We report the observation of new properties of primary cosmic rays, neon (Ne), magnesium (Mg), and silicon (Si), measured in the rigidity range 2.15 GV to 3.0 TV with 1.8 × 10^6 Ne, 2.2 × 10^6 Mg, and 1.6 × 10^6 Si nuclei collected by the Alpha Magnetic Spectrometer experiment on the International Space Station. The Ne and Mg spectra have identical rigidity dependence above 3.65 GV. The three spectra have identical rigidity dependence above 86.5 GV, deviate from a single power law above 200 GV, and harden in an identical way. Unexpectedly, above 86.5 GV the rigidity dependence of primary cosmic rays Ne, Mg, and Si spectra is different from the rigidity dependence of primary cosmic rays He, C, and O. This shows that the Ne, Mg, and Si and He, C, and O are two different classes of primary cosmic rays.

Aguilar, M., Ali Cavasonza, L., Ambrosi, G., Arruda, L., Attig, N., Barao, F., et al. (2020). Properties of Neon, Magnesium, and Silicon Primary Cosmic Rays Results from the Alpha Magnetic Spectrometer. PHYSICAL REVIEW LETTERS, 124(21) [10.1103/PhysRevLett.124.211102].

Properties of Neon, Magnesium, and Silicon Primary Cosmic Rays Results from the Alpha Magnetic Spectrometer

Gervasi, M.;Grandi, D.;La Vacca, G.;Pensotti, S.;Rozza, D.;Tacconi, M.;Zannoni, M.;
2020

Abstract

We report the observation of new properties of primary cosmic rays, neon (Ne), magnesium (Mg), and silicon (Si), measured in the rigidity range 2.15 GV to 3.0 TV with 1.8 × 10^6 Ne, 2.2 × 10^6 Mg, and 1.6 × 10^6 Si nuclei collected by the Alpha Magnetic Spectrometer experiment on the International Space Station. The Ne and Mg spectra have identical rigidity dependence above 3.65 GV. The three spectra have identical rigidity dependence above 86.5 GV, deviate from a single power law above 200 GV, and harden in an identical way. Unexpectedly, above 86.5 GV the rigidity dependence of primary cosmic rays Ne, Mg, and Si spectra is different from the rigidity dependence of primary cosmic rays He, C, and O. This shows that the Ne, Mg, and Si and He, C, and O are two different classes of primary cosmic rays.
Articolo in rivista - Articolo scientifico
Cosmic Ray Acceleration, Cosmic Ray Composition & Spectra, Cosmic RayPropagation, Cosmic Ray Spectra
English
M. Aguilar et al. (AMS Collaboration)
Aguilar, M., Ali Cavasonza, L., Ambrosi, G., Arruda, L., Attig, N., Barao, F., et al. (2020). Properties of Neon, Magnesium, and Silicon Primary Cosmic Rays Results from the Alpha Magnetic Spectrometer. PHYSICAL REVIEW LETTERS, 124(21) [10.1103/PhysRevLett.124.211102].
Aguilar, M; Ali Cavasonza, L; Ambrosi, G; Arruda, L; Attig, N; Barao, F; Barrin, L; Bartoloni, A; Başeğmez-du Pree, S; Battiston, R; Becker, U; Behlmann, M; Beischer, B; Berdugo, J; Bertucci, B; Bindi, V; de Boer, W; Bollweg, K; Borgia, B; Boschini, M; Bourquin, M; Bueno, E; Burger, J; Burger, W; Burmeister, S; Cai, X; Capell, M; Casaus, J; Castellini, G; Cervelli, F; Chang, Y; Chen, G; Chen, H; Chen, Y; Cheng, L; Chou, H; Chouridou, S; Choutko, V; Chung, C; Clark, C; Coignet, G; Consolandi, C; Contin, A; Corti, C; Cui, Z; Dadzie, K; Dai, Y; Delgado, C; Della Torre, S; Demirköz, M; Derome, L; Di Falco, S; Di Felice, V; Díaz, C; Dimiccoli, F; von Doetinchem, P; Dong, F; Donnini, F; Duranti, M; Egorov, A; Eline, A; Feng, J; Fiandrini, E; Fisher, P; Formato, V; Freeman, C; Galaktionov, Y; Gámez, C; García-López, R; Gargiulo, C; Gast, H; Gebauer, I; Gervasi, M; Giovacchini, F; Gómez-Coral, D; Gong, J; Goy, C; Grabski, V; Grandi, D; Graziani, M; Guo, K; Haino, S; Han, K; Hashmani, R; He, Z; Heber, B; Hsieh, T; Hu, J; Huang, Z; Incagli, M; Jang, W; Jia, Y; Jinchi, H; Kanishev, K; Khiali, B; Kim, G; Kirn, T; Konyushikhin, M; Kounina, O; Kounine, A; Koutsenko, V; Kuhlman, A; Kulemzin, A; La Vacca, G; Laudi, E; Laurenti, G; Lazzizzera, I; Lebedev, A; Lee, H; Lee, S; Li, J; Li, M; Li, Q; Li, S; Li, T; Li, Z; Light, C; Lin, C; Lippert, T; Liu, Z; Lu, S; Lu, Y; Luebelsmeyer, K; Luo, J; Lyu, S; Machate, F; Mañá, C; Marín, J; Marquardt, J; Martin, T; Martínez, G; Masi, N; Maurin, D; Menchaca-Rocha, A; Meng, Q; Mo, D; Molero, M; Mott, P; Mussolin, L; Ni, J; Nikonov, N; Nozzoli, F; Oliva, A; Orcinha, M; Palermo, M; Palmonari, F; Paniccia, M; Pashnin, A; Pauluzzi, M; Pensotti, S; Phan, H; Piandani, R; Plyaskin, V; Poluianov, S; Qi, X; Qin, X; Qu, Z; Quadrani, L; Rancoita, P; Rapin, D; Reina Conde, A; Rosier-Lees, S; Rozhkov, A; Rozza, D; Sagdeev, R; Schael, S; Schmidt, S; Schulz von Dratzig, A; Schwering, G; Seo, E; Shan, B; Shi, J; Siedenburg, T; Solano, C; Sonnabend, R; Song, J; Sun, Q; Sun, Z; Tacconi, M; Tang, X; Tang, Z; Tian, J; Ting, S; Ting, S; Tomassetti, N; Torsti, J; Tüysüz, C; Urban, T; Usoskin, I; Vagelli, V; Vainio, R; Valente, E; Valtonen, E; Vázquez Acosta, M; Vecchi, M; Velasco, M; Vialle, J; Wallmann, C; Wang, L; Wang, N; Wang, Q; Wang, S; Wang, X; Wang, Z; Wei, J; Weng, Z; Wu, H; Xiong, R; Xu, W; Yan, Q; Yang, Y; Yi, H; Yu, Y; Yu, Z; Zannoni, M; Zhang, C; Zhang, F; Zhang, F; Zhang, J; Zhang, Z; Zhao, F; Zheng, Z; Zhuang, H; Zhukov, V; Zichichi, A; Zimmermann, N; Zuccon, P
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/276237
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