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Yoon, Y. S; Ahn, H. S; Allison, P. S; Bagliesi, M. G; Beatty, J. J; Bigongiari, G; Boyle, P. J; Childers, J. T; Conklin, N. B; Coutu, S; DuVernois, M. A; Ganel, O; Han, J. H; Jeon, J. A; Kim, K. C; Lee, M. H; Lutz, L; Maestro, P; Malinine, A; Marrocchesi, P. S; Minnick, S. A; Mognet, S. I; Nam, S; Nutter, S; Park, I. H; Park, N. H; Seo, E. S; Sina, R; Swordy, S; Wakely, S. P; Wu, J; Yang, J; Zei, R; Zinn, S. Y
Astrophysical journal/The Astrophysical journal, 02/2011, Volume: 728, Issue: 2Journal Article
Cosmic-ray proton and helium spectra have been measured with the balloon-borne Cosmic Ray Energetics And Mass experiment flown for 42 days in Antarctica in the 2004-2005 austral summer season. High-energy cosmic-ray data were collected at an average altitude of ~38.5 km with an average atmospheric overburden of ~3.9 g cm--2. Individual elements are clearly separated with a charge resolution of ~0.15 e (in charge units) and ~0.2 e for protons and helium nuclei, respectively. The measured spectra at the top of the atmosphere are represented by power laws with a spectral index of --2.66 ? 0.02 for protons from 2.5 TeV to 250 TeV and --2.58 ? 0.02 for helium nuclei from 630 GeV nucleon--1 to 63 TeV nucleon--1. They are harder than previous measurements at a few tens of GeV nucleon--1. The helium flux is higher than that expected from the extrapolation of the power law fitted to the lower-energy data. The relative abundance of protons to helium nuclei is 9.1 ? 0.5 for the range from 2.5 TeV nucleon--1 to 63 TeV nucleon--1. This ratio is considerably smaller than the previous measurements at a few tens of GeV nucleon--1.
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