Bibcode
Aguilar, M.; Ali Cavasonza, L.; Alpat, B.; Ambrosi, G.; Arruda, L.; Attig, N.; Aupetit, S.; Azzarello, P.; Bachlechner, A.; Barao, F.; Barrau, A.; Barrin, L.; Bartoloni, A.; Basara, L.; Başeǧmez-du Pree, S.; Battarbee, M.; Battiston, R.; Becker, U.; Behlmann, M.; Beischer, B.; Berdugo, J.; Bertucci, B.; Bindel, K. F.; Bindi, V.; de Boer, W.; Bollweg, K.; Bonnivard, V.; Borgia, B.; Boschini, M. J.; Bourquin, M.; Bueno, E. F.; Burger, J.; Burger, W. J.; Cai, X. D.; Capell, M.; Caroff, S.; Casaus, J.; Castellini, G.; Cervelli, F.; Chang, Y. H.; Chen, A. I.; Chen, G. M.; Chen, H. S.; Chen, Y.; Cheng, L.; Chou, H. Y.; Choumilov, E.; Choutko, V.; Chung, C. H.; Clark, C.; Clavero, R.; Coignet, G.; Consolandi, C.; Contin, A.; Corti, C.; Creus, W.; Crispoltoni, M.; Cui, Z.; Dadzie, K.; Dai, Y. M.; 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.; Egorov, A.; Eline, A.; Eronen, T.; Feng, J.; Fiandrini, E.; Fisher, P.; Formato, V.; Galaktionov, Y.; Gallucci, G.; García-López, R. J.; Gargiulo, C.; Gast, H.; Gebauer, I.; Gervasi, M.; Ghelfi, A.; 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.; Heil, M.; Hsieh, T. H. et al.
Bibliographical reference
Physical Review Letters, Volume 121, Issue 5, id.051103
Advertised on:
8
2018
Journal
Citations
77
Refereed citations
63
Description
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 ×106
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 ΦN can be presented as
the sum of its primary component ΦNP and
secondary component ΦNS,
ΦN=ΦNP+ΦNS,
and we found ΦN is well described by the weighted sum of
the oxygen flux ΦO (primary cosmic rays) and the boron
flux ΦB (secondary cosmic rays), with
ΦNP=(0.090 ±0.002
)×ΦO and ΦNS=(0.62
±0.02 )×ΦB 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.
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