Towards Understanding the Origin of Cosmic-Ray Positrons
Haino S; Oliva A; Fisher P; Diaz C; Zannoni M; Gervasi M; Yan Q; Gong J; Shan BS; Liu Z; Popkow A; Zheng ZM; Grabski V; Laudi E; Battiston R; Barrin L; Galaktionov Y; Gebauer I; Lee HT; Valente E; Tacconi M; Masi N; Coignet G; Menchaca-Rocha A; Cai XD; Maurin D; Corti C; Choutko V; Cheng L; Jinchi H; Pashnin A; Mott P; Beischer B; Wang ZX; Schwering G; Bertucci B; Chang YH; Formato V; Valtonen E; Kanishev K; Gomez-Coral DM; Guo KH; Capell M; Cervelli F; Clark C; de Boer W; Dadzie K; Nozzoli F; Demirkoz MB; Molero M; Phan HD; Eline A; Burger J; Lazzizzera I; Tomassetti N; Rosier-Lees S; Li TX; Zuccon P; Wei J; Lin CH; Qin X; Luo F; Weng ZL; Mana C; Lu YS; Burger WJ; Behlmann M; Chen GM; Pohl M; Yang Y; Fiandrini E; Lu SQ; Della Torre S; Zhang JH; Martinez G; Hsieh TH; Wang XQ; Qi XM; Chung CH; Plyaskin V; Machate F; Siedenburg T; Perrina C; Chou HY; Li JQ; Dong F; Consolandi C; Azzarello P; Song JW; Mussolin L; Duranti M; Vagelli V; Rancoita PG; Paniccia M; Tian J; Pensotti S; Jia Y; Crispoltoni M; Quadrani L; Eronen T; Datta A; Di Falco S; Solano C; Yi H; Rapin D; Gargiulo C; Zeissler S; Wu H; Sagdeev R; Han KC; Ting SCC; Laurenti G; Donnini F; Kounina O; Koutsenko V; Zhang Z; Barao F; Light C; Zhuang HL; Seo ES; Lyu SS; Wang X; Bartoloni A; Vecchi M; Berdugo J; Liu FZ; Orcinha M; Caroff S; Pauluzzi M; Bindi V; Wang NH; Konak C; Acosta MV; Borgia B; Urban T; Kounine A; Liu H; Luebelsmeyer K; Zimmermann N; Zhang C; Li Q; Bachlechner A; Ting SM; Vialle JP; Marin J; Xiong RQ; Ni JQ; He ZH; Becker U; Lee SC; Bollweg K; Velasco M; Bourquin M; Nikonov N; Dimiccoli F; Vizan J; Egorov A; Shi JY; Bueno EF; Attig N; von Doetinchem P; Schmidt SM; Arruda L; Rozza D; Khiali B; Gast H; Tang XW; Palermo M; Basegmez-du Pree S; Boschini MJ; Lebedev A; Zhao F; Qu ZY; Graziani M; Kulemzin A; Ambrosi G; Chen Y; Yu ZQ; Dai YM; Aguilar M; Martin T; Garcia-Lopez RJ; Giovacchini F; Meng Q; Poireau V; Zhang F; Xu W; Mo DC; Nelson T; Castellini G; Huang ZC; Cavasonza LA; Derome L; Chen HS; Tang ZC; Zichichi A; La Vacca G; Li ZH; Barrau A; Cui Z; Rozhkov A; Zhukov V; Luo X; Kirn T; Delgado C; Leluc C; Yu YJ; Casaus J; Conde AR; Wang LQ; Heil M; Luo JZ; Lippert T; Picot-Clemente N; Palmonari F; Torsti J; Huang H; Sun ZT; Contin A; Wang QL; Incagli M; Feng J; von Dratzig AS; Schael S; Grandi D; Goy C; Basara L
Towards Understanding the Origin of Cosmic-Ray Positrons
AMER PHYSICAL SOC
Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2021042824275
https://urn.fi/URN:NBN:fi-fe2021042824275
Tiivistelmä
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 E-s = 810(-180)(+310) GeV is established with a significance of more than 4 sigma. 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.
Kokoelmat
- Rinnakkaistallenteet [19207]