Towards Understanding the Origin of Cosmic-Ray Electrons
Burger WJ; Liu H; Zimmerman N; He ZH; Feng J; Grandi D; Ting SCC; Chen Y; Battiston R; Consolandi C; Di Felice V; Ambrosi G; Nozzoli F; Mott P; Qi XM; Sagdeev R; Cavasonza LA; Huang ZC; Phan HD; Crispoltoni M; Egorov A; Bindi V; Gast H; Pauluzzi M; Shi JY; Laudi E; von Dratzig AS; Li ZH; Wei J; Palmonari F; Borgia B; Wang XQ; Poireau V; Gebauer I; Guo KH; Della Torre S; de Boer W; Pohl M; Capell M; Yan Q; Lu YS; Basegmez-du Pree S; Zhang Z; Schmidt SM; Castellini G; Jinchi H; Datta A; Contin A; Rozza D; Goy C; Jia Y; Chen GM; Demirkoz MB; Wang X; Lin CH; Diaz C; Dimiccoli F; Laurenti G; Attig N; Becker U; Tomassetti N; Ting SM; Popkow A; La Vacca G; Rapin D; Formato V; Clark C; Pensotti S; Tang XW; Lu SQ; Weng ZL; Galaktionov Y; Xiong RQ; Gargiulo C; Vecchi M; Lipper T; Luebelsmeyer K; Palermo M; Bourquin M; Schael S; Solano C; Kulemzin A; Fiandrini E; Arruda L; Zhao F; Huang H; Li Q; Machate F; Schwering G; Xu W; Dadzie K; Bueno EF; Torsti J; Cervelli F; Wang QL; Yu YJ; Wang ZX; Bertucci B; Rozhkov A; Velasco M; Yang Y; Barrau A; Li JQ; Song JW; Gervasi M; Gong J; Acosta MV; Cui Z; Marin J; von Doetinchem P; Lee SC; Zuccon P; Nikonov N; Rancoita PG; Cheng L; Mana C; Bollweg K; Lee HT; Chou HY; Mo DC; Beischer B; Dong F; Valtonen E; Light C; Lazzizzera I; Grabski V; Bartoloni A; Eline A; Kounine A; Zhang JH; Derome L; Lyu SS; Nelson T; Sun ZT; Yi H; Lebedev A; Li TX; Luo JZ; Siedenburg T; Vagelli V; Menchaca-Rocha A; Eronen T; Conde AR; Qin X; Urban T; Kounin O; Barrin L; Zhang C; Khiali B; Choutko V; Kirn T; Wang NH; Zheng ZM; Valente E; Heil M; Chung CH; Perrina C; Ni JQ; Vizan J; Han KC; Oliva A; Delgado C; Pashnin A; Berdugo J; Basara L; Seo ES; Tacconi M; Chang YH; Corti C; Zhukov V; Hsieh TH; Di Falco S; Koutsenko V; Martin T; Wang LQ; Leluc C; Tian J; Maurin D; Shan BS; Qu ZY; Liu Z; Zichichi A; Giovacchini F; Picot-Clemente N; Wu H; Incagli M; Gomez-Coral DM; Zhuang HL; Quadrani L; Zeissler S; Donnini F; Casaus J; Aguilar M; Martinez G; Graziani M; Yu ZQ; Haino S; Kanishev K; Zannoni M; Bachlechner A; Burger J; Azzarello P; Tang ZC; Konak C; Orcinha M; Duranti M; Behlmann M; Cai XD; Coignet G; Meng Q; Mussolin L; Rosier-Lee S; Plyaskin V; Vialle JP; Alpat B; Chen HS; Fisher P; Molero M; Luo F; Garcia-Lopez RJ; Boschini MJ; Paniccia M; Zhang F; Dai YM; Liu FZ; Caroff S; Masi N; Luo X; Barao F
Towards Understanding the Origin of Cosmic-Ray Electrons
AMER PHYSICAL SOC
Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2021042824824
https://urn.fi/URN:NBN:fi-fe2021042824824
Tiivistelmä
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.
Kokoelmat
- Rinnakkaistallenteet [19207]