| Literature DB >> 30768313 |
M Aguilar1, L Ali Cavasonza2, G Ambrosi3, L Arruda4, N Attig5, P Azzarello6, A Bachlechner2, F Barao4, A Barrau7, L Barrin8, A Bartoloni9, L Basara10, S Başeğmez-du Pree11, R Battiston10,12, U Becker13, M Behlmann13, B Beischer2, J Berdugo1, B Bertucci3,14, V Bindi15, W de Boer16, K Bollweg17, B Borgia9,18, M J Boschini19, M Bourquin6, E F Bueno20, J Burger13, W J Burger10, X D Cai13, M Capell13, S Caroff21, J Casaus1, G Castellini22, F Cervelli23, Y H Chang24, G M Chen25, H S Chen25,26, Y Chen6, L Cheng27, H Y Chou24, V Choutko13, C H Chung2, C Clark17, G Coignet21, C Consolandi15, A Contin28,29, C Corti15, M Crispoltoni3,14, Z Cui27, K Dadzie13, Y M Dai30, A Datta15, C Delgado1, S Della Torre19, M B Demirköz31, L Derome7, S Di Falco23, F Dimiccoli8,10, C Díaz1, P von Doetinchem15, F Dong32, F Donnini3, M Duranti3, A Egorov13, A Eline13, T Eronen33, J Feng13, E Fiandrini3,14, P Fisher13, V Formato3, Y Galaktionov13, R J García-López34, C Gargiulo8, H Gast2, I Gebauer16, M Gervasi19,35, F Giovacchini1, D M Gómez-Coral36, J Gong32, C Goy21, V Grabski36, D Grandi19,35, M Graziani16, K H Guo37, S Haino38, K C Han39, Z H He37, M Heil13, T H Hsieh13, H Huang38, Z C Huang37, M Incagli23, Yi Jia13, H Jinchi39, K Kanishev10, B Khiali3, Th Kirn2, C Konak31, O Kounina13, A Kounine13, V Koutsenko13, A Kulemzin13, G La Vacca19,35, E Laudi8, G Laurenti28, I Lazzizzera10,12, A Lebedev13, H T Lee40, S C Lee38, C Leluc6, J Q Li32, Q Li32, T X Li37, Z H Li25, C Light15, C H Lin38, T Lippert5, F Z Liu13, Hu Liu13,24, Z Liu6, S Q Lu38, Y S Lu25, K Luebelsmeyer2, F Luo27, J Z Luo32, Xi Luo15, S S Lyu37, F Machate2, C Mañá1, J Marín1, T Martin17, G Martínez1, N Masi28, D Maurin7, A Menchaca-Rocha36, Q Meng32, D C Mo37, M Molero1, P Mott17, L Mussolin3,14, T Nelson15, J Q Ni37, N Nikonov2, F Nozzoli10, A Oliva1, M Orcinha4, M Palermo15, F Palmonari28,29, M Paniccia6, A Pashnin13, M Pauluzzi3,14, S Pensotti19,35, C Perrina6, H D Phan13, N Picot-Clemente41, V Plyaskin13, M Pohl6, V Poireau21, A Popkow15, L Quadrani28,29, X M Qi37, X Qin13, Z Y Qu38, P G Rancoita19, D Rapin6, A Reina Conde34, S Rosier-Lees21, A Rozhkov13, D Rozza19,35, R Sagdeev42, C Solano13, S Schael2, S M Schmidt5, A Schulz von Dratzig2, G Schwering2, E S Seo41, B S Shan43, J Y Shi32, T Siedenburg2, J W Song27, Z T Sun25, M Tacconi19,35, X W Tang25, Z C Tang25, J Tian3,14, Samuel C C Ting13,8, S M Ting13, N Tomassetti3,14, J Torsti33, T Urban17, V Vagelli3,14, E Valente9,18, E Valtonen33, M Vázquez Acosta34, M Vecchi11,20, M Velasco1, J P Vialle21, J Vizán1, L Q Wang27, N H Wang27, Q L Wang30, X Wang13, X Q Wang25,26, Z X Wang37, J Wei6, Z L Weng13, H Wu32, R Q Xiong32, W Xu13, Q Yan13, Y Yang44, H Yi32, Y J Yu30, Z Q Yu25, M Zannoni19,35, S Zeissler16, C Zhang25, F Zhang25, J H Zhang32, Z Zhang13, F Zhao25,26, Z M Zheng43, H L Zhuang25, V Zhukov2, A Zichichi28,29, N Zimmermann2, P Zuccon10,12.
Abstract
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 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.Entities:
Year: 2019 PMID： 30768313 DOI： 10.1103/PhysRevLett.122.041102
Source DB: PubMed Journal: Phys Rev Lett ISSN： 0031-9007 Impact factor: 9.161