Spectral hardening of cosmic ray protons and helium nuclei in supernova remnant shocks  

作　　者：Wen-Hui Lin Bi-Wen Bao Ze-Jun Jiang Li Zhang 林文慧;鲍必文;姜泽军;张力(Department of Astronomy, Yunnan University,Key Laboratory of Astroparticle physics of Yunnan Province)

机构地区：[1]Department of Astronomy, Yunnan University,Key Laboratory of Astroparticle physics of Yunnan Province

出　　处：《Chinese Physics C》2019年第5期23-28,共6页中国物理C（英文版）

基　　金：Supported by the National Natural Science Foundation of China(11433004,U1738211,11563009);the Yunnan Applied Basic Research Projects(2015FB103,2016FB001,2018FY001(-003));National Key R&D Program of China(2018YFA0404204)

摘　　要：The observed hardening of the spectra of cosmic ray protons and helium nuclei is studied within the model of nonlinear diffusive shock acceleration of supernova remnants(SNRs). In this model, the injected particles with energies below the spectral "knee" are assumed to be described by two populations with different spectral indexes around 200 GeV. The high-energy population is dominated by the particles with energies above 200 GeV released upstream of the shock of SNR, and the low-energy population is attributed to the particles with energies below 200 GeV released downstream of the shock of SNR. In this scenario, the spectral hardening of cosmic ray protons and helium nuclei observed by PAMELA, AMS-02, and CREAM experiments can be reproduced.The observed hardening of the spectra of cosmic ray protons and helium nuclei is studied within the model of nonlinear diffusive shock acceleration of supernova remnants(SNRs). In this model, the injected particles with energies below the spectral "knee" are assumed to be described by two populations with different spectral indexes around 200 GeV. The high-energy population is dominated by the particles with energies above 200 GeV released upstream of the shock of SNR, and the low-energy population is attributed to the particles with energies below 200 GeV released downstream of the shock of SNR. In this scenario, the spectral hardening of cosmic ray protons and helium nuclei observed by PAMELA, AMS-02, and CREAM experiments can be reproduced.

关 键 词：GALACTIC COSMIC ray SUPERNOVA REMNANTS shock acceleration 

分 类 号：O4[理学—物理]