Observations of Forbush Decreases of Cosmic-Ray Electrons and Positrons with the Dark Matter Particle Explorer
Articolo
Data di Pubblicazione:
2021
Citazione:
Observations of Forbush Decreases of Cosmic-Ray Electrons and Positrons with the Dark Matter Particle Explorer / Alemanno, F; An, Q; Azzarello, P; Barbato, Fct; Bernardini, Pl; Bi, Xj; Cai, Ms; Casilli, E; Catanzani, Ero; Chang, J; Chen, Dy; Chen, Jl; Chen, Zf; Cui, My; Cui, Ts; Cui, Yx; Dai, Ht; De Benedittis, A; De Mitri, I; de Palma, F; Deliyergiyev, M; Di Santo, M; Ding, Q; Dong, Tk; Dong, Zx; Donvito, G; Droz, D; Duan, Jl; Duan, Kk; D'Urso, D; Fan, Rr; Fan, Yz; Fang, F; Fang, K; Feng, Cq; Feng, L; Fusco, P; Gao, M; Gargano, F; Gong, K; Gong, Yz; Guo, Dy; Guo, Jh; Han, Sx; Hu, Ym; Huang, Gs; Huang, Xy; Huang, Yy; Ionica, M; Jiang, W; Kong, J; Kotenko, A; Kyratzis, D; Li, S; Lei, Sj; Li, Wh; Li, Wl; Li, X; Li, Xq; Liang, Ym; Liu, Cm; Liu, H; Liu, J; Liu, Sb; Liu, Y; Loparco, F; Luo, Cn; Ma, M; Ma, Px; Ma, T; Ma, Xy; Marsella, G; Mazziotta, Mn; Mo, D; Niu, Xy; Pan, X; Parenti, A; Peng, Wx; Peng, Xy; Perrina, C; Qiao, R; Rao, Jn; Ruina, A; Salinas, M; Zhi, Sg; Shen, Wh; Shen, Zq; Shen, Zt; Silveri, L; Song, Jx; Stolpovskiy, M; Su, H; Su, M; Sun, Hr; Sun, Zy; Surdo, A; Teng, Xj; Tykhonov, A; Wang, Jz; Wang, Lg; Wang, S; Wang, Sx; Wang, Xl; Wang, Y; Wang, Yf; Wang, Yz; Wei, Dm; Wei, Jj; Wei, Yf; Wu, D; Wu, J; Wu, Lb; Wu, Ss; Wu, X; Xia, Zq; Xu, Eh; Xu, Ht; Xu, Zh; Xu, Zl; Xue, Gf; Xu, Zz; Yang, Hb; Yang, P; Yang, Yq; Yao, Hj; Yu, Yh; Yuan, Gw; Yuan, Q; Yue, C; Zang, Jj; Zhang, Sx; Zhang, Wz; Zhang, Y; Zhang, Y; Zhang, Yj; Zhang, Yl; Zhang, Yp; Zhang, Yq; Zhang, Zy; Zhang, Z; Zhao, C; Zhao, Hy; Zhao, Xf; Zhou, Cy; Zhu, Y; Chen, W; Feng, L; Luo, X; Zhu, Cr. - In: THE ASTROPHYSICAL JOURNAL LETTERS. - ISSN 2041-8205. - 920:2(2021), p. L43. [10.3847/2041-8213/ac2de6]
Abstract:
The Forbush decrease (FD) represents the rapid decrease of the intensities of charged particles accompanied with the coronal mass ejections or high-speed streams from coronal holes. It has been mainly explored with the ground-based neutron monitor network, which indirectly measures the integrated intensities of all species of cosmic rays by counting secondary neutrons produced from interaction between atmospheric atoms and cosmic rays. The space-based experiments can resolve the species of particles but the energy ranges are limited by the relatively small acceptances except for the most abundant particles like protons and helium. Therefore, the FD of cosmic-ray electrons and positrons have just been investigated by the PAMELA experiment in the low-energy range (<5 GeV) with limited statistics. In this paper, we study the FD event that occurred in 2017 September with the electron and positron data recorded by the Dark Matter Particle Explorer. The evolution of the FDs from 2 GeV to 20 GeV with a time resolution of 6 hr are given. We observe two solar energetic particle events in the time profile of the intensity of cosmic rays, the earlier, and weaker, one has not been shown in the neutron monitor data. Furthermore, both the amplitude and recovery time of fluxes of electrons and positrons show clear energy dependence, which is important in probing the disturbances of the interplanetary environment by the coronal mass ejections.
Tipologia CRIS:
1.1 Articolo in rivista
Elenco autori:
Alemanno, F; An, Q; Azzarello, P; Barbato, Fct; Bernardini, Pl; Bi, Xj; Cai, Ms; Casilli, E; Catanzani, Ero; Chang, J; Chen, Dy; Chen, Jl; Chen, Zf; Cui, My; Cui, Ts; Cui, Yx; Dai, Ht; De Benedittis, A; De Mitri, I; de Palma, F; Deliyergiyev, M; Di Santo, M; Ding, Q; Dong, Tk; Dong, Zx; Donvito, G; Droz, D; Duan, Jl; Duan, Kk; D'Urso, D; Fan, Rr; Fan, Yz; Fang, F; Fang, K; Feng, Cq; Feng, L; Fusco, P; Gao, M; Gargano, F; Gong, K; Gong, Yz; Guo, Dy; Guo, Jh; Han, Sx; Hu, Ym; Huang, Gs; Huang, Xy; Huang, Yy; Ionica, M; Jiang, W; Kong, J; Kotenko, A; Kyratzis, D; Li, S; Lei, Sj; Li, Wh; Li, Wl; Li, X; Li, Xq; Liang, Ym; Liu, Cm; Liu, H; Liu, J; Liu, Sb; Liu, Y; Loparco, F; Luo, Cn; Ma, M; Ma, Px; Ma, T; Ma, Xy; Marsella, G; Mazziotta, Mn; Mo, D; Niu, Xy; Pan, X; Parenti, A; Peng, Wx; Peng, Xy; Perrina, C; Qiao, R; Rao, Jn; Ruina, A; Salinas, M; Zhi, Sg; Shen, Wh; Shen, Zq; Shen, Zt; Silveri, L; Song, Jx; Stolpovskiy, M; Su, H; Su, M; Sun, Hr; Sun, Zy; Surdo, A; Teng, Xj; Tykhonov, A; Wang, Jz; Wang, Lg; Wang, S; Wang, Sx; Wang, Xl; Wang, Y; Wang, Yf; Wang, Yz; Wei, Dm; Wei, Jj; Wei, Yf; Wu, D; Wu, J; Wu, Lb; Wu, Ss; Wu, X; Xia, Zq; Xu, Eh; Xu, Ht; Xu, Zh; Xu, Zl; Xue, Gf; Xu, Zz; Yang, Hb; Yang, P; Yang, Yq; Yao, Hj; Yu, Yh; Yuan, Gw; Yuan, Q; Yue, C; Zang, Jj; Zhang, Sx; Zhang, Wz; Zhang, Y; Zhang, Y; Zhang, Yj; Zhang, Yl; Zhang, Yp; Zhang, Yq; Zhang, Zy; Zhang, Z; Zhao, C; Zhao, Hy; Zhao, Xf; Zhou, Cy; Zhu, Y; Chen, W; Feng, L; Luo, X; Zhu, Cr
Link alla scheda completa:
Pubblicato in: