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Phys Rev Lett. 2016 Dec 2;117(23):231102. Epub 2016 Nov 28.

Precision Measurement of the Boron to Carbon Flux Ratio in Cosmic Rays from 1.9 GV to 2.6 TV with the Alpha Magnetic Spectrometer on the International Space Station.

Aguilar M1, Ali Cavasonza L2, Ambrosi G3, Arruda L4, Attig N5, Aupetit S6, Azzarello P7, Bachlechner A2, Barao F4, Barrau A6, Barrin L8, Bartoloni A9, Basara L10, Başeğmez-du Pree S11, Battarbee M12, Battiston R10,13, Becker U14, Behlmann M14, Beischer B2, Berdugo J1, Bertucci B3,15, Bindel KF16, Bindi V17, Boella G18,19, de Boer W16, Bollweg K20, Bonnivard V6, Borgia B9,21, Boschini MJ18, Bourquin M7, Bueno EF22, Burger J14, Cadoux F7, Cai XD14, Capell M14, Caroff S23, Casaus J1, Castellini G24, Cervelli F25, Chae MJ26, Chang YH27, Chen AI14, Chen GM11, Chen HS11, Cheng L28, Chou HY27, Choumilov E14, Choutko V14, Chung CH2, Clark C20, Clavero R29, Coignet G23, Consolandi C17, Contin A30,31, Corti C17, Creus W32, Crispoltoni M8,3,15, Cui Z28, Dai YM33, Delgado C1, Della Torre S18, Demakov O14, Demirköz MB34, Derome L6, Di Falco S25, Dimiccoli F10,13, Díaz C1, von Doetinchem P17, Dong F35, Donnini F8,3,15, Duranti M3,15, D'Urso D3, Egorov A14, Eline A14, Eronen T12, Feng J32, Fiandrini E3,15, Finch E36, Fisher P14, Formato V8,3, Galaktionov Y14, Gallucci G25, García B1, García-López RJ29, Gargiulo C8, Gast H2, Gebauer I16, Gervasi M18,19, Ghelfi A6, Giovacchini F1, Goglov P14, Gómez-Coral DM37, Gong J35, Goy C23, Grabski V37, Grandi D18, Graziani M3,15, Guo KH38, Haino S32, Han KC39, He ZH38, Heil M14, Hoffman J17, Hsieh TH14, Huang H32, Huang ZC38, Huh C40, Incagli M25, Ionica M3, Jang WY40, Jinchi H39, Kang SC40, Kanishev K10,13, Kim GN40, Kim KS40, Kirn T2, Konak C34, Kounina O14, Kounine A14, Koutsenko V14, Krafczyk MS14, La Vacca G18, Laudi E8, Laurenti G30, Lazzizzera I10,13, Lebedev A14, Lee HT41, Lee SC32, Leluc C7, Li HS42, Li JQ14, Li JQ35, Li Q35, Li TX38, Li W43, Li Y7, Li ZH11, Li ZY32, Lim S40, Lin CH32, Lipari P9, Lippert T5, Liu D27, Liu H1, Lordello VD22, Lu SQ32, Lu YS11, Luebelsmeyer K2, Luo F28, Luo JZ35, Lv SS38, Machate F2, Majka R36, Mañá C1, Marín J1, Martin T20, Martínez G1, Masi N30, Maurin D6, Menchaca-Rocha A37, Meng Q35, Mikuni VM22, Mo DC38, Morescalchi L25, Mott P20, Nelson T17, Ni JQ38, Nikonov N2, Nozzoli F3, Oliva A1, Orcinha M4, Palmonari F30,31, Palomares C1, Paniccia M7, Pauluzzi M3,15, Pensotti S18,19, Pereira R17, Picot-Clemente N44, Pilo F25, Pizzolotto C3, Plyaskin V14, Pohl M7, Poireau V23, Putze A23, Quadrani L30,31, Qi XM38, Qin X3, Qu ZY32, Räihä T2, Rancoita PG18, Rapin D7, Ricol JS6, Rosier-Lees S23, Rozhkov A14, Rozza D18, Sagdeev R45, Sandweiss J36, Saouter P7, Schael S2, Schmidt SM5, Schulz von Dratzig A2, Schwering G2, Seo ES44, Shan BS43, Shi JY35, Siedenburg T2, Son D40, Song JW28, Sun WH14, Tacconi M18, Tang XW11, Tang ZC11, Tao L23, Tescaro D29, Ting SC14,8, Ting SM14, Tomassetti N3,15, Torsti J12, Türkoğlu C34, Urban T20, Vagelli V3,15, Valente E9,21, Vannini C25, Valtonen E12, Vázquez Acosta M29, Vecchi M22, Velasco M1, Vialle JP23, Vitale V3, Vitillo S7, Wang LQ28, Wang NH28, Wang QL33, Wang X14, Wang XQ11, Wang ZX38, Wei CC32, Weng ZL14, Whitman K17, Wienkenhöver J2, Wu H35, Wu X7, Xia X1, Xiong RQ35, Xu W14, Yan Q14, Yang J26, Yang M11, Yang Y42, Yi H35, Yu YJ33, Yu ZQ11, Zeissler S16, Zhang C11, Zhang J14, Zhang JH35, Zhang SD14, Zhang SW11, Zhang Z14, Zheng ZM43, Zhu ZQ14, Zhuang HL11, Zhukov V2, Zichichi A30,31, Zimmermann N2, Zuccon P14; AMS Collaboration.

Author information

1
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain.
2
I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany.
3
INFN Sezione di Perugia, I-06100 Perugia, Italy.
4
Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal.
5
Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany.
6
Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France.
7
DPNC, Université de Genève, CH-1211 Genève 4, Switzerland.
8
European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland.
9
INFN Sezione di Roma 1, I-00185 Roma, Italy.
10
INFN TIFPA, I-38123 Povo, Trento, Italy.
11
Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China.
12
Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland.
13
Università di Trento, I-38123 Povo, Trento, Italy.
14
Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
15
Università di Perugia, I-06100 Perugia, Italy.
16
Institut für Experimentelle Kernphysik, Karlsruhe Institute of Technology (KIT), D-76128 Karlsruhe, Germany.
17
Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA.
18
INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy.
19
Università di Milano-Bicocca, I-20126 Milano, Italy.
20
National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA.
21
Università di Roma La Sapienza, I-00185 Roma, Italy.
22
Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970 São Carlos, São Paulo, Brazil.
23
Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France.
24
CNR-IROE, I-50125 Firenze, Italy.
25
INFN Sezione di Pisa, I-56100 Pisa, Italy.
26
Department of Physics, Ewha Womans University, Seoul 120-750, Korea.
27
National Central University (NCU), Chung-Li, Tao Yuan 32054, Taiwan.
28
Shandong University (SDU), Jinan, Shandong, 250100 China.
29
Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain.
30
INFN Sezione di Bologna, I-40126 Bologna, Italy.
31
Università di Bologna, I-40126 Bologna, Italy.
32
Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan.
33
Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China.
34
Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey.
35
Southeast University (SEU), Nanjing 210096, China.
36
Physics Department, Yale University, New Haven, Connecticut 06520, USA.
37
Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico.
38
Sun Yat-Sen University (SYSU), Guangzhou 510275, China.
39
National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan 32546, Taiwan.
40
CHEP, Kyungpook National University, 41566 Daegu, Korea.
41
Academia Sinica Grid Center (ASGC), Nankang, Taipei 11529, Taiwan.
42
National Cheng Kung University, Tainan 70101, Taiwan.
43
Beihang University (BUAA), Beijing 100191, China.
44
IPST, University of Maryland, College Park, Maryland 20742, USA.
45
East-West Center for Space Science, University of Maryland, College Park, Maryland 20742, USA.

Abstract

Knowledge of the rigidity dependence of the boron to carbon flux ratio (B/C) is important in understanding the propagation of cosmic rays. The precise measurement of the B/C ratio from 1.9 GV to 2.6 TV, based on 2.3 million boron and 8.3 million carbon nuclei collected by AMS during the first 5 years of operation, is presented. The detailed variation with rigidity of the B/C spectral index is reported for the first time. The B/C ratio does not show any significant structures in contrast to many cosmic ray models that require such structures at high rigidities. Remarkably, above 65 GV, the B/C ratio is well described by a single power law R^{Δ} with index Δ=-0.333±0.014(fit)±0.005(syst), in good agreement with the Kolmogorov theory of turbulence which predicts Δ=-1/3 asymptotically.

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