Direct Measurement of the Cosmic-Ray Proton Spectrum from 50 GeV to 10 TeV with the Calorimetric Electron Telescope on the International Space Station

被引：145

作者：

Adriani, O. ^{[1
,2
]}

Akaike, Y. ^{[3
,4
]}

Asano, K. ^{[5
]}

Asaoka, Y. ^{[6
,7
]}

Bagliesi, M. G. ^{[8
,9
]}

Berti, E. ^{[1
,2
]}

Bigongiari, G. ^{[8
,9
]}

Binns, W. R. ^{[10
,11
]}

Bonechi, S. ^{[8
,9
]}

Bongi, M. ^{[1
,2
]}

Brogi, P. ^{[8
,9
]}

Bruno, A. ^{[12
]}

Buckley, J. H. ^{[10
,11
]}

Cannady, N. ^{[13
]}

Castellini, G. ^{[14
]}

Checchia, C. ^{[15
,16
]}

Cherry, M. L. ^{[13
]}

Collazuol, G. ^{[15
,16
]}

Di Felice, V ^{[17
,18
]}

Ebisawa, K. ^{[19
]}

Fuke, H. ^{[19
]}

Guzik, T. G. ^{[13
]}

Hams, T. ^{[3
,4
,20
]}

Hasebe, N. ^{[6
]}

Hibino, K. ^{[21
]}

Ichimura, M. ^{[22
]}

Ioka, K. ^{[23
]}

Ishizaki, W. ^{[5
]}

Israel, M. H. ^{[10
,11
]}

Kasahara, K. ^{[6
]}

Kataoka, J. ^{[6
]}

Kataoka, R. ^{[24
]}

Katayose, Y. ^{[25
]}

Kato, C. ^{[26
]}

Kawanaka, N. ^{[27
,28
]}

Kawakubo, Y. ^{[13
,29
]}

Kohri, K. ^{[30
]}

Krawczynski, H. S. ^{[10
,11
]}

Krizmanic, J. F. ^{[3
,4
,20
]}

Lomtadze, T. ^{[9
]}

Maestro, P. ^{[8
,9
]}

Marrocchesi, P. S. ^{[8
,9
]}

Messineo, A. M. ^{[9
,31
]}

Mitchell, J. W. ^{[4
]}

Miyake, S. ^{[32
]}

Moiseev, A. A. ^{[4
,20
,33
]}

Mori, K. ^{[6
,19
]}

Mori, M. ^{[34
]}

Mori, N. ^{[2
]}

Motz, H. M. ^{[35
]}

机构：

[1] Univ Florence, Dept Phys, Via Sansone 1, I-50019 Sesto, Fiorentino, Italy

[2] Ist Nazl Fis Nucl, Sez Florence, Via Sansone 1, I-50019 Sesto, Fiorentino, Italy

[3] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA

[4] NASA, GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA

[5] Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778582, Japan

[6] Waseda Univ, Waseda Res Inst Sci & Engn, Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan

[7] Japan Aerosp Explorat Agcy, Human Spaceflight Technol Directorate, JEM Utilizat Ctr, 2-1-1 Sengen, Tsukuba, Ibaraki 3058505, Japan

[8] Univ Siena, Dept Phys Sci Earth & Environm, Via Roma 56, I-53100 Siena, Italy

[9] Ist Nazl Fis Nucl, Sez Pisa, Polo Fibonacci, Largo B Pontecorvo 3, I-56127 Pisa, Italy

[10] Washington Univ, Dept Phys, One Brookings Dr, St Louis, MO 63130 USA

[11] Washington Univ, McDonnell Ctr Space Sci, One Brookings Dr, St Louis, MO 63130 USA

[12] NASA, GSFC, Heliospher Phys Lab, Greenbelt, MD 20771 USA

[13] Louisiana State Univ, Dept Phys & Astron, 202 Nicholson Hall, Baton Rouge, LA 70803 USA

[14] Natl Res Council CNR, Inst Appl Phys IFAC, Via Madonna Piano 10, I-50019 Sesto, Fiorentino, Italy

[15] Univ Padua, Dept Phys & Astron, Via Marzolo 8, I-35131 Padua, Italy

[16] Ist Nazl Fis Nucl, Sez Padova, Via Marzolo 8, I-35131 Padua, Italy

[17] Univ Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy

[18] Ist Nazl Fis Nucl, Sez Rome Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy

[19] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan

[20] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA

[21] Kanagawa Univ, 3-27-1 Rokkakubashi, Yokohama, Kanagawa 2218686, Japan

[22] Hirosaki Univ, Grad Sch Sci & Technol, Fac Sci & Technol, 3 Bunkyo, Hirosaki, Aomori 0368561, Japan

[23] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan

[24] Natl Inst Polar Res, 10-3 Midori Cho, Tachikawa, Tokyo 1908518, Japan

[25] Yokohama Natl Univ, Div Intelligent Syst Engn, Fac Engn, 79-5 Tokiwadai, Yokohama, Kanagawa 2408501, Japan

[26] Shinshu Univ, Fac Sci, 3-1-1 Asahi, Matsumoto, Nagano 3908621, Japan

[27] Kyoto Univ, Hakubi Ctr, Sakyo Ku, Yoshida Honmachi, Kyoto 6068501, Japan

[28] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan

[29] Aoyama Gakuin Univ, Dept Phys & Math, Coll Sci & Engn, Chuo Ku, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 2525258, Japan

[30] High Energy Accelerator Res Org, Inst Particle & Nucl Studies, 1-1 Oho, Tsukuba, Ibaraki 3050801, Japan

[31] Univ Pisa, Polo Fibonacci, Largo B Pontecorvo 3, I-56127 Pisa, Italy

[32] Ibaraki Coll, Natl Inst Technol, Dept Elect & Elect Syst Engn, 866 Nakane, Hitachinaka, Ibaraki 3128508, Japan

[33] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[34] Ritsumeikan Univ, Coll Sci & Engn, Dept Phys Sci, Kusatsu, Shiga 5258577, Japan

[35] Waseda Univ, Global Ctr Sci & Engn, Fac Sci & Engn, Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan

[36] RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

[37] Univ Denver, Dept Phys & Astron, Phys Bldg,Room 211,2112 East Wesley Ave, Denver, CO 80208 USA

[38] ASI Sci Data Ctr ASDC, Via Politecn Snc, I-00133 Rome, Italy

[39] Nihon Univ, Coll Ind Technol, 1-2-1 Izumi, Narashino, Chiba 2758575, Japan

[40] Univ Tokyo, Kavli Inst Phys & Math Universe, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan

[41] Waseda Univ, Sch Adv Sci & Engn, Shinjuku Ku, 3-4-1 Okubo, Tokyo 1698555, Japan

[42] Osaka City Univ, Grad Sch Sci, Div Math & Phys, Sumiyoshi Ku, 3-3-138 Sugimoto, Osaka 5588585, Japan

[43] Natl Inst Quantum & Radiat Sci & Technol, Inage Ku, 4-9-1 Anagawa, Chiba 2638555, Japan

[44] Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648601, Japan

[45] Ibaraki Univ, Coll Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan

[46] Shibaura Inst Technol, Dept Elect Informat Syst, 307 Fukasaku, Minuma, Saitama 3378570, Japan

来源：

PHYSICAL REVIEW LETTERS | 2019年 / 122卷 / 18期

关键词：

SUPERNOVA-REMNANTS; ENERGY; COMPONENT; CALET;

D O I：

10.1103/PhysRevLett.122.181102

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

In this paper, we present the analysis and results of a direct measurement of the cosmic-ray proton spectrum with the CALET instrument onboard the International Space Station, including the detailed assessment of systematic uncertainties. The observation period used in this analysis is from October 13, 2015 to August 31, 2018 (1054 days). We have achieved the very wide energy range necessary to carry out measurements of the spectrum from 50 GeV to 10 TeV covering, for the first time in space, with a single instrument the whole energy interval previously investigated in most cases in separate subranges by magnetic spectrometers (BESS-TeV, PAMELA, and AMS-02) and calorimetric instruments (ATIC, CREAM, and NUCLEON). The observed spectrum is consistent with AMS-02 but extends to nearly an order of magnitude higher energy, showing a very smooth transition of the power-law spectral index from -2.81 +/- 0.03 (50-500 GeV) neglecting solar modulation effects (or -2.87 +/- 0.06 including solar modulation effects in the lower energy region) to -2.56 +/- 0.04 (1-10 TeV), thereby confirming the existence of spectral hardening and providing evidence of a deviation from a single power law by more than 3 sigma.

引用

页数：8

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