Properties of Heavy Secondary Fluorine Cosmic Rays: Results from the Alpha Magnetic Spectrometer.

M Aguilar,T Urban,Z Liu,J Berdugo,Xi Luo,M Valencia-Otero,B Heber,L Wang,L Derome,B Khiali,A Kounine,D Rapin,V Formato,D Grandi,C Delgado,A Kulemzin,A Schulz Von Dratzig,W Xu,V Plyaskin,D Maurin,I Lazzizzera,D Rozza,F Donnini,M Molero,M Tacconi,B Alpat,Z Shakfa,L Barrin,J Marín,A Rozhkov,J Gong,F Dimiccoli,S Wang,C Solano,C Consolandi,R Piandani,G Laurenti,J Marquardt,L Mussolin,O Kounina,R Battiston,P Von Doetinchem,T Su,E Fiandrini,Q Li,J Casaus,P Zuccon,K Bollweg,R Sonnabend,C Mañá,C Zheng,B Borgia,C Gargiulo,F Giovacchini,S Haino,E Valente,E Robyn,A Lebedev,S Pensotti,X Wang,A Zichichi,X Qin,S Della Torre,F Machate,A Pashnin,S Di Falco,L Ali Cavasonza,Yu Wang,M Li,K Kanishev,T Siedenburg,M Palermo,Y Chen,C Goy,N Nikonov,Z Cui,L Quadrani,Y Yang,F Nozzoli,K Dadzie,A Egorov,S Schael,Z Zhang,H Jinchi,G La Vacca,G Schwering,G Castellini,V Grabski,S Li,V Koutsenko,Yi Jia,F Cervelli,S Chouridou,M Bourquin,F Zhang,C Díaz,J Torsti,P Mott,M Pauluzzi,M Konyushikhin,A Oliva,G Ambrosi,V Vagelli,V Choutko,M Duranti,V Bindi,C Zhang,C Corti,F Palmonari,M Vecchi,M Incagli,K Luebelsmeyer,B Bertucci,M Behlmann,C Freeman,M Zannoni,E Laudi,A Contin,N Masi,B Beranek,M Gervasi,M Orcinha,G Coignet,M Paniccia,M Capell,V Di Felice,C Gámez,A Eline,L Arruda,M Graziani,N Attig,H Gast,H Y Chou ,F Z Zhang ,Rami Vainio ,Qiang Sun ,Qi Yan ,P G Rancoita ,Z M Zheng ,Jiayu Hu ,J P Vialle ,Z Y Qu ,Nicola Tomassetti ,Seth Pree ,Th Lippert ,Thierry Martin ,Jiwei Song ,Xiaojian Song ,Stepan Poluianov ,R K Hashmani ,Chao-Hung Lin ,Jie Tian ,A Conde ,Yangyi Yu ,F Barão ,G N Kim ,Fengyi Zhao ,C X Wang ,Matthew S Allen ,A Menchaca‐Rocha ,J D Burger ,B Demirköz ,S Q Lu ,В В Михайлов ,D M Gómez-Coral ,Z H Li ,K Han ,Andrew Kuhlman ,J H Feng ,W Y Jang ,Lidia Strigari ,J Q Li ,Lin Cheng ,W J Burger ,H L Zhuang ,C H Douglas Clark ,Xudong Cai ,S C Lee ,Sönke Burmeister ,Zhao-Huan Yu ,H S Chen ,Yao Lu ,Y H Chang ,R Z Sagdeev ,R Q Xiong ,Dong-Chuan Mo ,Q L Wang ,Christopher Light ,R J García-López ,C H Chung ,Yu Galaktionov ,Zhicheng Tang ,Z H He ,Э Валтонен ,J D Negrete ,H D Phan ,J H Li ,Shaoyu Lyu ,E S Seo ,I I Yashin ,Z M Wang ,G Martìnez ,E F Bueno ,Cenk Tüysüz ,Z T Sun ,Mónica Vázquez Acosta ,Timothy H Hsieh ,X Tang ,Jiahui Wei ,Junzhou Luo ,P H Fisher ,Juncheng Liang ,Samuel C.c Ting ,M Boschini ,N H Wang ,S Rosier‐Lees ,G M Chen ,Mayda Velasco ,Z Weng ,S M Ting ,H R Wu ,J H Liu ,B S Shan ,В Жуков ,Qiao Meng ,Ilya Usoskin ,G R Chen ,Fang Dong ,T Kirn ,Yi Han ,J H Zhang ,H T Lee ,Alessandro Bartoloni ,L Q Wang

doi:10.1103/physrevlett.126.081102

Abstract

Precise knowledge of the charge and rigidity dependence of the secondary cosmic ray fluxes and the secondary-to-primary flux ratios is essential in the understanding of cosmic ray propagation. We report the properties of heavy secondary cosmic ray fluorine F in the rigidity R range 2.15GV to 2.9 TV based on 0.29million events collected by the Alpha Magnetic Spectrometer experiment on the International Space Station. The fluorine spectrum deviates from a single power law above 200GV. The heavier secondary-to-primary F/Si flux ratio rigidity dependence is distinctly different from the lighter B/O (or B/C) rigidity dependence. In particular, above 10GV, the F/Si/B/O ratio can be described by a power law R^{δ} with δ=0.052±0.007. This shows that the propagation properties of heavy cosmic rays, from F to Si, are different from those of light cosmic rays, from He to O, and that the secondary cosmic rays have two classes.

Highlights

12IPST, University of Maryland, College Park, Maryland 20742, USA 13CHEP, Kyungpook National University, 41566 Daegu, Korea 14CNR-IROE, 50125 Firenze, Italy
the secondary-to-primary flux ratios is essential in the understanding of cosmic ray propagation
We report the properties of heavy secondary cosmic ray fluorine F in the rigidity R range

Summary

Published by the American Physical Society

AMS has shown that all light secondary-to-primary ratios, Li/C, Li/O, Be/C, Be/O, B/C, and B/O, deviate from a single power law (harden) above 200 GV [10,11] This strongly favors that the hardening of all light cosmic rays is due to propagation effects [2,9,12]. In this Letter, we report the precise measurement of the F flux in the rigidity range from 2.15 GV to 2.9 TV based on 0.29 million fluorine nuclei collected by AMS during the first 8.5 years (May 19, 2011 to October 30, 2019) of operation aboard the International Space Station (ISS). These templates contain only noninteracting events by requiring that L1 and L3–L8 measure the same charge value This background varies from 4% to 15% depending on rigidity. Data analysis.—The isotropic flux Φi in the ith rigidity bin ðRi; Ri þ ΔRiÞ is given by

Ni AiεiTiΔRi

Spectral Index γ