Precision measurements by the Alpha Magnetic Spectrometer on the International Space Station of the primary cosmic-ray electron flux in the range 0.5 to 700 GeV and the positron flux in the range 0.5 to 500 GeV are presented. The electron flux and the positron flux each require a description beyond a single power-law spectrum. Both the electron flux and the positron flux change their behavior at ∼30 GeV but the fluxes are significantly different in their magnitude and energy dependence. Between 20 and 200 GeV the positron spectral index is significantly harder than the electron spectral index. The determination of the differing behavior of the spectral indices versus energy is a new observation and provides important information on the origins of cosmic-ray electrons and positrons.

Aguilar, M., Aisa, D., Alvino, A., Ambrosi, G., Andeen, K., Arruda, L., et al. (2014). Electron and Positron Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station. PHYSICAL REVIEW LETTERS, 113(12), 121102-121110 [10.1103/PhysRevLett.113.121102].

Electron and Positron Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

BOELLA, GIULIANO FILIPPO;GERVASI, MASSIMO;LA VACCA, GIUSEPPE;PENSOTTI, SIMONETTA;ROZZA, DAVIDE;TACCONI, MAURO;
2014

Abstract

Precision measurements by the Alpha Magnetic Spectrometer on the International Space Station of the primary cosmic-ray electron flux in the range 0.5 to 700 GeV and the positron flux in the range 0.5 to 500 GeV are presented. The electron flux and the positron flux each require a description beyond a single power-law spectrum. Both the electron flux and the positron flux change their behavior at ∼30 GeV but the fluxes are significantly different in their magnitude and energy dependence. Between 20 and 200 GeV the positron spectral index is significantly harder than the electron spectral index. The determination of the differing behavior of the spectral indices versus energy is a new observation and provides important information on the origins of cosmic-ray electrons and positrons.
Articolo in rivista - Articolo scientifico
Cosmic rays, electron flux, positron flux, international space station
English
121102
121110
9
Aguilar, M., Aisa, D., Alvino, A., Ambrosi, G., Andeen, K., Arruda, L., et al. (2014). Electron and Positron Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station. PHYSICAL REVIEW LETTERS, 113(12), 121102-121110 [10.1103/PhysRevLett.113.121102].
Aguilar, M; Aisa, D; Alvino, A; Ambrosi, G; Andeen, K; Arruda, L; Attig, N; Azzarello, P; Bachlechner, A; Barao, F; Barrau, A; Barrin, L; Bartoloni, A; Basara, L; Battarbee, M; Battiston, R; Bazo, J; Becker, U; Behlmann, M; Beischer, B; Berdugo, J; Bertucci, B; Bigongiari, G; Bindi, V; Bizzaglia, S; Bizzarri, M; Boella, G; de Boer, W; Bollweg, K; Bonnivard, V; Borgia, B; Borsini, S; Boschini, M; Bourquin, M; Burger, J; Cadoux, F; Cai, X; Capell, M; Caroff, S; Casaus, J; Cascioli, V; Castellini, G; Cernuda, I; Cervelli, F; Chae, M; Chang, Y; Chen, A; Chen, H; Cheng, G; Chen, H; Cheng, L; Chikanian, A; Chou, H; Choumilov, E; Choutko, V; Chung, C; Clark, C; Clavero, R; Coignet, G; Consolandi, C; Contin, A; Corti, C; Coste, B; Cui, Z; Dai, M; Delgado, C; Della Torre, S; Demirköz, M; Derome, L; Di Falco, S; Di Masso, L; Dimiccoli, F; Díaz, C; von Doetinchem, P; Du, W; Duranti, M; D’Urso, D; Eline, A; Eppling, F; Eronen, T; Fan, Y; Farnesini, L; Feng, J; Fiandrini, E; Fiasson, A; Finch, E; Fisher, P; Galaktionov, Y; Gallucci, G; García, B; García López, R; Gast, H; Gebauer, I; Gervasi, M; Ghelfi, A; Gillard, W; Giovacchini, F; Goglov, P; Gong, J; Goy, C; Grabski, V; Grandi, D; Graziani, M; Guandalini, C; Guerri, I; Guo, K; Habiby, M; Haino, S; Han, K; He, Z; Heil, M; Hoffman, J; Hsieh, T; Huang, Z; Huh, C; Incagli, M; Ionica, M; Jang, W; Jinchi, H; Kanishev, K; Kim, G; Kim, K; Kirn, T; Kossakowski, R; Kounina, O; Kounine, A; Koutsenko, V; Krafczyk, M; Kunz, S; LA VACCA, G; Laudi, E; Laurenti, G; Lazzizzera, I; Lebedev, A; Lee, H; Lee, S; Leluc, C; Li, H; Li, J; Li, Q; Li, Q; Li, T; Li, W; Li, Y; Li, Z; Li, Z; Lim, S; Lin, C; Lipari, P; Lippert, T; Liu, D; Liu, H; Lomtadze, T; Lu, M; Lu, Y; Luebelsmeyer, K; Luo, F; Luo, J; Lv, S; Majka, R; Malinin, A; Mañá, C; Marín, J; Martin, T; Martínez, G; Masi, N; Maurin, D; Menchaca Rocha, A; Meng, Q; Mo, D; Morescalchi, L; Mott, P; Müller, M; Ni, J; Nikonov, N; Nozzoli, F; Nunes, P; Obermeier, A; Oliva, A; Orcinha, M; Palmonari, F; Palomares, C; Paniccia, M; Papi, A; Pedreschi, E; Pensotti, S; Pereira, R; Pilo, F; Piluso, A; Pizzolotto, C; Plyaskin, V; Pohl, M; Poireau, V; Postaci, E; Putze, A; Quadrani, L; Qi, X; Rancoita, P; Rapin, D; Ricol, J; Rodríguez, I; Rosier Lees, S; Rozhkov, A; Rozza, D; Sagdeev, R; Sandweiss, J; Saouter, P; Sbarra, C; Schael, S; Schmidt, S; Schuckardt, D; von Dratzig, A; Schwering, G; Scolieri, G; Seo, E; Shan, B; Shan, Y; Shi, J; Shi, X; Shi, Y; Siedenburg, T; Son, D; Spada, F; Spinella, F; Sun, W; Sun, W; Tacconi, M; Tang, C; Tang, X; Tang, Z; Tao, L; Tescaro, D; Ting, S; Ting, S; Tomassetti, N; Torsti, J; Türkoğlu, C; Urban, T; Vagelli, V; Valente, E; Vannini, C; Valtonen, E; Vaurynovich, S; Vecchi, M; Velasco, M; Vialle, J; Wang, L; Wang, Q; Wang, R; Wang, X; Wang, Z; Weng, Z; Whitman, K; Wienkenhöver, J; Wu, H; Xia, X; Xie, M; Xie, S; Xiong, R; Xin, G; Xu, N; Xu, W; Yan, Q; Yang, J; Yang, M; Ye, Q; Yi, H; Yu, Y; Yu, Z; Zeissler, S; Zhang, J; Zhang, M; Zhang, X; Zhang, Z; Zheng, Z; Zhuang, H; Zhukov, V; Zichichi, A; Zimmermann, N; Zuccon, P; Zurbach, C
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/53199
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