Towards Understanding the Origin of Cosmic-Ray Electrons

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

doi:10.1103/physrevlett.122.101101

Towards Understanding the Origin of Cosmic-Ray Electrons

Atıf İçin Kopyala

Aguilar M., Cavasonza L. A., Alpat B., Ambrosi G., Arruda L., Attig N., ...Daha Fazla

PHYSICAL REVIEW LETTERS, cilt.122, sa.10, 2019 (SCI-Expanded)

Yayın Türü: Makale / Tam Makale
Cilt numarası: 122 Sayı: 10
Basım Tarihi: 2019
Doi Numarası: 10.1103/physrevlett.122.101101
Dergi Adı: PHYSICAL REVIEW LETTERS
Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus
Orta Doğu Teknik Üniversitesi Adresli: Evet

Özet

Precision results on cosmic-ray electrons are presented in the energy range from 0.5 GeV to 1.4 TeV based on 28.1 x 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(-5.2)(+5.4) GeV compared to the lower energy trends, but the nature of this excess is different from the positron flux excess above 25.2 +/- 1.8 GeV. Contrary to the positron flux, which has an exponential energy cutoff of 810(-180)(+310) GeV, at the 5 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.