| Literature DB >> 26636836 |
M Aguilar1, D Aisa2,3, B Alpat2, A Alvino2, G Ambrosi2, K Andeen4, L Arruda5, N Attig6, P Azzarello7, A Bachlechner8, F Barao5, A Barrau9, L Barrin10, A Bartoloni11, L Basara12, M Battarbee13, R Battiston12,14, J Bazo2, U Becker15, M Behlmann15, B Beischer8, J Berdugo1, B Bertucci2,3, V Bindi16, S Bizzaglia2, M Bizzarri2,3, G Boella17,18, W de Boer4, K Bollweg19, V Bonnivard9, B Borgia11,20, S Borsini2, M J Boschini17, M Bourquin7, J Burger15, F Cadoux7, X D Cai15, M Capell15, S Caroff21, J Casaus1, G Castellini22, I Cernuda1, D Cerreta2,3, F Cervelli23, M J Chae24, Y H Chang25, A I Chen15, G M Chen26, H Chen15, H S Chen26, L Cheng27, H Y Chou25, E Choumilov15, V Choutko15, C H Chung8, C Clark19, R Clavero28, G Coignet21, C Consolandi16, A Contin29,30, C Corti16, E Cortina Gil7, B Coste10,12, W Creus25, M Crispoltoni2,3, Z Cui27, Y M Dai31, C Delgado1, S Della Torre17, M B Demirköz32, L Derome9, S Di Falco23, L Di Masso2,3, F Dimiccoli12,14, C Díaz1, P von Doetinchem16, F Donnini2,3, M Duranti2,3, D D'Urso2, A Egorov15, A Eline15, F J Eppling15, T Eronen13, Y Y Fan33, L Farnesini2, J Feng21,33, E Fiandrini2,3, A Fiasson21, E Finch34, P Fisher15, V Formato10,2, Y Galaktionov15, G Gallucci23, B García1, R García-López28, C Gargiulo10, H Gast8, I Gebauer4, M Gervasi17,18, A Ghelfi9, F Giovacchini1, P Goglov15, J Gong35, C Goy21, V Grabski36, D Grandi17, M Graziani2,3, C Guandalini29, I Guerri23,37, K H Guo38, D Haas7, M Habiby7, S Haino33, K C Han39, Z H He38, M Heil15, J Hoffman25,16, T H Hsieh15, Z C Huang38, C Huh40, M Incagli23, M Ionica2, W Y Jang40, H Jinchi39, K Kanishev10,12,14, G N Kim40, K S Kim40, Th Kirn8, M A Korkmaz32, R Kossakowski21, O Kounina15, A Kounine15, V Koutsenko15, M S Krafczyk15, G La Vacca17, E Laudi2,3, G Laurenti29, I Lazzizzera12,14, A Lebedev15, H T Lee41, S C Lee33, C Leluc7, H L Li33, J Q Li35, J Q Li35, Q Li15, Q Li15, T X Li38, W Li42, Y Li7, Z H Li26, Z Y Li33, S Lim40, C H Lin33, P Lipari11, T Lippert6, D Liu33, H Liu35, Hu Liu1, M Lolli29, T Lomtadze23, M J Lu12, S Q Lu33, Y S Lu26, K Luebelsmeyer8, F Luo27, J Z Luo35, S S Lv38, R Majka34, C Mañá1, J Marín1, T Martin19, G Martínez1, N Masi29, D Maurin9, A Menchaca-Rocha36, Q Meng35, D C Mo38, L Morescalchi23, P Mott19, M Müller8, T Nelson16, J Q Ni38, N Nikonov4, F Nozzoli2, P Nunes5, A Obermeier8, A Oliva1, M Orcinha5, F Palmonari29,30, C Palomares1, M Paniccia7, A Papi2, M Pauluzzi2,3, E Pedreschi23, S Pensotti17,18, R Pereira16, N Picot-Clemente43, F Pilo23, A Piluso2,3, C Pizzolotto2, V Plyaskin15, M Pohl7, V Poireau21, A Putze21, L Quadrani29,30, X M Qi38, X Qin2, Z Y Qu33, T Räihä8, P G Rancoita17, D Rapin7, J S Ricol9, I Rodríguez1, S Rosier-Lees21, A Rozhkov15, D Rozza17, R Sagdeev44, J Sandweiss34, P Saouter7, S Schael8, S M Schmidt6, A Schulz von Dratzig8, G Schwering8, G Scolieri2, E S Seo43, B S Shan42, Y H Shan42, J Y Shi35, X Y Shi15, Y M Shi45, T Siedenburg8, D Son40, J W Song27, F Spada11, F Spinella23, W Sun15, W H Sun15, M Tacconi10,17, C P Tang38, X W Tang26, Z C Tang26, L Tao21, D Tescaro28, Samuel C C Ting15, S M Ting15, N Tomassetti9, J Torsti13, C Türkoğlu32, T Urban19, V Vagelli4,2, E Valente11,20, C Vannini23, E Valtonen13, S Vaurynovich15, M Vecchi46, M Velasco1, J P Vialle21, V Vitale2, S Vitillo7, L Q Wang27, N H Wang27, Q L Wang31, R S Wang45, X Wang15, Z X Wang38, Z L Weng15, K Whitman16, J Wienkenhöver8, M Willenbrock15, H Wu35, X Wu7, X Xia1, M Xie15, S Xie45, R Q Xiong35, N S Xu38, W Xu15, Q Yan15, J Yang24, M Yang26, Y Yang47, Q H Ye45, H Yi35, Y J Yu31, Z Q Yu26, S Zeissler4, C Zhang26, J H Zhang35, M T Zhang38, S D Zhang15, S W Zhang26, X B Zhang38, Z Zhang38, Z M Zheng42, H L Zhuang26, V Zhukov8, A Zichichi29,30, N Zimmermann8, P Zuccon15.
Abstract
Knowledge of the precise rigidity dependence of the helium flux is important in understanding the origin, acceleration, and propagation of cosmic rays. A precise measurement of the helium flux in primary cosmic rays with rigidity (momentum/charge) from 1.9 GV to 3 TV based on 50 million events is presented and compared to the proton flux. The detailed variation with rigidity of the helium flux spectral index is presented for the first time. The spectral index progressively hardens at rigidities larger than 100 GV. The rigidity dependence of the helium flux spectral index is similar to that of the proton spectral index though the magnitudes are different. Remarkably, the spectral index of the proton to helium flux ratio increases with rigidity up to 45 GV and then becomes constant; the flux ratio above 45 GV is well described by a single power law.Entities:
Year: 2015 PMID： 26636836 DOI： 10.1103/PhysRevLett.115.211101
Source DB: PubMed Journal: Phys Rev Lett ISSN： 0031-9007 Impact factor: 9.161