Towards Understanding the Origin of Cosmic-Ray Positrons

M. Aguilar, L. Ali Cavasonza, G. Ambrosi, L. Arruda, N. Attig, P. Azzarello, A. Bachlechner, F. Barao, A. Barrau, L. Barrin, A. Bartoloni, L. Basara, S. Başeǧmez-Du Pree, R. Battiston, U. Becker, M. Behlmann, B. Beischer, J. Berdugo, B. Bertucci, V. BindiW. De Boer, K. Bollweg, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, X. D. Cai, M. Capell, S. Caroff, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, M. Crispoltoni, Z. Cui, K. Dadzie, Y. M. Dai, A. Datta, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, F. Dimiccoli, C. Díaz, P. Von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, T. Eronen, J. Feng, E. Fiandrini, P. Fisher, V. Formato, Y. Galaktionov, R. J. García-López, C. Gargiulo, H. Gast, I. Gebauer, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, K. H. Guo, S. Haino, K. C. Han, Z. H. He, M. Heil, T. H. Hsieh, H. Huang, Z. C. Huang, M. Incagli, Yi Jia, H. Jinchi, K. Kanishev, B. Khiali, Th Kirn, C. Konak, O. Kounina, A. Kounine, V. Koutsenko, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, A. Lebedev, H. T. Lee, S. C. Lee, C. Leluc, J. Q. Li, Q. Li, T. X. Li, Z. H. Li, C. Light, C. H. Lin, T. Lippert, F. Z. Liu, Hu Liu, Z. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, F. Luo, J. Z. Luo, Xi Luo, S. S. Lyu, F. MacHate, C. Mañá, J. Marín, T. Martin, G. Martínez, N. Masi, D. Maurin, A. Menchaca-Rocha, Q. Meng, D. C. Mo, M. Molero, P. Mott, L. Mussolin, T. Nelson, J. Q. Ni, N. Nikonov, F. Nozzoli, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, C. Perrina, H. D. Phan, N. Picot-Clemente, V. Plyaskin, M. Pohl, V. Poireau, A. Popkow, L. Quadrani, X. M. Qi, X. Qin, Z. Y. Qu, P. G. Rancoita, D. Rapin, A. Reina Conde, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, C. Solano, S. Schael, S. M. Schmidt, A. Schulz Von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, J. Y. Shi, T. Siedenburg, J. W. Song, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C.C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, T. Urban, V. Vagelli, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, J. Vizán, L. Q. Wang, N. H. Wang, Q. L. Wang, X. Wang, X. Q. Wang, Z. X. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, H. Yi, Y. J. Yu, Z. Q. Yu, M. Zannoni, S. Zeissler, C. Zhang, F. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, N. Zimmermann, P. Zuccon

研究成果: Article同行評審

111 引文 斯高帕斯(Scopus)

摘要

Precision measurements of cosmic ray positrons are presented up to 1 TeV based on 1.9 million positrons collected by the Alpha Magnetic Spectrometer on the International Space Station. The positron flux exhibits complex energy dependence. Its distinctive properties are (a) a significant excess starting from 25.2±1.8 GeV compared to the lower-energy, power-law trend, (b) a sharp dropoff above 284-64+91 GeV, (c) in the entire energy range the positron flux is well described by the sum of a term associated with the positrons produced in the collision of cosmic rays, which dominates at low energies, and a new source term of positrons, which dominates at high energies, and (d) a finite energy cutoff of the source term of Es=810-180+310 GeV is established with a significance of more than 4σ. These experimental data on cosmic ray positrons show that, at high energies, they predominantly originate either from dark matter annihilation or from other astrophysical sources.

原文English
文章編號041102
期刊Physical review letters
122
發行號4
DOIs
出版狀態Published - 2019

All Science Journal Classification (ASJC) codes

  • 物理與天文學 (全部)

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