Cosmic-Ray Boron Flux Measured from 8.4 GeV/n to 3.8 TeV/n with the Calorimetric Electron Telescope on the International Space Station

被引：26

作者：

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

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

Asano, K. ^{[5
]}

Asaoka, Y. ^{[5
]}

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

Bigongiari, G. ^{[6
,7
]}

Binns, W. R. ^{[8
,9
]}

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

Brogi, P. ^{[6
,7
]}

Bruno, A. ^{[10
]}

Buckley, J. H. ^{[8
,9
]}

Cannady, N. ^{[11
,12
,13
]}

Castellini, G. ^{[14
]}

Checchia, C. ^{[6
,7
]}

Cherry, M. L. ^{[15
]}

Collazuol, G. ^{[16
,17
]}

de Nolfo, G. A. ^{[10
]}

Ebisawa, K. ^{[18
]}

Ficklin, A. W. ^{[15
]}

Fuke, H. ^{[18
]}

Gonzi, S. ^{[1
,2
]}

Guzik, T. G. ^{[15
]}

Hams, T. ^{[11
]}

Hibino, K. ^{[19
]}

Ichimura, M. ^{[20
]}

Ioka, K. ^{[21
]}

Ishizaki, W. ^{[5
]}

Israe, M. H. ^{[8
,9
]}

Kasahara, K. ^{[22
]}

Kataoka, J. ^{[23
]}

Kataoka, R. ^{[24
]}

Katayose, Y. ^{[25
]}

Kato, C. ^{[26
]}

Kawanaka, N. ^{[21
]}

Kawakubo, Y. ^{[15
]}

Kobayashi, K. ^{[3
,4
]}

Kohri, K. ^{[27
]}

Krawczynski, H. S. ^{[8
,9
]}

Krizmanic, J. F. ^{[12
]}

Maestro, P. ^{[6
,7
]}

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

Messineo, A. M. ^{[7
,28
]}

Mitchell, J. W. ^{[12
]}

Miyake, S. ^{[29
]}

Moiseev, A. A. ^{[12
,13
,30
]}

Mori, M. ^{[31
]}

Mori, N. ^{[2
]}

Motz, H. M. ^{[32
]}

Munakata, K. ^{[26
]}

Nakahira, S. ^{[18
]}

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] Waseda Univ, Waseda Res Inst Sci & Engn, Shinjuku Ku, 17 Kikuicho, Tokyo 1620044, Japan

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

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

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

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

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

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

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

[11] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, 1000 Hilltop Circle, Baltimore, MD 21250 USA

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

[13] NASA GSFC, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA

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

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

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

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

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

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

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

[21] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kitashirakawa Oiwakecho, Kyoto 6068502, Japan

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

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

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

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

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

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

[28] Univ Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy

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

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

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

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

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

[34] Natl Inst Informat & Commun Technol, Quantum ICT Adv Dev Ctr, 4-2-1 Nukui Kitamachi, Koganei, Tokyo 1848795, Japan

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

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

[37] Osaka Metropolitan Univ, Grad Sch Sci, Sumiyoshi Ku, 3-3-138 Sugimoto, Osaka 5588585, Japan

[38] Osaka Metropolitan Univ, Nambu Yoichiro Inst Theoret & Expt Phys, Sumiyoshi Ku, 3-3-138 Sugimoto, Osaka 5588585, Japan

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

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

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

来源：

PHYSICAL REVIEW LETTERS | 2022年 / 129卷 / 25期

关键词：

ENERGY-SPECTRA; NUCLEI; SECONDARY; PROPAGATION;

D O I：

10.1103/PhysRevLett.129.251103

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

We present the measurement of the energy dependence of the boron flux in cosmic rays and its ratio to the carbon flux in an energy interval from 8.4 GeV/n to 3.8 TeV/n based on the data collected by the Calorimetric Electron Telescope (CALET) during similar to 6.4 yr of operation on the International Space Station. An update of the energy spectrum of carbon is also presented with an increase in statistics over our previous measurement. The observed boron flux shows a spectral hardening at the same transition energy E0 similar to 200 GeV/n of the C spectrum, though B and C fluxes have different energy dependences. The spectral index of the B spectrum is found to be gamma = -3.047 +/- 0.024 in the interval 25 < E < 200 GeV/n. The B spectrum hardens by Delta gamma(B) = 0.25 +/- 0.12, while the best fit value for the spectral variation of C is Delta gamma(C) = 0.19 +/- 0.03. The B/C flux ratio is compatible with a hardening of 0.09 +/- 0.05, though a single power-law energy dependence cannot be ruled out given the current statistical uncertainties. A break in the B/C ratio energy dependence would support the recent AMS-02 observations that secondary cosmic rays exhibit a stronger hardening than primary ones. We also perform a fit to the B/C ratio with a leaky-box model of the cosmic-ray propagation in the Galaxy in order to probe a possible residual value lambda(0) of the mean escape path length lambda at high energy. We find that our B/C data are compatible with a nonzero value of lambda(0), which can be interpreted as the column density of matter that cosmic rays cross within the acceleration region.

引用

页数：7

共 39 条

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