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Ali Cavasonza, L; Arruda, L; Aupetit, S; Bachlechner, A; Barrau, A; Bartoloni, A; Başeğmez-du Pree, S; Battiston, R; Bertucci, B; Cai, X D; Castellini, G; Cervelli, F; Chen, H S; Chen, Y; Cheng, L; Chou, H Y; Choutko, V; Clavero, R; Consolandi, C; Corti, C; Cui, Z; Datta, A; Delgado, C; Derome, L; Díaz, C; von Doetinchem, P; Dong, F; Egorov, A; Eline, A; Eronen, T; Fiandrini, E; Gallucci, G; Gast, H; Gebauer, I; Gervasi, M; Ghelfi, A; Gómez-Coral, D M; Gong, J; Goy, C; Haino, S; He, Z H; Heil, M; Khiali, B; Kounina, O; Kounine, A; Lebedev, A; Li, H S; Li, Z Y; Liu, Hu; Liu, Z; Luebelsmeyer, K; Luo, F; Luo, J Z; Marín, J; Martin, T; Masi, N; Menchaca-Rocha, A; Meng, Q; Mott, P; Ni, J Q; Nikonov, N; Palmonari, F; Phan, H D; Pohl, M; Qi, X M; Qin, X; Rancoita, P G; Rapin, D; Ricol, J S; Rosier-Lees, S; Rozza, D; Schael, S; Shi, J Y; Siedenburg, T; Tacconi, M; Tang, Z C; Tescaro, D; Ting, S M; Torsti, J; Urban, T; Vagelli, V; Valente, E; Vecchi, M; Vialle, J P; Wang, N H; Wang, Q L; Wang, X Q; Wei, C C; Wei, J; Whitman, K; Xiong, R Q; Xu, W; Yang, Y; Yu, Y J; Zhang, J; Zhang, S W; Zheng, Z M; Zhuang, H L; Zhukov, V; Zichichi, A
Physical review letters, 2018-Aug-03, Letnik: 121, Številka: 5Journal Article
A precision measurement of the nitrogen flux with rigidity (momentum per unit charge) from 2.2 GV to 3.3 TV based on 2.2×10^{6} events is presented. The detailed rigidity dependence of the nitrogen flux spectral index is presented for the first time. The spectral index rapidly hardens at high rigidities and becomes identical to the spectral indices of primary He, C, and O cosmic rays above ∼700 GV. We observed that the nitrogen flux Φ_{N} can be presented as the sum of its primary component Φ_{N}^{P} and secondary component Φ_{N}^{S}, Φ_{N}=Φ_{N}^{P}+Φ_{N}^{S}, and we found Φ_{N} is well described by the weighted sum of the oxygen flux Φ_{O} (primary cosmic rays) and the boron flux Φ_{B} (secondary cosmic rays), with Φ_{N}^{P}=(0.090±0.002)×Φ_{O} and Φ_{N}^{S}=(0.62±0.02)×Φ_{B} over the entire rigidity range. This corresponds to a change of the contribution of the secondary cosmic ray component in the nitrogen flux from 70% at a few GV to <30% above 1 TV.
