COSMIC-RAY PROTON AND HELIUM SPECTRA FROM THE FIRST CREAM FLIGHT

被引：308

作者：

Yoon, Y. S. ^{[1
,2
]}

Ahn, H. S. ^{[1
]}

Allison, P. S. ^{[3
]}

Bagliesi, M. G. ^{[4
,5
]}

Beatty, J. J. ^{[3
]}

Bigongiari, G. ^{[4
,5
]}

Boyle, P. J. ^{[6
,7
]}

Childers, J. T. ^{[8
]}

Conklin, N. B. ^{[9
]}

Coutu, S. ^{[9
]}

DuVernois, M. A. ^{[8
]}

Ganel, O. ^{[1
]}

Han, J. H. ^{[1
]}

Jeon, J. A. ^{[10
]}

Kim, K. C. ^{[1
]}

Lee, M. H. ^{[1
]}

Lutz, L. ^{[1
]}

Maestro, P. ^{[4
,5
]}

Malinine, A. ^{[1
]}

Marrocchesi, P. S. ^{[4
,5
]}

Minnick, S. A. ^{[11
]}

Mognet, S. I. ^{[9
]}

Nam, S. ^{[10
]}

Nutter, S. ^{[12
]}

Park, I. H. ^{[10
]}

Park, N. H. ^{[6
,7
,10
]}

Seo, E. S. ^{[1
,2
]}

Sina, R. ^{[1
]}

Swordy, S. ^{[6
,7
]}

Wakely, S. P. ^{[6
,7
]}

Wu, J. ^{[1
]}

Yang, J. ^{[10
]}

Zei, R. ^{[4
,5
]}

Zinn, S. Y. ^{[1
]}

机构：

[1] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA

[2] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[3] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[4] Univ Siena, Dept Phys, I-53100 Siena, Italy

[5] Ist Nazl Fis Nucl, I-53100 Siena, Italy

[6] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[7] Univ Chicago, Dept Phys, Chicago, IL 60637 USA

[8] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA

[9] Penn State Univ, Dept Phys, University Pk, PA 16802 USA

[10] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea

[11] Kent State Univ, Dept Phys, New Philadelphia, OH 44663 USA

[12] No Kentucky Univ, Dept Phys & Geol, Highland Hts, KY 41099 USA

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 728卷 / 02期

关键词：

balloons; cosmic rays; instrumentation: detectors; ISM: abundances; methods: data analysis; REMNANT RX J1713.7-3946; SILICON CHARGE DETECTOR; ENERGY-SPECTRA; NUCLEI; TEV; ACCELERATION; CALORIMETER; PERFORMANCE; ENERGETICS; ELECTRONS;

D O I：

10.1088/0004-637X/728/2/122

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 similar to 38.5 km with an average atmospheric overburden of similar to 3.9 g cm(-2). Individual elements are clearly separated with a charge resolution of similar to 0.15 e (in charge units) and similar to 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).

引用

页数：8

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