Observations of Forbush Decreases of cosmic ray electrons and positrons with the Dark Matter Particle Explorer
Creators: name: Alemanno, Francesca
name: An, Qi
name: Azzarello, Philipp
name: Barbato, Felicia Carla Tiziana
name: Bernardini, Paolo
name: Bi, XiaoJun
name: Cai, MingSheng
name: Casilli, Elisabetta
name: Catanzani, Enrico
name: Chang, Jin
name: Chen, DengYi
name: Chen, JunLing
name: Chen, ZhanFang
name: Cui, MingYang
name: Cui, TianShu
name: Cui, YuXing
name: Dai, HaoTing
name: De Benedittis, Antonio
name: De Mitri, Ivan
name: de Palma, Francesco
name: Deliyergiyev, Maksym
name: Di Santo, Margherita
name: Ding, Qi
name: Dong, TieKuang
name: Dong, ZhenXing
name: Donvito, Giacinto
name: Droz, David
name: Duan, JingLai
name: Duan, KaiKai
name: D'Urso, Domenico
name: Fan, RuiRui
name: Fan, YiZhong
name: Fang, Fang
name: Fang, Kun
name: Feng, ChangQing
name: Feng, Lei
name: Fusco, Piergiorgio
name: Gao, Min
name: Gargano, Fabio
name: Gong, Ke
name: Gong, YiZhong
name: Guo, DongYa
name: Guo, JianHua
name: Han, ShuangXue
name: Hu, YiMing
name: Huang, GuangShun
name: Huang, XiaoYuan
name: Huang, YongYi
name: Ionica, Maria
name: Jiang, Wei
name: Kong, Jie
name: Kotenko, Andrii
name: Kyratzis, Dimitrios
name: Li, .
name: Lei, ShiJun
name: Li, WenHao
name: Li, WeiLiang
name: Li, Xiang
name: Li, XianQiang
name: Liang, YaoMing
name: Liu, ChengMing
name: Liu, Hao
name: Liu, Jie
name: Liu, ShuBin
name: Liu, Yang
name: Loparco, Francesco
name: Luo, ChuanNing
name: Ma, Miao
name: Ma, PengXiong
name: Ma, Tao
name: Ma, XiaoYong
name: Marsella, Giovanni
name: Mazziotta, Mario Nicola
name: Mo, Dan
name: Niu, XiaoYang
name: Pan, Xu
name: Parenti, Andrea
name: Peng, WenXi
name: Peng, XiaoYan
name: Perrina, Chiara
name: Qiao, Rui
name: Rao, JiaNing
name: Ruina, Arshia
name: Salinas, MariaMunoz
name: Shangguan, Zhi
name: Shen, WeiHua
name: Shen, ZhaoQiang
name: Shen, ZhongTao
name: Silveri, Leandro
name: Song, JingXing
name: Stolpovskiy, Mikhail
name: Su, Hong
name: Su, Meng
name: Sun, HaoRan
name: Sun, ZhiYu
name: Surdo, Antonio
name: Teng, XueJian
name: Tykhonov, Andrii
name: Wang, JinZhou
name: Wang, LianGuo
name: Wang, Shen
name: Wang, ShuXin
name: Wang, XiaoLian
name: Wang, Ying
name: Wang, YanFang
name: Wang, YuanZhu
name: Wei, DaMing
name: Wei, JiaJu
name: Wei, YiFeng
name: Wu, Di
name: Wu, Jian
name: Wu, LiBo
name: Wu, Sha Sha
name: Wu, Xin
name: Xia, ZiQing
name: Xu, EnHeng
name: Xu, HaiTao
name: Xu, ZhiHui
name: Xu, ZunLei
name: Xue, GuoFeng
name: Xu, ZiZong
name: Yang, HaiBo
name: Yang, Peng
name: Yang, YaQing
name: Yao, Hui Jun
name: Yu, YuHong
name: Yuan, GuanWen
name: Yuan, Qiang
name: Yue, Chuan
name: Zang, JingJing
name: Zhang, ShengXia
name: Zhang, WenZhang
name: Zhang, Yan
name: Zhang, Yi
name: Zhang, YongJie
name: Zhang, YunLong
name: Zhang, YaPeng
name: Zhang, YongQiang
name: Zhang, ZhiYong
name: Zhang, Zhe
name: Zhao, Cong
name: Zhao, HongYun
name: Zhao, XunFeng
name: Zhou, ChangYi
name: Zhu, Yan
name: Chen, Wei
name: Feng, Li
name: Luo, Xi
name: Zhu, ChengRui
Publisher: name: arXiv
Year: 2021
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The Forbush Decrease (FD) represents the rapid decrease of the intensities of charged particles accompanied with the coronal mass ejections (CMEs) or high-speed streams from coronal holes. It has been mainly explored with ground-based neutron monitors network which indirectly measure the integrated intensities of all species of cosmic rays by counting secondary neutrons produced from interaction between atmosphere atoms and cosmic rays. The space-based experiments can resolve the species of particles but the energy ranges are limited by the relative 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 ($&lt;5$ GeV) with limited statistics. In this paper, we study the FD event occurred in September, 2017, 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 hours are given. We observe two solar energetic particle events in the time profile of the intensity of cosmic rays, the earlier and weak 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.
description: This article is dedicated to the 72nd anniversary of People's Republic of China