Towards Understanding the Origin of Cosmic-Ray Electrons

作者：M. Aguilar, L. Ali Cavasonza, B. Alpat, G. Ambrosi, L. Arruda, N. Attig, P. Azzarello, A. Bachlechner, F. Barão, Aurélien Barrau, L. Barrin, A. Bartoloni, L. Basara, Seth Pree, R. Battiston, U. Becker, M. Behlmann, B. Beischer, J. Berdugo, B. Bertucci, V. Bindi, W. De Boer, K. Bollweg, B. Borgia, M. Boschini, M. Bourquin, E. F. Bueno, J.D. Burger, W. J. Burger, Xudong Cai, M. Capell, Sami Caroff, J. Casaus, G. Castellini, F. Cervelli, Yuan-Hann Chang, G. M. Chen, H. S. Chen, Y. Chen, Lin Cheng, H. Y. Chou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, M. Crispoltoni, Z. Cui, S. Kokou Dadzie, Ye Dai, A. Datta, C. Delgado, S. Della Torre, B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, F. Dimiccoli, C. Díaz, P. von Doetinchem, Fang Dong, F. Donnini, M. Duranti, A. I. Egorov, A. Eline, T. Eronen, J. H. Feng, E. Fiandrini, P.H. Fisher, V. Formato, Yu. Galaktionov, R. J. Garcı́a López, Corrado Gargiulo, H. Gast, Iris Gebauer, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, Varlen Grabski, D. Grandi, M. Graziani, K. H. Guo, S. Haino, K. C. Han, Z. H. He, M. Heil, Timothy 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, Qiang Li, T. X. Li, Z. H. Li, Christopher Light, Chao‐Hung Lin, Thomas Lippert, F. Z. Liu, Hu Liu, Zhen Liu, S. Q. Lu, Yudong Lu, K. Luebelsmeyer, Feng Luo, Junzhou Luo, Xi Luo, Shaoyu Lyu, F. Machate, C. Mañá, J. Marín, T. Martin, G. Martı́nez, N. Masi, D. Maurin, A. Menchaca-Rocha, Q. Meng, Dong-Chuan 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-Clémente, 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. Z. Sagdeev, C. Solano, S. Schael, Susann Schmidt, A. Schulz von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, J. Y. Shi, T. Siedenburg, Jiwei Song, Z. T. Sun, M. Tacconi, Xiao Tang, Zhi-Cheng Tang, Jie Tian, Samuel C.C. Ting, S.M. Ting, Nicola 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, H. Wang, Qiuliang Wang, X. Wang, X. Q. Wang, Z. X. Wang, Chuncheng Wei, Z. Weng, H. Wu, R. Q. Xiong, W. Xu, Qi Yan, Y. Yang, Han Yi, Yaxin 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 · 发表于：Physical Review Letters · 年份：2019 · DOI：10.1103/physrevlett.122.101101 · 被引用次数：162 · 研究领域：Dark Matter and Cosmic Phenomena、Astrophysics and Cosmic Phenomena、Neutrino Physics Research

Precision results on cosmic-ray electrons are presented in the energy range from 0.5 GeV to 1.4 TeV based on $28.1\ifmmode\times\else\texttimes\fi{}{10}^{6}$ electrons collected by the Alpha Magnetic Spectrometer on the International Space Station. In the entire energy range the electron and positron spectra have distinctly different magnitudes and energy dependences. The electron flux exhibits a significant excess starting from $42.{1}_{\ensuremath{-}5.2}^{+5.4}\text{ }\text{ }\mathrm{GeV}$ compared to the lower energy trends, but the nature of this excess is different from the positron flux excess above $25.2\ifmmode\pm\else\textpm\fi{}1.8\text{ }\text{ }\mathrm{GeV}$. Contrary to the positron flux, which has an exponential energy cutoff of $81{0}_{\ensuremath{-}180}^{+310}\text{ }\text{ }\mathrm{GeV}$, at the $5\ensuremath{\sigma}$ level the electron flux does not have an energy cutoff below 1.9 TeV. In the entire energy range the electron flux is well described by the sum of two power law components. The different behavior of the cosmic-ray electrons and positrons measured by the Alpha Magnetic Spectrometer is clear evidence that most high energy electrons originate from different sources than high energy positrons.