[ { "id": "authors:5s4zk-77d24", "collection": "authors", "collection_id": "5s4zk-77d24", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140827-090127162", "type": "article", "title": "Io encounters past and present: A heavy ion comparison", "author": [ { "family_name": "Cohen", "given_name": "C. M. S.", "orcid": "0000-0002-0978-8127", "clpid": "Cohen-C-M-S" }, { "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": "Cooper", "given_name": "J. F.", "clpid": "Cooper-J-F" }, { "family_name": "Murphy", "given_name": "N.", "clpid": "Murphy-N" }, { "family_name": "Gehrels", "given_name": "N.", "clpid": "Gehrels-N" } ], "abstract": "The heavy ion counter (HIC) on the Galileo spacecraft consists of two low-energy telescopes that were proof-test models of the telescopes used for the cosmic ray subsystem (CRS) on Voyager. The telescopes on HIC were improved to better withstand the intense radiation environment of the Jovian system and to measure higher-energy particles with greater sensitivity. The similarity of these two instruments makes it natural to compare the data in an effort to glean insight on the behavior of heavy ion fluxes at higher energies and how the inner Jovian magnetosphere has changed in the last 18 years. Inside L = 6, the oxygen spectrum suggests a spectral break at \u223c 7500 MeV/Gauss, corresponding to ions with gyroradii of \u223c 1.5 R_(Io) at L = 6. A comparison of the phase space densities show remarkable agreement between the two time periods outside of the Io orbit, with differential spectra consistent with \u03b3 \u223c \u22128 above \u223c 6 MeV/nucleon. Near Io Galileo observed a large density gradient not apparent in the Voyager data that may be due to local time asymmetries or a decrease in the radial diffusion rate.", "doi": "10.1029/1999JA000021", "issn": "0148-0227", "publisher": "American Geophysical Union", "publication": "Journal of Geophysical Research A", "publication_date": "2000-04-01", "series_number": "A4", "volume": "105", "issue": "A4", "pages": "7775-7782" }, { "id": "authors:pdaek-z9b78", "collection": "authors", "collection_id": "pdaek-z9b78", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150108-132035904", "type": "article", "title": "The ACE Science Center", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Davis", "given_name": "A. J.", "clpid": "Davis-A-J" }, { "family_name": "Hammond", "given_name": "J. S.", "clpid": "Hammond-J-S" }, { "family_name": "Sears", "given_name": "S. R.", "clpid": "Sears-S-R" } ], "abstract": "Abstract. The Advanced Composition Explorer (ACE) mission is supported by the ACE Science Center for the purposes of processing and distributing ACE data, and facilitating collaborative work on the data by instrument investigators and by the space physics community at large. The Science\nCenter will strive to ensure that the data are properly archived and easily available. In particular, it is intended that use of a centralized science facility will guarantee 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. Secondary functions performed by the Science Center include acting as an interface between the scientists and the mission operations\nteam.", "doi": "10.1023/A:1005096317576", "issn": "0038-6308", "publisher": "Springer", "publication": "Space Science Reviews", "publication_date": "1998-07", "series_number": "1-4", "volume": "86", "issue": "1-4", "pages": "649-663" }, { "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: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: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: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: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:9rtgs-px940", "collection": "authors", "collection_id": "9rtgs-px940", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140225-110013580", "type": "article", "title": "Effects of Absorption by lo on Composition of Energetic Heavy lons", "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": "Murphy", "given_name": "N.", "clpid": "Murphy-N" } ], "abstract": "The Galileo heavy ion counter is sensitive to ions with atomic numbers Z \u2265 6 and energies\ngreater than ~6 MeV per nucleon. During Galileo's passage through Jupiter's inner\nmagnetosphere, the observed composition of these heavy ions was consistent with the\npresence of singly ionized iogenic O, Na, and S and highly ionized solar C, O, and Ne.\nThe solar component is absorbed more strongly by lo because its gyroradius is smaller\nthan Io's diameter.", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1996-10-18", "series_number": "5286", "volume": "274", "issue": "5286", "pages": "393-394" }, { "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:p6z7z-taz94", "collection": "authors", "collection_id": "p6z7z-taz94", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140619-160623174", "type": "article", "title": "Fragmentation cross sections of relativistic ^(84)_(36)Kr and ^(109)_(47)Ag nuclei in targets from hydrogen to lead", "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": "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" } ], "abstract": "With the addition of krypton and silver projectiles we have extended our previous studies of the fragmentation of heavy relativistic nuclei in targets ranging in mass from hydrogen to lead. These projectiles were studied at a number of discrete energies between 450 and 1500A MeV. The total and partial charge-changing cross sections were determined for each energy, target, and projectile, and the values compared with previous predictions. A new parametrization of the dependence of the total charge-changing cross sections on the target and projectile is introduced, based on nuclear charge radii derived from electron scattering. We have also parametrized the energy dependence of the total cross sections over the range of energies studied. New parameters were found for a previous representation of the partial charge-changing cross sections in hydrogen and a new parametrization has been introduced for the nonhydrogen targets. The evidence that limiting fragmentation has been attained for these relatively light projectile nuclei at Bevalac energies is shown to be inconclusive, and further measurements at higher energies will be needed to address this question.", "doi": "10.1103/PhysRevC.52.3277", "issn": "0556-2813", "publisher": "American Physical Society", "publication": "Physical Review C", "publication_date": "1995-12", "series_number": "6", "volume": "52", "issue": "6", "pages": "3277-3280" }, { "id": "authors:t856j-89r87", "collection": "authors", "collection_id": "t856j-89r87", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140624-135742495", "type": "article", "title": "Solar Particle Induced Upsets in the TDRS-1 Attitude Control System RAM During the October 1989 Solar Particle Events", "author": [ { "family_name": "Croley", "given_name": "D. R.", "clpid": "Croley-D-R" }, { "family_name": "Garrett", "given_name": "H. B.", "clpid": "Garrett-H-B" }, { "family_name": "Murphy", "given_name": "G. B.", "clpid": "Murphy-G-B" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" } ], "abstract": "The three large solar particle events, beginning on October 19, 1989 and lasting approximately six days, were characterized by high fluences of solar protons and heavy ions at 1 AU. During these events, an abnormally large number of upsets (243) were observed in the random access memory of the attitude control system (ACS) control processing electronics (CPE) on-board the geosynchronous TDRS-1 (Telemetry and Data Relay Satellite). The RAM unit affected was composed of eight Fairchild 93L422 memory chips. The Galileo spacecraft, launched on October 18, 1989 (one day prior to the solar particle events) observed the fluxes of heavy ions experienced by TDRS-1. Two solid-state detector telescopes on-board Galileo designed to measure heavy ion species and energy, were turned on during time periods within each of the three separate events. The heavy ion data have been modeled and the time history of the events reconstructed to estimate heavy ion fluences. These fluences were converted to effective LET spectra after transport through the estimated shielding distribution around the TDRS-1 ACS system. The number of single event upsets (SEU) expected was calculated by integrating the measured cross section for the Fairchild 93L422 memory chip with average effective LET spectrum. The expected number of heavy ion induced SEUs calculated was 176. GOES-7 proton data, observed during the solar particle events, were used to estimate the number of proton-induced SEUs by integrating the proton fluence spectrum incident on the memory chips, with the two-parameter Bendel cross section for proton SEU's. The proton fluence spectrum at the device level \nwas gotten by transporting the protons through the estimated \nshielding distribution. The number of calculated proton-induced \nSEU's was 72, yielding a total of 248 predicted SEU's, very \nclose to the 243 observed SEU's. These calculations uniquely \ndemonstrate the roles that solar heavy ions and protons played in \nthe production of SEU's during the October 1989 solar particle \nevents.", "doi": "10.1109/23.467946", "issn": "0018-9499", "publisher": "IEEE", "publication": "IEEE Transactions on Nuclear Science", "publication_date": "1995-10", "series_number": "5", "volume": "42", "issue": "5", "pages": "1489-1496" }, { "id": "authors:fe9c5-mhq97", "collection": "authors", "collection_id": "fe9c5-mhq97", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140619-153743030", "type": "article", "title": "The Charge-Changing Fragmentation of 10.6 GeV/nucleon ^(197)Au 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" } ], "abstract": "We have measured the charge-changing cross sections of 10.6 GeV/nucleon ^(197)Au nuclei interacting in targets of CH_2 (polyethylene), C, Al, Cu, Sn, and Pb. Cross sections for H are calculated from those measured in C and CH_2. The total charge-changing cross sections are higher than those measured at energies of \u22641 GeV/nucleon. The measured cross sections for the heavier targets are somewhat larger than those predicted by a model based on data taken at lower energies with lighter targets. Partial charge-changing cross sections for the production of fragments from the incident Au projectiles were measured for charge changes (\u0394Z) from \u0394Z=+1_(,80)Hg, down to approximately \u0394Z=-29_(,50)Sn. In comparison to lower energy measurements, these partial cross sections are found to be smaller for small \u0394Z and larger or the same for large \u0394Z. The H partial cross sections are found to follow a power law in \u0394Z similar to that for heavier targets, instead of the exponential form observed at lower energies. Factorization is found to hold for all partial cross sections with \u0394Z greater than two. In the heavier targets, the cross sections for one and two proton removal have significant contributions from electromagnetic dissociation. The electromagnetic dissociation contribution to the total cross section is derived and found to be relatively small, but with a strong dependence on the charge of the target nuclei of the form Z_T^(1.75\u00b10.01).", "doi": "10.1103/PhysRevC.52.334", "issn": "0556-2813", "publisher": "American Physical Society", "publication": "Physical Review C", "publication_date": "1995-07", "series_number": "1", "volume": "52", "issue": "1", "pages": "334-337" }, { "id": "authors:4ahn0-za354", "collection": "authors", "collection_id": "4ahn0-za354", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140612-113711597", "type": "article", "title": "Charge-changing fragmentation of 10.6 GeV/nucleon ^(197)Au 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" }, { "literal": "UHIC collaboraion" } ], "abstract": "We have measured the charge-changing cross sections of 10.6 GeV/nucleon ^(197)Au nuclei interacting in targets of CH2 (polyethylene), C, Al, Cu, Sn, and Pb. Cross sections for H are calculated from those measured in C and CH_2. The total charge-changing cross sections are higher than those measured at energies of \u22641 GeV/nucleon. The measured cross sections for the heavier targets are somewhat larger than those predicted by a model based on data taken at lower energies with lighter targets. Partial charge-changing cross sections for the production of fragments from the incident Au projectiles were measured for charge changes (\u0394Z) from \u0394Z=+1, _(80)Hg, down to approximately \u0394Z=-29, _(50)Sn. In comparison to lower energy measurements, these partial cross sections are found to be smaller for small \u0394Z and larger or the same for large \u0394Z. The H partial cross sections are found to follow a power law in \u0394Z similar to that for heavier targets, instead of the exponential form observed at lower energies. Factorization is found to hold for all partial cross sections with \u0394Z greater than two. In the heavier targets, the cross sections for one and two proton removal have significant contributions from electromagnetic dissociation. The electromagnetic dissociation contribution to the total cross section is derived and found to be relatively small, but with a strong dependence on the charge of the target nuclei of the form Z__T^(1.75\u00b10.01).", "doi": "10.1103/PhysRevC.52.334", "issn": "0556-2813", "publisher": "American Physical Society", "publication": "Physical Review C", "publication_date": "1995-07", "series_number": "1", "volume": "52", "issue": "1", "pages": "334-345" }, { "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:0965n-5ky85", "collection": "authors", "collection_id": "0965n-5ky85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140523-100720835", "type": "article", "title": "Nuclear Fragmentation Parameters Needed for Interpretation of Observed Fluxes of UH Cosmic Ray 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": "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" }, { "literal": "UHIC collaboraion" } ], "abstract": "Any study of the origin of the UH nuclei in the cosmic rays requires that their observed abundances be propagated back to the source. This demands a knowledge of the interaction cross sections in the materials of the detectors, any local overlying matter, and the interstellar medium. New measurements of interaction probabilities of 10.6 GeV/n gold nuclei show significant differences from previous measurements made at less than 1.0 GeV/n nuclei. These differences are particularly marked for a hydrogen target. Hence, those cross sections previously measured at low energies not be applied to cosmic ray observations made at energies \u2265 2 GeV/n. Without a measurement of the energy dependence of these cross sections it will be difficult to make reliable propagation calculations, since the differences between measured and predicted cross sections are still at the 20 to 30% level.", "doi": "10.1016/0273-1177(94)00007-N", "issn": "0273-1177", "publisher": "Elsevier", "publication": "Advances in Space Research", "publication_date": "1995", "series_number": "6", "volume": "15", "issue": "6", "pages": "39-48" }, { "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:n5vj7-vhp66", "collection": "authors", "collection_id": "n5vj7-vhp66", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140523-092704083", "type": "article", "title": "Charge-pickup by Heavy Relativistic 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": "Geer", "given_name": "L. Y.", "clpid": "Geer-L-Y" }, { "family_name": "Klarmann", "given_name": "J.", "clpid": "Klarmann-J" }, { "literal": "UHIC collaboraion" } ], "abstract": "In the interactions of relativistic heavy projectile nuclei with target nuclei there is a measurable probability for the projectile nuclei to pick up a charge during the interaction. We report here new measurements, made in a wide range of targets, of the cross sections for charge-pickup of gold nuclei with energies of 10.6 GeV/nucleon, and of silver and krypton nuclei with energies between 1.4 and 0.5 GeV/nucleon. The excitation functions of these cross sections are discussed using all the measurements available to us and indicate that there are significant decreases in the cross sections as the energies increase. A weak target dependence is seen. Previously these cross sections have been reported to have a strong, approximately quadratic, dependence on the projectile mass. This conclusion has to be modified in the light of these new measurements. Instead, we suggest that the cross sections show a strong exponential dependence on either the fractional neutron excesses or, equivalently, on the neutron to nucleon ratios of the projectile nuclei.", "doi": "10.1103/PhysRevC.50.1065", "issn": "0556-2813", "publisher": "American Physical Society", "publication": "Physical Review C", "publication_date": "1994-08", "series_number": "2", "volume": "50", "issue": "2", "pages": "1065-1076" }, { "id": "authors:t9ya9-xcq64", "collection": "authors", "collection_id": "t9ya9-xcq64", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140516-104704903", "type": "article", "title": "Interactions of 10.6 GeV/n Gold Nuclei in Targets from _1H to _(82)Pb", "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": "Gauld", "given_name": "B.W.", "clpid": "Gault-B-W" }, { "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" } ], "abstract": "The 10.6 GeV/n gold beam from the AGS has been allowed to interact in a wide range\nof targets. The emerging fragments with charges between _(80)Hg and _(57)La have been identified.\nPreliminary values have been determined for tile total cross sections for charge changing\ninteractions, for the partial cross sections for the production of heavy fragments, and for the\npartial cross sections for charge pickup.", "doi": "10.1016/0375-9474(94)90661-0", "issn": "0375-9474", "publisher": "Elsevier", "publication": "Nuclear Physics A", "publication_date": "1994-01-03", "volume": "566", "pages": "427-430" }, { "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:3e6s9-27q49", "collection": "authors", "collection_id": "3e6s9-27q49", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140512-103823930", "type": "article", "title": "PET: A Proton/Electron Telescope for Studies of Magnetospheric, Solar, and Galactic Particles", "author": [ { "family_name": "Cook", "given_name": "W. R.", "clpid": "Cook-W-R" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Kecman", "given_name": "B.", "clpid": "Kecman-B" }, { "family_name": "Mewaldt", "given_name": "R. A.", "orcid": "0000-0003-2178-9111", "clpid": "Mewaldt-R-A" }, { "family_name": "Selesnick", "given_name": "R. S.", "clpid": "Selesnick-R-S" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Baker", "given_name": "D. N.", "clpid": "Baker-D-N" }, { "family_name": "von Rosenvinge", "given_name": "T. T.", "clpid": "von-Rosenvinge-T-T" }, { "family_name": "Blake", "given_name": "J. B.", "clpid": "Blake-J-B" }, { "family_name": "Callis", "given_name": "L. B.", "clpid": "Callis-L-B" } ], "abstract": "The proton/electron telescope (PET) on SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) is designed to provide measurements of energetic electrons and light nuclei from solar, Galactic, and magnetospheric sources. PET is an all solid-state system that will measure the differential energy spectra of electrons from ~1 to ~30 MeV and H and He nuclei from ~20 to ~300 MeV/nucleon, with isotope resolution of H and He extending from ~20 to ~80 MeV/nucleon. As SAMPEX scans all local times and geomagnetic cutoffs over the course of its near-polar orbit, PET will characterize precipitating relativistic electron events during periods of declining solar activity, and it will examine whether the production rate of odd nitrogen and hydrogen molecules in the middle atmosphere by precipitating electrons is sufficient to affect O_3 depletion. In addition, PET will complement studies of the elemental and isotopic composition of energetic heavy (Z>2) nuclei on SAMPEX by providing measurements of H, He, and electrons. Finally, PET has limited capability to identify energetic positrons from potential natural and man-made sources.", "doi": "10.1109/36.225523", "issn": "0196-2892", "publisher": "IEEE Transactions on Geoscience and Remote Sensing", "publication": "IEEE Transactions on Geoscience and Remote Sensing", "publication_date": "1993-05", "series_number": "3", "volume": "31", "issue": "3", "pages": "565-571" }, { "id": "authors:5ybza-tm133", "collection": "authors", "collection_id": "5ybza-tm133", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140307-151617567", "type": "article", "title": "MAST: a mass spectrometer telescope for studies of the isotopic composition of solar, anomalous, and galactic cosmic ray nuclei", "author": [ { "family_name": "Cook", "given_name": "W. R.", "clpid": "Cook-W-R" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Kecman", "given_name": "B.", "clpid": "Kecman-B" }, { "family_name": "Mewaldt", "given_name": "R. A.", "orcid": "0000-0003-2178-9111", "clpid": "Mewaldt-R-A" }, { "family_name": "Selesnick", "given_name": "R. S.", "clpid": "Selesnick-R-S" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "von Rosenvinge", "given_name": "T. T.", "clpid": "von-Rosenvinge-T-T" } ], "abstract": "The mass spectrometer telescope (MAST) on SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) is designed to provide high-resolution measurements of the isotopic composition of energetic nuclei from He to Ni (Z=2 to 28) over the energy range from ~10 to several hundred MeV/nucleon. During large solar flares MAST will measure the isotopic abundances of solar energetic particles to determine directly the composition of the solar corona, while during solar quiet times MAST will study the isotopic composition of galactic cosmic rays. In addition, MAST will measure the isotopic composition of both interplanetary and trapped fluxes of anomalous cosmic rays, believed to be a sample of the nearby interstellar medium.", "doi": "10.1109/36.225522", "issn": "0196-2892", "publisher": "IEEE", "publication": "IEEE Transactions on Geoscience and Remote Sensing", "publication_date": "1993-05", "series_number": "3", "volume": "31", "issue": "3", "pages": "557-564" }, { "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:1fsab-kyb09", "collection": "authors", "collection_id": "1fsab-kyb09", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140429-100145815", "type": "article", "title": "The Galileo Heavy Element Monitor", "author": [ { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Gehrels", "given_name": "N.", "clpid": "Gehrels-N" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" } ], "abstract": "The Heavy Ion Counter on the Galileo spacecraft will monitor energetic heavy nuclei of the elements from C to Ni, with energies from \u223c 6 to \u223c 200 MeV nucl^(-1). The instrument will provide measurements of trapped heavy ions in the Jovian magnetosphere, including those high-energy heavy ions with the potential for affecting the operation of the spacecraft electronic circuitry. We describe the instrument, which is a modified version of the Voyager CRS instrument.", "doi": "10.1007/BF00216859", "issn": "0038-6308", "publisher": "Springer", "publication": "Space Science Reviews", "publication_date": "1992-05", "series_number": "1-4", "volume": "60", "issue": "1-4", "pages": "305-315" }, { "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: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: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: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:6z1mj-1qc95", "collection": "authors", "collection_id": "6z1mj-1qc95", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-110735443", "type": "article", "title": "Determination of the Cross Sections for the Production of Fragments from Relativistic Nucleus-Nucleus Interactions. Part I: Measurements", "author": [ { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "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": "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" } ], "abstract": "Relativistic iron, lanthanum, holmium, and gold projectile nuclei with several different energies have been fragmented in targets of polyethylene, carbon, aluminum, copper, and lead. Our detectors cleanly resolve the individual charges of the heaviest of these fragments and provide some limited information on the masses. We have measured 1256 elemental partial cross sections for the production of fragments from interactions in these target materials. Values have been derived for another 417 cross sections in a hydrogen medium. These cross sections depend on the energy and mass of the projectile nuclei as well as on the nature of the target. Total charge-changing cross sections were also found, but only in a composite target, and have been shown to be weakly dependent on energy. The mean mass losses observed for fragments that have lost a few protons show that typically many neutrons are lost with each proton, producing fragment nuclei that must be highly proton rich, and consequently very unstable. The cross sections for charge pickup on heavy targets show a rapid increase with decreasing energy, particularly for the heaviest targets. The systematics of the dependencies of the partial cross sections will be discussed in a companion paper.", "doi": "10.1103/PhysRevC.42.2508", "issn": "0556-2813", "publisher": "American Physical Society", "publication": "Physical Review C", "publication_date": "1990-12", "series_number": "6", "volume": "42", "issue": "6", "pages": "2508-2530" }, { "id": "authors:zq353-n6873", "collection": "authors", "collection_id": "zq353-n6873", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140501-111116037", "type": "article", "title": "Determination of the Cross Sections for the Production of Fragments from Relativistic Nucleus-Nucleus Interactions. Part II: Parametric Fits", "author": [ { "family_name": "Cummings", "given_name": "J. R.", "clpid": "Cummings-J-R" }, { "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": "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" } ], "abstract": "Measurements of the partial charge-changing cross sections for the fragmentation of relativistic iron, lanthanum, holmium, and gold nuclei of several different energies incident on targets of polyethylene, carbon, aluminum, and copper have been reported in an accompanying paper. This paper describes the systematics of the variations of these cross sections with energy, projectile, target, and fragment. We have been able to generate a seven-parameter global fit to 795 measured cross sections for the heavy targets which fits the data with a standard deviation of 7%. We have also generated a similar global fit to 303 measured cross sections for a hydrogen target which fits the data with a standard deviation of 10%. These representations imply that the hypothesis of limiting fragmentation is only accurate to some 20\u201330 %. Weak factorization can apply, but fits that are marginally better, and more physically plausible, can be obtained without factorization. We have identified, and discussed, a number of caveats to the applicability of these fits outside, and inside, the range of energies and masses covered. Excessively large cross sections for the loss of a single proton from the projectile nuclei suggest electromagnetic dissociation. The cross sections for fragments that experience large charge changes appear to become independent of the size of the charge change. Very heavy projectiles have a significant probability of experiencing fission.", "doi": "10.1103/PhysRevC.42.2530", "issn": "0556-2813", "publisher": "American Physical Society", "publication": "Physical Review C", "publication_date": "1990-12", "series_number": "6", "volume": "42", "issue": "6", "pages": "2530-2545" }, { "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: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:0rcdy-4fb66", "collection": "authors", "collection_id": "0rcdy-4fb66", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140429-095757981", "type": "article", "title": "Elemental Abundances of Ultraheavy Cosmic Rays", "author": [ { "family_name": "Binns", "given_name": "W. R.", "orcid": "0000-0001-6110-3407", "clpid": "Binns-W-R" }, { "family_name": "Fixsen", "given_name": "D. J.", "clpid": "Fixsen-D-J" }, { "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" } ], "abstract": "The elemental composition of the cosmic-ray source is different from that which has been generally taken as the composition of the solar system. No general enrichment of products of either r-process or s-process nucleosynthesis accounts for the differences over the entire range of ultraheavy (Z > 30) elements; specific determination of nucleosynthetic contributions to the differences depends upon an understanding of the nature of any acceleration fractionation. Comparison between the cosmic-ray source abundances and the abundances of C1 and C2 chondritic meteorites suggests the possibility that differences between the cosmic-ray source and the \"standard (C1) solar system\" may not be due to acceleration fractionation of the cosmic rays, but may be due instead to a fractionation of the C1 abundances with respect to the interstellar abundances.", "doi": "10.1016/0273-1177(84)90289-8", "issn": "0273-1177", "publisher": "Elsevier", "publication": "Advances in Space Research", "publication_date": "1984", "series_number": "2-3", "volume": "4", "issue": "2-3", "pages": "25-34" }, { "id": "authors:e37ah-87g94", "collection": "authors", "collection_id": "e37ah-87g94", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140421-140007292", "type": "article", "title": "Cosmic Ray Abundances of Sn, Te, Xe, and Ba Nuclei Measured on HEAO 3", "author": [ { "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": "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": "Krombel", "given_name": "K. E.", "clpid": "Krombel-K-E" }, { "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" } ], "abstract": "Elements with even atomic number ( Z) in the interval 50 ~ Z ~ 56 have been resolved in the\ncosmic radiation using the Heavy Nuclei Experiment on the HEAO 3 satellite. The observation that\n50Sn and 56Ba are more abundant than 52Te Elements with even atomic number ( Z) in the interval 50 ~ Z ~ 56 have been resolved in the\ncosmic radiation using the Heavy Nuclei Experiment on the HEAO 3 satellite. The observation that\n50Sn and 56Ba are more abundant than 52Te \nand 54Xe is inconsistent with a purer-process cosmic-ray\nsource. Adjustment of source abundances for an enhancement of those elements with a low first\nionization potential does not change this conclusion and 54Xe is inconsistent with a purer-process cosmic-ray\nsource. Adjustment of source abundances for an enhancement of those elements with a low first\nionization potential does not change this conclusion.", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1983-04-15", "volume": "267", "pages": "L93-L96" }, { "id": "authors:8s41n-nds25", "collection": "authors", "collection_id": "8s41n-nds25", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140409-080134015", "type": "article", "title": "Cosmic-ray abundances of Sn, Te, Xe, and BA nuclei measured on HEAO 3", "author": [ { "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": "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": "Krombel", "given_name": "K. E.", "clpid": "Krombel-K-E" }, { "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" } ], "abstract": "Elements with even atomic number (Z) in the interval 50 \u2264 Z \u2264 56 have been resolved in the cosmic radiation using the Heavy Nuclei Experiment on the HEAO 3 satellite. The observation that _(50)Sn and _(56)Ba are more abundant than _(52)Te and _(54)Xe is inconsistent with a pure r-process cosmic-ray source. Adjustment of source abundances for an enhancement of those elements with a low first ionization potential does not change this conclusion.", "doi": "10.1086/184010", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "1983-04-15", "series_number": "2", "volume": "267", "issue": "2", "pages": "L93-L96" }, { "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: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: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: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: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: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: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:cjnp5-ht349", "collection": "authors", "collection_id": "cjnp5-ht349", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140304-105424511", "type": "article", "title": "The abundance of the actinides in the cosmic radiation as measured on HEAO 3", "author": [ { "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": "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" } ], "abstract": "The HEAO 3 detector of heavy cosmic-ray nuclei has observed one possible actinide nucleus and\nsome 100 nuclei of the platinum-lead group of elements. The resulting upper limit of 3% for the\nabundance ratio of actinides to platinum-lead nuclides is significantly lower than previous results\nfrom other observations. This new limit is inconsistent with freshly synthesized, pure r-process\nsources for cosmic-ray nuclei in this charge interval but is consistent with a source having a\ncomposition similar to the solar system, or to aged r-process material. We observe no events with a\ncharge greater than 96.", "doi": "10.1086/183899", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1982-10-15", "series_number": "2", "volume": "261", "issue": "2", "pages": "L117-L120" }, { "id": "authors:ff5ns-6zt61", "collection": "authors", "collection_id": "ff5ns-6zt61", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140210-140754733", "type": "article", "title": "Energetic Charged Particles in Saturn's Magnetosphere: Voyager 2 Results", "author": [ { "family_name": "Vogt", "given_name": "R. E.", "clpid": "Vogt-R-E" }, { "family_name": "Chenette", "given_name": "D. L.", "clpid": "Chenette-D-L" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "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": "Schardt", "given_name": "A. W.", "clpid": "Schardt-A-W" }, { "family_name": "Trainor", "given_name": "J. H.", "clpid": "Trainor-J-H" }, { "family_name": "Lal", "given_name": "N.", "clpid": "Lal-N" }, { "family_name": "McDonald", "given_name": "F. B.", "clpid": "McDonald-F-B" } ], "abstract": "Results from the cosmic-ray system on Voyager 2 in Saturn's magnetosphere are presented. During the inbound pass through the outer magnetosphere, the \u2265 0.43-million-electron-volt proton flux was more intense, and both the proton and electron fluxes were more variable, than previously observed. These changes are attributed to the influence on the magnetosphere of variations in the solar wind conditions. Outbound, beyond 18 Saturn radii, impulsive bursts of 0.14- to > 1.0- million-electron-volt electrons were observed. In the inner magnetosphere, the charged particle absorption signatures of Mimas, Enceladus, and Tethys are used to constrain the possible tilt and offset of Saturn's internal magnetic dipole. At \u223c 3 Saturn radii, a transient decrease was observed in the electron flux which was not due to Mimas. Characteristics of this decrease suggest the existence of additional material, perhaps another satellite, in the orbit of Mimas.", "doi": "10.1126/science.215.4532.577", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1982-01-29", "series_number": "4532", "volume": "215", "issue": "4532", "pages": "577-582" }, { "id": "authors:g27hj-9h956", "collection": "authors", "collection_id": "g27hj-9h956", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140212-075813791", "type": "article", "title": "Cosmic-ray abundances of elements with atomic number 26 \u2264 Z \u2264 40 measured on HEAO 3", "author": [ { "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": "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" } ], "abstract": "Individual elements in the cosmic radiation of even atomic number (Z) in the interval 26 \u2264 Z \u2264 40 have been resolved and their relative abundances measured. The results are inconsistent with a\ncosmic-ray source whose composition in this charge interval is dominated by r-process nucleosynthests.\nThe ratios of cosmic-ray source abundances to solar system abundances in this interval\nfollow the same general correlation with first ionization potential as for the lighter elements although\nthere are deviations in detail.", "doi": "10.1086/183602", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1981-08-01", "series_number": "3", "volume": "247", "issue": "3", "pages": "L115-L118" }, { "id": "authors:13qja-ss431", "collection": "authors", "collection_id": "13qja-ss431", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140417-151939075", "type": "article", "title": "Cosmic-Ray Abundances of Elements with Atomic Number 26 \u2264 Z \u2264 40 Measured on HEAO-3", "author": [ { "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": "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" } ], "abstract": "Individual elements in the cosmic radiation of even atomic number (Z) in the interval 26 \u2264 Z \u2264 40 have been resolved and their relative abundances measured. The results are inconsistent with a\ncosmic-ray source whose composition in this charge interval is dominated by r-process nucleosynthes1s.\nThe ratios of cosmic-ray source abundances to solar system abundances in this interval\nfollow the same general correlation with first ionization potential as for the lighter elements although\nthere are deviations in detail.", "doi": "10.1086/183602", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "1981-08-01", "series_number": "3", "volume": "247", "issue": "3", "pages": "L115-L118" }, { "id": "authors:k3vhe-24s63", "collection": "authors", "collection_id": "k3vhe-24s63", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140205-155430624", "type": "article", "title": "Energetic Charged Particles in Saturn's Magnetosphere:\n Voyager 1 Results", "author": [ { "family_name": "Vogt", "given_name": "R. E.", "clpid": "Vogt-R-E" }, { "family_name": "Chenette", "given_name": "D. L.", "clpid": "Chenette-D-L" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "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": "Schardt", "given_name": "A. W.", "clpid": "Schardt-A-W" }, { "family_name": "Trainor", "given_name": "J. H.", "clpid": "Trainor-J-H" }, { "family_name": "Lal", "given_name": "N.", "clpid": "Lal-N" }, { "family_name": "McDonald", "given_name": "F. B.", "clpid": "McDonald-F-B" } ], "abstract": "Voyager 1 provided the first look at Saturn's magnetotail and magnetosphere during relatively quiet interplanetary conditions. This report discusses the energetic particle populations of the outer magnetosphere of Saturn and absorption features associated with Titan and Rhea, and compares these observations with Pioneer 11 data of a year earlier. The trapped proton fluxes had soft spectra, represented by power laws E^\u2013\u03b3 in kinetic energy E, with \u03b3 \u223c 7 in the outer magnetosphere and \u03b3 \u223c 9 in the magnetotail. Structure associated with the magnetotial was observed as close as 10 Saturn radii (Rs) on the outbound trajectory. The proton and electron fluxes in the outer magnetosphere and in the magnetotail were variable and appeared to respond to changes in interplanetary conditions. Protons with energies \u2265 2 million electron volts had free access to the magnetosphere from interplanetary space and were not stably trapped outside \u223c 7.5 Rs.", "doi": "10.1126/science.212.4491.231", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1981-04-10", "series_number": "4491", "volume": "212", "issue": "4491", "pages": "231-234" }, { "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: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: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: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:vj0ph-jm616", "collection": "authors", "collection_id": "vj0ph-jm616", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140206-162824597", "type": "article", "title": "Voyager 2: Energetic Ions and Electrons in the Jovian Magnetosphere", "author": [ { "family_name": "Vogt", "given_name": "R. E.", "clpid": "Vogt-R-E" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Gehrels", "given_name": "N.", "clpid": "Gehrels-N" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Trainor", "given_name": "J. H.", "clpid": "Trainor-J-H" }, { "family_name": "Schardt", "given_name": "A. W.", "clpid": "Schardt-A-W" }, { "family_name": "Conlon", "given_name": "T. F.", "clpid": "Conlon-T-F" }, { "family_name": "McDonald", "given_name": "F. B.", "clpid": "McDonald-F-B" } ], "abstract": "The Voyager 2 encounter has enhanced our understanding of earlier results and provided measurements beyond 160 Jupiter radii (RJ) in the magnetotail. Significant fluxes of energetic sulfur and oxygen nuclei (4 to 15 million electron volts per nucleon) of Jovian origin were observed inside 25 RJ, and the gradient in phase space density at 12 RJ indicates that the ions are diffusing inward. A substantially longer time delay versus distance was found for proton flux maxima in the active hemisphere in the magnetotail at Jovicentric longitudes \u03bbIII, = 260\u00b0 to 320\u00b0 than in the inactive hemisphere at \u03bbIII, = 85\u00b0 to l10\u00b0. These delays can be related to the radial motion of plasma expanding into the magnetotail, and differences in the expansion speeds between the active and inactive hemispheres can produce rarefaction regions in trapped particles. It is suggested that the 10-hour modulation of interplanetary Jovian electrons may be associated with the arrival at the dawn magnetopause of a rarefaction region each planetary rotation.", "doi": "10.1126/science.206.4421.984", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1979-11-23", "series_number": "4421", "volume": "206", "issue": "4421", "pages": "984-987" }, { "id": "authors:xfk3m-wkf28", "collection": "authors", "collection_id": "xfk3m-wkf28", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140417-135117781", "type": "article", "title": "Voyager 2: Energetic Ions and Electrons in the Jovian Magnetosphere", "author": [ { "family_name": "Vogt", "given_name": "R. E.", "clpid": "Vogt-R-E" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Gehrels", "given_name": "N.", "clpid": "Gehrels-N" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Trainor", "given_name": "J. H.", "clpid": "Trainor-J-H" }, { "family_name": "Schardt", "given_name": "A. W.", "clpid": "Schardt-A-W" }, { "family_name": "Conlon", "given_name": "T. F.", "clpid": "Conlon-T-F" }, { "family_name": "McDonald", "given_name": "F. B.", "clpid": "McDonald-F-B" } ], "abstract": "Abstract. The Voyager 2 encounter has enhanced our understanding of earlier\nresults and provided measurements beyond 160 Jupiter radii (RJ) in the magnetotail. Significant fluxes of energetic sulfur and oxygen nuclei (4 to 15 million electron volts per nucleon) of Jovian origin were observed inside 25R^j, and the gradient in phase space density at 12 R^J indicates that the ions are diffusing inward. A substantially longer time delay versus distance was found for proton flux maxima in the active\nhemisphere in the magnetotail at Jovicentric longitudes Am = 260\u00b0 to 320\u00b0 than in the inactive hemisphere at Am = 85\u00b0 to 110\u00b0. These delays can be related to the radial motion of plasma expanding into the magnetotail, and differences in the expansion speeds between the active and inactive hemispheres can produce rarefaction regions in trapped particles. It is suggested that the JO-hour modulation of interplanetary Jovian electrons may be associated with the arrival at the dawn magnetopause of a rarefaction region each planetary rotation.", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1979-11-13", "series_number": "4421", "volume": "206", "issue": "4421", "pages": "984-987" }, { "id": "authors:h254q-afn90", "collection": "authors", "collection_id": "h254q-afn90", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140205-163501718", "type": "article", "title": "Voyager 1: Energetic Ions and Electrons in the Jovian Magnetosphere", "author": [ { "family_name": "Vogt", "given_name": "R. E.", "clpid": "Vogt-R-E" }, { "family_name": "Cook", "given_name": "W. R.", "clpid": "Cook-W-R" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "family_name": "Garrard", "given_name": "T. L.", "clpid": "Garrard-T-L" }, { "family_name": "Gehrels", "given_name": "N.", "clpid": "Gehrels-N" }, { "family_name": "Stone", "given_name": "E. C.", "orcid": "0000-0002-2010-5462", "clpid": "Stone-E-C" }, { "family_name": "Trainor", "given_name": "J. H.", "clpid": "Trainor-J-H" }, { "family_name": "Schardt", "given_name": "A. W.", "clpid": "Schardt-A-W" }, { "family_name": "Conlon", "given_name": "T.", "clpid": "Conlon-T" }, { "family_name": "Lal", "given_name": "N.", "clpid": "Lal-N" }, { "family_name": "McDonald", "given_name": "F. B.", "clpid": "McDonald-F-B" } ], "abstract": "The observations of the cosmic-ray subsystem have added significantly to our knowledge of Jupiter's magnetosphere. The most surprising result is the existence of energetic sulfur, sodium, and oxygen nuclei with energies above 7 megaelectron volts per nucleon which were found inside of Io's orbit. Also, significant fluxes of similarly energetic ions reflecting solar cosmic-ray composition were observed\nthroughout the magnetosphere beyond 11 times the radius of Jupiter. It was also found that energetic protons are enhanced by 30 to 70 percent in the active\nhemisphere. Finally, the first observations were made of the magnetospheric tail in the dawn direction out to 160 Jupiter radii.", "doi": "10.1126/science.204.4396.1003", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1979-06-01", "series_number": "4396", "volume": "204", "issue": "4396", "pages": "1003-1007" }, { "id": "authors:3m3nj-nnj50", "collection": "authors", "collection_id": "3m3nj-nnj50", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140414-110553333", "type": "article", "title": "The Voyager Cosmic Ray Experiment", "author": [ { "family_name": "Stilwell", "given_name": "D. E.", "clpid": "Stilwell-D-E" }, { "family_name": "Davis", "given_name": "W. D.", "clpid": "Davis-W-D" }, { "family_name": "Joyce", "given_name": "R. M.", "clpid": "Joyce-R-M" }, { "family_name": "McDonald", "given_name": "F. B.", "clpid": "McDonald-F-B" }, { "family_name": "Trainor", "given_name": "J. H.", "clpid": "Trainor-J-H" }, { "family_name": "Althouse", "given_name": "W. E.", "clpid": "Althouse-W-E" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "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 Voyager Cosmic Ray Experiment includes seven dE/dx-\nE telescopes to measure the energy and charge of\nparticles of 1 \u2264 Z \u2264 26 in the energy range 1-500 MeV/\nnucleon and to measure electron energy in the range\n3 \u2264 E_e \u2264 110 MeV. Isotopic composition of hydrogen\nthrough sulfur in the range up to 75 MeV/nucleon can\nalso be resolved. The electronic systems include a\ndual-gain, charge sensitive preamplifier, 4096-channel\npulse height analyzers for three parameter analysis of\nselected events, and an event type readout polling\nscheme to maximize the use of available telemetry\nspace and to enhance the occurrence of rare events in\nthe data. Details of the detector, electronic and\nmechanical design are presented.", "doi": "10.1109/TNS.1979.4329683", "issn": "0018-9499", "publisher": "IEEE", "publication": "IEEE Transactions on Nuclear Science", "publication_date": "1979-02", "series_number": "1", "volume": "26", "issue": "1", "pages": "513-520" }, { "id": "authors:q892j-zpx42", "collection": "authors", "collection_id": "q892j-zpx42", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140205-074259302", "type": "article", "title": "A Cosmic Ray Isotope Spectrometer", "author": [ { "family_name": "Althouse", "given_name": "W. E.", "clpid": "Althouse-W-E" }, { "family_name": "Cummings", "given_name": "A. C.", "orcid": "0000-0002-3840-7696", "clpid": "Cummings-A-C" }, { "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": "Vogt", "given_name": "R. E.", "clpid": "Vogt-R-E" } ], "abstract": "We describe a new instrument to be flown on ISEE-C which is optimized to measure the isotopic composition of solar and galactic cosmic rays with ~5 to ~250 MeV/nucleon. A mass resolution of \u227e 0.3 AMU should be achieved for all elements with charge Z \u2264 30.", "doi": "10.1109/TGE.1978.294547", "issn": "0018-9413", "publisher": "IEEE", "publication": "IEEE Transactions on Geoscience Electronics", "publication_date": "1978-07", "series_number": "3", "volume": "16", "issue": "3", "pages": "204-207" }, { "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" }, { "id": "authors:4yc6s-ws465", "collection": "authors", "collection_id": "4yc6s-ws465", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140409-091634684", "type": "article", "title": "Solar Modulation of Cosmic-Ray Protons and He Nuclei", "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": "We present the results of a detailed, quantitative study of the\nsolar modulation of cosmic-ray protons and He nuclei. The study\nis based on: (a) observations over the 1966 to 1970 period with\nballoon- and satellite-borne instruments, (b) numerical solutions\nof the cosmic-ray transport equation, and (c) propagation parameters\nderived from studies of near-Earth and interstellar spectra\nof cosmic-ray electrons. We find that consistent, quantitatively\nsatisfactory results may be obtained with a model of solar modulation\nwhich uses a diffusion coefficient separable into functions\nof heliocentric radius and particle rigidity and in which\nadiabatic deceleration has a dominant role in shaping the low-energy\nspectra of nuclei near 1 AU.", "publisher": "Proceedings of the 13th International Cosmic Ray Conference", "publication": "Proceedings of the 13th International Cosmic Ray Conference", "publication_date": "1973", "pages": "732-737" } ]