0-3 that were included in\nour analysis.", "publisher": "University of Adelaide", "publication_date": "1990" }, { "id": "authors:fv41x-69566", "collection": "authors", "collection_id": "fv41x-69566", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140507-141130693", "type": "book_section", "title": "Cosmic Ray Elemental Abundances for 26 33 as Measured on HEAO-3", "author": [ { "family_name": "Newport", "given_name": "B. J.", "clpid": "Newport-B-J" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" } ], "contributor": [ { "family_name": "Jones", "given_name": "F. C.", "clpid": "Jones-F-C" } ], "abstract": "The Heavy Nuclei Experiment on (HEAO-3) high energy astronomy observatory 3 uses a combination of ion chambers and a Cerenkov counter. During analysis, each particle is assigned two parameters, Zc and Zi, proportional to the square roots of the Cerenkov and mean ionization signals respectively. Because the ionization signal is double valued, a unique assignment of particle charge, Z, is not possible in general. Previous work was limited to particles of either high rigidity or low energy, for which a unique charge assignment was possible, although those subsets contain less than 50% of the total number of particles observed. The maximum likelihood technique was used to determine abundances for the complete data set from approx. 1.5 to approx. 80 GeV/amu.", "publisher": "Goddard Space Flight Center", "publication_date": "1985" }, { "id": "authors:csg22-7z285", "collection": "authors", "collection_id": "csg22-7z285", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-134843543", "type": "book_section", "title": "Energy Spectra of Elements with 18 \u2264 Z \u2264 28 Between 10 and 300 GeV/amu", "author": [ { "family_name": "Jones", "given_name": "Michael D.", "clpid": "Jones-M-D" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" } ], "contributor": [ { "family_name": "Jones", "given_name": "F. C.", "clpid": "Jones-F-C" } ], "abstract": "The HEAO-3 Heavy Nuclei Experiment (Binns, et al., 1981) is\ncomposed of ionization chambers above and below a plastic Cherenkov counter. We\nhave measured the energy dependence of the abundances of elements with atomic\nnumber, Z, between 18 and 28 at very high energies where they are rare and thus need\nthe large area x time of this experiment. We extend the measurements of the Danish French\nHEAO-3 experiment (Englemann, et al., 19S3) to higher energies, using the\nrelativistic rise of ionization signal as a measure of energy, and determine source\nabundances for Ar and Ca.", "publisher": "Goddard Space Flight Center", "publication_date": "1985" }, { "id": "authors:z903s-dye87", "collection": "authors", "collection_id": "z903s-dye87", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140423-143013765", "type": "book_section", "title": "Energy Spectra of Ultraheavy Cosmic Rays Results from HEAO-3", "author": [ { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Jones", "given_name": "M. D.", "clpid": "Jones-M-D" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Durgaprasad", "given_name": "N.", "clpid": "Durgaprasad-N" } ], "abstract": "The HEAO-3 Heavy Nuclei Experiment measures\ncosmic-ray energy directly in the interval 400 to\n~1200 MeV/amu. Geomagnetic cutoffs can also be\nderived up to ~15 GV. We present preliminary\nrigidity spectra of various ultraheavy cosmic-ray\nelements relative to iron.", "publisher": "Tata Institute of Fundamental Research", "publication_date": "1983" }, { "id": "authors:jfgzg-03n34", "collection": "authors", "collection_id": "jfgzg-03n34", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140423-140020677", "type": "book_section", "title": "Cosmic Ray Elemental Abundances for 26 \u2264 Z \u2264 42 Measured on HEAO-3", "author": [ { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Grossman", "given_name": "D. P.", "clpid": "Grossman-D-P" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Jones", "given_name": "M. D.", "clpid": "Jones-M-D" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Durgaprasad", "given_name": "N.", "clpid": "Durgaprasad-N" } ], "abstract": "Measurements from the Heavy Nuclei Experiment (Binns et al. 1981a)\naboard the HEAO-3 satellite have been used to extract definite-abundance\nvalues for the even charge nuclei and upper limit values for the less\nabundant odd charge nuclei. Individual peaks in the charge spectrum for\neven charge nuclei over this charge region are observed and the cosmic ray\nabundances obtained from this charge spectrum are compared with abundances\ncharacteristic of the solar system and with a solar system r process.", "publisher": "Tata Institute of Fundamental Research", "publication_date": "1983" }, { "id": "authors:nmtnp-knx28", "collection": "authors", "collection_id": "nmtnp-knx28", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140423-142851255", "type": "book_section", "title": "The Cosmic-Ray Abundances of the Platinum-Lead Elements as Measured on HEAO-3", "author": [ { "family_name": "Fixsen", "given_name": "D. J.", "clpid": "Fixsen-D-J" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Newport", "given_name": "B. J.", "clpid": "Newport-B-J" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "contributor": [ { "family_name": "Durgaprasad", "given_name": "N.", "clpid": "Durgaprasad-N" } ], "abstract": "The relative abundances of elements in the charge ranges of 75 \u2264 Z \u2264 79 (platinum) and 80 \u2264 Z \u2264 83 (lead) should be a sensitive indication of the contributions of the r- and s-processes in nucleosynthesis. Data from the HEAO 3 Heavy Nuclei Experiment are used to establish abundances, relative to iron, of these elements in the cosmic radiation, as well as the ratio of 'secondary' elements, in the 62 \u2264 Z \u2264 74 range, to the primary lead-platinum elements. These results appear to suggest that either the source abundances are deficient in s-process elements or that they are not organized solely by first ionization potential. In addition, present propagation models can adequately represent the relative abundances of primary and secondary elements.", "publisher": "Tata Institute of Fundamental Research", "publication_date": "1983" }, { "id": "authors:qw4v7-8h893", "collection": "authors", "collection_id": "qw4v7-8h893", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140423-143205864", "type": "book_section", "title": "Interactions of 200 GeV Gold Nuclei in Light Elements", "author": [ { "family_name": "Brewster", "given_name": "N. R.", "clpid": "Brewster-N-R" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Jones", "given_name": "M. D.", "clpid": "Jones-M-D" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Newport", "given_name": "B. J.", "clpid": "Newport-B-J" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "contributor": [ { "family_name": "Durgaprasad", "given_name": "N.", "clpid": "Durgaprasad-N" } ], "abstract": "Total charge-changing cross sections and partial cross-sections\nfor interactions of 200 GeV ^(197)_(79)Au nuclei incident\non carbon and polyethylene (CH_2) targets have been\nmeasured during a calibration of the HEA0-3 Heavy Nuclei\nExperiment. From these we infer the total and partial\ncross-sections for ^(197)_(79)Au incident on hydrogen. The effects\nof using these cross-sections in one model of cosmic ray\npropagation are illustrated. Comparisons to predictions\nusing semi-empirical formulae are shown.", "publisher": "Tata Institute of Fundamental Research", "publication_date": "1983" }, { "id": "authors:83gyx-j8e80", "collection": "authors", "collection_id": "83gyx-j8e80", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140423-144319881", "type": "book_section", "title": "Correlation of Source Abundances of Ultraheavy Cosmic Rays with First Ionization Potential - Results from HEAO-3", "author": [ { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Grossman", "given_name": "D. P.", "clpid": "Grossman-D-P" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Margolis", "given_name": "S. H.", "clpid": "Margolis-S-H" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Krombel", "given_name": "K. E.", "clpid": "Krombel-K-E" }, { "family_name": "Brewster", "given_name": "N. R.", "clpid": "Brewster-N-R" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Durgaprasad", "given_name": "N.", "clpid": "Durgaprasad-N" } ], "abstract": "The cosmic-ray-source abundances inferred from HEAO-3 observation by the Heavy Nuclei Experiment for 30 < Z < 60 generally follow the correlation with first-ionization potential which has previously been observed for Z < 30. However the low Ge abundance suggests that the elemental \"volatility\" may be an organizing factor.", "publisher": "Tata Institute of Fundamental Research", "publication_date": "1983" }, { "id": "authors:7ccyx-h7a81", "collection": "authors", "collection_id": "7ccyx-h7a81", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140423-143400546", "type": "book_section", "title": "Abundances of 'Secondary' Elements Among the Ultraheavy Cosmic Rays - Results from HEAO-3", "author": [ { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Margolis", "given_name": "S. H.", "clpid": "Margolis-S-H" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Brewster", "given_name": "N. R.", "clpid": "Brewster-N-R" }, { "family_name": "Fixsen", "given_name": "D. J.", "clpid": "Fixsen-D-J" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Durgaprasad", "given_name": "N.", "clpid": "Durgaprasad-N" } ], "abstract": "The HEAO-3 Heavy Nuclei Experiment has measured elemental abundances of ultraheavy cosmic rays near earth. The elements with atomic number (Z) in the intervals 44 < Z < 48 and 62 < Z < 74 arriving at earth are expected to have significant secondary components. However, their source abundances are unlikely to be low enough to warrant treating them as pure secondaries. The present results are consistent with solar system abundances modified for first ionization potential with possibly some enhancement of the r to s ratio.", "publisher": "Tata Institute of Fundamental Research", "publication_date": "1983" }, { "id": "authors:v1s17-qjb84", "collection": "authors", "collection_id": "v1s17-qjb84", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140423-141835138", "type": "book_section", "title": "Cosmic-Ray Abundances of the Even Charge Elements from _(50)Sn to _(58)Ce Measured on HEAO-3", "author": [ { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Krombel", "given_name": "K. E.", "clpid": "Krombel-K-E" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Klamiann", "given_name": "J.", "clpid": "Klamiann-J" }, { "family_name": "Brewster", "given_name": "N. R.", "clpid": "Brewster-N-R" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Durgaprasad", "given_name": "N.", "clpid": "Durgaprasad-N" } ], "abstract": "Elements with even atomic number (Z) in the interval 50 \u2264\n Z \u2264 58 have been\nresolved in the cosmic radiation using the Heavy Nuclei Experiment on the\nHEAO-3 satellite. The observation that _(50)Sn and _(56)Ba are more abundant that _(52)Te\nand _(54)Xe indicates a substantial s-process contribution to the cosmic ray source. A\nsignificant abundance of _(58)Ce provides further support for this finding.", "publisher": "Tata Institute of Fundamental Research", "publication_date": "1983" }, { "id": "authors:hw2cn-gq710", "collection": "authors", "collection_id": "hw2cn-gq710", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140423-144626311", "type": "book_section", "title": "The Non-Z^2 Response of the Heavy Nuclei Cosmic Ray Detector on HEAO-3", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Newport", "given_name": "B. J.", "clpid": "Newport-B-J" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Jones", "given_name": "M. D.", "clpid": "Jones-M-D" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Durgaprasad", "given_name": "N.", "clpid": "Durgaprasad-N" } ], "abstract": "A combination of ion chambers and Cerenkov radiators similar to the Heavy Nuclei Experiment flown on HEAO-3 was calibrated at the Bevalac heavy-ion accelerator using beams of Mn-25 nuclei at kinetic energies up to about 1700 MeV/nucleon and Au-79 nuclei up to about 1000 MeV/nucleon. The data show only a small deviation (about 2-3 charge units at Au) from the Z^2 scaling used previously (Binns et al., 1981, 1982, 1983) to analyze the HNE data. Although at lower energy, the calibration indicates that the published relative abundances of the _(50)Sn/_(56)Ba group and the published upper-limit actinide abundances are not likely to be significantly affected by non-Z^2 effects.", "publisher": "Tata Institute of Fundamental Research", "publication_date": "1983" }, { "id": "authors:v9w9z-6rv70", "collection": "authors", "collection_id": "v9w9z-6rv70", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181115-131341372", "type": "book_section", "title": "Heavy Nuclei Experiment on HEAO-3", "book_title": "Origin of Cosmic Rays", "author": [ { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Fickle", "given_name": "R.", "clpid": "Fickle-R-K" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" } ], "contributor": [ { "family_name": "Setti", "given_name": "Giancarlo", "clpid": "Setti-G" }, { "family_name": "Speda", "given_name": "G.", "clpid": "Speda-G" }, { "family_name": "Wolfendale", "given_name": "A. W.", "clpid": "Wolfendale-A-W" } ], "abstract": "The third High Energy Astronomical Observatory, HEAO-3 was launched on the 20th Sept., 1979 into a 496 km, 43.6\u00b0 orbit, and has since been successfully returning data from all three experiments on board. One of these experiments, that intended to study the heavy and ultra heavy nuclei in the cosmic radiation, is described here.", "doi": "10.1017/s0074180900074453", "isbn": "9789400984752", "publisher": "Kluwer", "place_of_publication": "Dordrecht", "publication_date": "1981", "pages": "91-92" }, { "id": "authors:2e5fw-vn450", "collection": "authors", "collection_id": "2e5fw-vn450", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140417-154647949", "type": "book_section", "title": "Abundances of Cosmic Ray Nuclei Heavier than _(50)Sn", "author": [ { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" } ], "abstract": "Preliminary results are reported from 430 days of exposure of the heavy nuclei experiment on the HEAO-3 spacecraft. These results are confined to the heavy nuclei with Z \u2265 50 and emphasize the conclusions obtained on the relative numbers of actinides and heavy stable elements in the lead-platinum region. The extreme paucity of actinides found is inconsistent with the predictions of a cosmic ray source that is highly enriched in r-process material, but quite consistent with a source whose composition is similar to that of normal solar system material. An upper limit, at the. 95% confidence level, is placed in the ratio of nuclei with Z \u2265 88/(74 \u2264 Z \u226487) of 0.03.", "publisher": "CEN Saclay", "publication_date": "1981" }, { "id": "authors:sp46z-c5r70", "collection": "authors", "collection_id": "sp46z-c5r70", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140417-151643116", "type": "book_section", "title": "Implications of Ultraheavy Cosmic-Ray Source Composition Derived from Observations by the HEAO-3 Heavy Nuclei Experiment", "author": [ { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "abstract": "We have derived the contribution of r-process\nand s-process nucleosynthesis to the Cameron\n(1980) solar system (SS) abundances for Z~33.\nIn the interval 34 ~Zs; 40 our HEA0-3 data\nextrapolated to the cosmic-ray source (CRS)\nfit the solar system mix better than r-process.\nIn the interval 26 < Z < 40 the HEA0-3 results for\nCRS/SS follow the same general correlation with\nfirst ionization potential as for the lighter\neiements although there are deviations in detail.", "publisher": "CEN Saclay", "publication_date": "1981" }, { "id": "authors:bkem1-npf74", "collection": "authors", "collection_id": "bkem1-npf74", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140417-151754488", "type": "book_section", "title": "Abundances of Cosmic Ray Nuclei for 26 \u2264 Z \u2264 40 From HEAO-3 Heavy Nuclei Experiment", "author": [ { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Israel", "given_name": "M. H.", "orcid": "0000-0002-8104-208X", "clpid": "Israel-M-H" }, { "family_name": "Fickle", "given_name": "R. K.", "clpid": "Fickle-R-K" }, { "family_name": "Waddington", "given_name": "C. J.", "clpid": "Waddington-C-J" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "abstract": "Individual elements in the cosmic radiation of\neven atomic number (Z)in the interval 26\u2264 Z \u2264 40\nhave been resolved and their relative abundances\nmeasured. The results are inconsistent with a\ncosmic-ray source whose composition in this charge\ninterval is dominated by r-process nucleosynthesis.", "publisher": "CEN Saclay", "publication_date": "1981" }, { "id": "authors:ets7e-77937", "collection": "authors", "collection_id": "ets7e-77937", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140409-092309559", "type": "book_section", "title": "Relation of the Radial Gradient of Cosmic-Ray Protons to the Size of the Solar-Modulation Region", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Vogt", "given_name": "R. E.", "clpid": "Vogt-R-E" } ], "abstract": "The radial intensity-gradient of cosmic-ray protons has been\ncalculated for a range of values of the distance to the boundary\nof a spherically symmetric solar-modulation region. We find\nthat the radial dependence of the gradients may be described\nin terms of two characteristic domains of the modulation region:\n(a) an \"inner region\" where the gradients are relatively small\nand constant, and (b), an \"outer region\"' where the gradients\nare large and show a strong radial dependence. The magnitude\nof the gradient in the inner region is small for reasonable\nvalues for the physical parameters of the modulation mechanism.", "publisher": "Colorado Associated University Press", "publication_date": "1973" } ]