PMO OpenIR
Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite
An, Q.1,2; Asfandiyarov, R.3; Azzarello, P.3; Bernardini, P.4,5; Bi, X. J.6,7; Cai, M. S.8,9; Chang, J.8,9; Chen, D. Y.7,8; Chen, H. F.1,2; Chen, J. L.10; Chen, W.7,8; Cui, M. Y.8; Cui, T. S.11; Dai, H. T.1,2; D'Amone, A.4,5; De Benedittis, A.4; De Mitri, I.12,13; Di Santo, M.4,5; Ding, M.7,10; Dong, T. K.8; Dong, Y. F.6; Dong, Z. X.11; Donvito, G.14; Droz, D.3; Duan, J. L.10; Duan, K. K.7,8; D'Urso, D.15,20; Fan, R. R.6; Fan, Y. Z.8,9; Fang, F.10; Feng, C. Q.1,2; Feng, L.8; Fusco, P.14,16,17; Gallo, V.3; Gan, F. J.1,2; Gao, M.6; Gargano, F.14; Gong, K.6; Gong, Y. Z.8; Guo, D. Y.6; Guo, J. H.8,9; Guo, X. L.8,9; Han, S. X.11; Hu, Y. M.8; Huang, G. S.1,2; Huang, X. Y.8; Huang, Y. Y.8; Ionica, M.15; Jiang, W.8,9; Jin, X.1,2; Kong, J.10; Lei, S. J.8; Li, S.7,8; Li, W. L.11; Li, X.8; Li, X. Q.11; Li, Y.10; Liang, Y. F.8; Liang, Y. M.11; Liao, N. H.8; Liu, C. M.1,2; Liu, H.8; Liu, J.10; Liu, S. B.1,2; Liu, W. Q.10; Liu, Y.8; Loparco, F.14,16,17; Luo, C. N.8,9; Ma, M.11; Ma, P. X.8,9; Ma, S. Y.1,2; Ma, T.8; Ma, X. Y.11; Marsella, G.4,5; Mazziotta, M. N.14; Mo, D.10; Niu, X. Y.10; Pan, X.8,9; Peng, W. X.6; Peng, X. Y.8; Qiao, R.6; Rao, J. N.11; Salinas, M. M.3; Shang, G. Z.11; Shen, W. H.11; Shen, Z. Q.7,8; Shen, Z. T.1,2; Song, J. X.11; Su, H.10; Su, M.8,18,19; Sun, Z. Y.10; Surdo, A.5; Teng, X. J.11; Tykhonov, A.3; Vitillo, S.3; Wang, C.1,2; Wang, H.11; Wang, H. Y.6; Wang, J. Z.6; Wang, L. G.11; Wang, Q.1,2; Wang, S.7,8; Wang, X. H.10; Wang, X. L.1,2; Wang, Y. F.1,2; Wang, Y. P.7,8; Wang, Y. Z.7,8; Wang, Z. M.12,13; Wei, D. M.8,9; Wei, J. J.8; Wei, Y. F.1,2; Wen, S. C.1,2; Wu, D.6; Wu, J.8,9; Wu, L. B.1,2; Wu, S. S.11; Wu, X.3; Xi, K.10; Xia, Z. Q.8,9; Xu, H. T.11; Xu, Z. H.8,9; Xu, Z. L.8; Xu, Z. Z.1,2; Xue, G. F.11; Yang, H. B.10; Yang, P.10; Yang, Y. Q.10; Yang, Z. L.10; Yao, H. J.10; Yu, Y. H.10; Yuan, Q.8,9; Yue, C.7,8; Zang, J. J.8; Zhang, F.6; Zhang, J. Y.6; Zhang, J. Z.10; Zhang, P. F.8; Zhang, S. X.10; Zhang, W. Z.11; Zhang, Y.7,8; Zhang, Y. J.10; Zhang, Y. L.1,2; Zhang, Y. P.10; Zhang, Y. Q.7,8; Zhang, Z.8; Zhang, Z. Y.1,2; Zhao, H.6; Zhao, H. Y.10; Zhao, X. F.11; Zhou, C. Y.11; Zhou, Y.10; Zhu, X.1,2; Zhu, Y.11; Zimmer, S.3
2019-09-01
Source PublicationSCIENCE ADVANCES
ISSN2375-2548
Volume5Issue:9Pages:10
Corresponding AuthorAn, Q.()
AbstractThe precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with 21/2 years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to similar to 100 TeV with high statistics. The measured spectrum confirms the spectral hardening at similar to 300 GeV found by previous experiments and reveals a softening at similar to 13.6 TeV, with the spectral index changing from similar to 2.60 to similar to 2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays.
DOI10.1126/sciadv.aax3793
WOS KeywordENERGY ; PAMELA ; CALIBRATION ; NUCLEI
Indexed BySCI
Language英语
WOS Research AreaScience & Technology - Other Topics
WOS SubjectMultidisciplinary Sciences
WOS IDWOS:000491128800094
PublisherAMER ASSOC ADVANCEMENT SCIENCE
Citation statistics
Document Type期刊论文
Identifierhttp://libir.pmo.ac.cn/handle/332002/28270
Collection中国科学院紫金山天文台
Corresponding AuthorAn, Q.
Affiliation1.Univ Sci & Technol China, State Key Lab Particle Detect & Elect, Hefei 230026, Anhui, Peoples R China
2.Univ Sci & Technol China, Dept Modern Phys, Hefei 230026, Anhui, Peoples R China
3.Univ Geneva, Dept Nucl & Particle Phys, CH-1211 Geneva, Switzerland
4.Univ Salento, Dipartimento Matemat & Fis E De Giorgi, I-73100 Lecce, Italy
5.INFN, Sez Lecce, I-73100 Lecce, Italy
6.Chinese Acad Sci, Inst High Energy Phys, Yuquan Rd 19B, Beijing 100049, Peoples R China
7.Univ Chinese Acad Sci, Yuquan Rd 19A, Beijing 100049, Peoples R China
8.Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210033, Jiangsu, Peoples R China
9.Univ Sci & Technol China, Sch Astron & Space Sci, Hefei 230026, Anhui, Peoples R China
10.Chinese Acad Sci, Inst Modern Phys, Nanchang Rd 509, Lanzhou 730000, Gansu, Peoples R China
11.Chinese Acad Sci, Natl Space Sci Ctr, Nanertiao 1, Beijing 100190, Peoples R China
12.GSSI, Via Iacobucci 2, I-67100 Laquila, Italy
13.INFN, Lab Nazl Gran Sasso, I-67100 Laquila, Italy
14.INFN, Sez Bari, I-70125 Bari, Italy
15.INFN, Sez Perugia, I-06123 Perugia, Italy
16.Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy
17.Politecn Bari, I-70126 Bari, Italy
18.Univ Hong Kong, Dept Phys, Pok Fu Lam, Hong Kong, Peoples R China
19.Univ Hong Kong, Lab Space Res, Pok Fu Lam, Hong Kong, Peoples R China
20.Univ Sassari, Dipartimento Chim & Farm, I-07100 Sassari, Italy
Recommended Citation
GB/T 7714
An, Q.,Asfandiyarov, R.,Azzarello, P.,et al. Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite[J]. SCIENCE ADVANCES,2019,5(9):10.
APA An, Q..,Asfandiyarov, R..,Azzarello, P..,Bernardini, P..,Bi, X. J..,...&Zimmer, S..(2019).Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite.SCIENCE ADVANCES,5(9),10.
MLA An, Q.,et al."Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite".SCIENCE ADVANCES 5.9(2019):10.
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