Towards Understanding the Origin of Cosmic-Ray Positrons
- Aguilar, M.
- Ali Cavasonza, L.
- Ambrosi, G.
- Arruda, L.
- Attig, N.
- Azzarello, P.
- Bachlechner, A.
- Barao, F.
- Barrau, A.
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- Basara, L.
- Başeğmez-du Pree, S.
- Battiston, R.
- Beischer, B.
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- Bertucci, B.
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- de Boer, W.
- Bollweg, K.
- Borgia, B.
- Boschini, M. J.
- Bourquin, M.
- Bueno, E. F.
- Caroff, S.
- Casaus, J.
- Castellini, G.
- Cervelli, F.
- Chang, Y. H.
- Chen, G. M.
- Chen, H. S.
- Chen, Y.
- Cheng, L.
- Chou, H. Y.
- Chung, C. H.
- Clark, C.
- Coignet, G.
- Consolandi, C.
- Contin, A.
- Corti, C.
- Crispoltoni, M.
- Cui, Z.
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- Datta, A.
- Delgado, C.
- Della Torre, S.
- Demirköz, M. B.
- Derome, L.
- Di Falco, S.
- Dimiccoli, F.
- Díaz, C.
- von Doetinchem, P.
- Dong, F.
- Donnini, F.
- Duranti, M.
- Eronen, T.
- Feng, J.
- Fiandrini, E.
- Formato, V.
- García-López, R. J.
- Gargiulo, C.
- Gast, H.
- Gebauer, I.
- Gervasi, M.
- Giovacchini, F.
- Gómez-Coral, D. M.
- Gong, J.
- Goy, C.
- Grabski, V.
- Grandi, D.
- Graziani, M.
- Guo, K. H.
- Haino, S.
- Han, K. C.
- He, Z. H.
- Huang, H.
- Huang, Z. C.
- Incagli, M.
- Jinchi, H.
- Kanishev, K.
- Khiali, B.
- Kirn, Th.
- Konak, C.
- La Vacca, G.
- Laudi, E.
- Laurenti, G.
- Lazzizzera, I.
- Lee, H. T.
- Lee, S. C.
- Leluc, C.
- Li, J. Q.
- Li, Q.
- Li, T. X.
- Li, Z. H.
- Light, C.
- Lin, C. H.
- Lippert, T.
- Liu, Z.
- Lu, S. Q.
- Lu, Y. S.
- Luebelsmeyer, K.
- Luo, F.
- Luo, J. Z.
- Luo, Xi
- Lyu, S. S.
- Machate, F.
- Mañá, C.
- Marín, J.
- Martin, T.
- Martínez, G.
- Masi, N.
- Maurin, D.
- Menchaca-Rocha, A.
- Meng, Q.
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- Molero, M.
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- Mussolin, L.
- Nelson, T.
- Ni, J. Q.
- Nikonov, N.
- Nozzoli, F.
- Oliva, A.
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- Palermo, M.
- Palmonari, F.
- Paniccia, M.
- Pauluzzi, M.
- Pensotti, S.
- Perrina, C.
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- Pohl, M.
- Poireau, V.
- Popkow, A.
- Quadrani, L.
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- Rapin, D.
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- Rosier-Lees, S.
- Rozhkov, A.
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- Sagdeev, R.
- Solano, C.
- Schael, S.
- Schmidt, S. M.
- Schulz von Dratzig, A.
- Schwering, G.
- Seo, E. S.
- Shan, B. S.
- Shi, J. Y.
- Siedenburg, T.
- Song, J. W.
- Sun, Z. T.
- Tacconi, M.
- Tang, X. W.
- Tang, Z. C.
- Tian, J.
- Tomassetti, N.
- Torsti, J.
- Urban, T.
- Vagelli, V.
- Valente, E.
- Valtonen, E.
- Vázquez Acosta, M.
- Vecchi, M.
- Velasco, M.
- Vialle, J. P.
- Vizán, J.
- Wang, L. Q.
- Wang, N. H.
- Wang, Q. L.
- Wang, X. Q.
- Wang, Z. X.
- Wei, J.
- Weng, Z. L.
- Wu, H.
- Xiong, R. Q.
- Xu, W.
- Yang, Y.
- Yi, H.
- Yu, Y. J.
- Yu, Z. Q.
- Zannoni, M.
- Zeissler, S.
- Zhang, C.
- Zhang, F.
- Zhang, J. H.
- Zhang, Z.
- Zhao, F.
- Zheng, Z. M.
- Zhuang, H. L.
- Zhukov, V.
- Zichichi, A.
- Zimmermann, N.
- Zuccon, P.
- Becker, Ulrich J
- Behlmann, Matthew Daniel
- Burger, Joseph D
- Cai, Xudong
- Capell, Michael H
- Choutko, Vitali
- Dadzie, K.
- Egorov, Alexander
- Eline, Alexandre
- Fisher, Peter H
- Galaktionov, Y.
- Heil, Melanie
- Hsieh, Timothy Hwa-wei
- Jia, Yi
- Kounina, Olga
- Kounine, Andrei
- Koutsenko, Vladimir
- Kulemzin, Alexander
- Lebedev, Alexei
- Liu, F. Z.
- Liu, Hu
- Pashnin, A.
- Phan, Huy Duc
- Plyaskin, Vasily
- Qin, Xiaoting
- Ting, Samuel
- Ting, Steve M
- Wang, X.
- Yan, Qi
DOIAbstract
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[superscript s] = 810...
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