Elemental Composition at the Cosmic-Ray Source Derived from the ACE-CRIS Instrument. I. _6C to _(28)Ni

Creators: Israel, M. H.; Lave, K. A.; Wiedenbeck, M. E.; Binns, W. R.; Christian, E. R.; Cummings, A. C.; Davis, A. J.; de Nolfo, G. A.; Leske, R. A.; Mewaldt, R. A.; Stone, E. C.; von Rosenvinge, T. T.

Abstract

We report new elemental source abundances from _6C to _(28)Ni for galactic cosmic rays, using observations from the Cosmic Ray Isotope Spectrometer (CRIS) on board the NASA Advanced Composition Explorer spacecraft. Abundances were calculated using CRIS energy spectra at energies below 550 MeV/nucleon from the 1997–98 and 2009–10 solar-minimum periods, as well as from the 2001–03 solar-maximum period. These new results, when combined with results for heavier elements reported in a forthcoming paper, are consistent with a model of galactic cosmic-ray origin where nuclei found in interstellar grains are accelerated preferentially over those found in interstellar gas, with this acceleration happening in OB associations.

Additional Information

© 2018 The American Astronomical Society. Received 2018 January 29; revised 2018 July 16; accepted 2018 August 3; published 2018 September 21. NASA grants NNX08AI11G and NNX13AH66G supported the work performed at the California Institute of Technology, the Jet Propulsion Laboratory, and Washington University in St. Louis. The work done at Goddard Space Flight Center was funded by NASA through the ACE Project. We thank Nasser Barghouty for his private communication of updated partial interaction cross sections of protons on heavy nuclei, and we thank Christina Cohen for her editorial assistance in preparing this manuscript.

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