Observations of Forbush Decreases of Cosmic-Ray Electrons and Positrons with the Dark Matter Particle Explorer

Observations of Forbush Decreases of Cosmic-Ray Electrons and Positrons with the Dark Matter Particle Explorer
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用暗物质粒子探测器观察福布什宇宙射线电子和正电子的减少

DOI：
10.3847/2041-8213/ac2de6
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发表时间：
2021-09
期刊：
Astrophysical Journal Letters
影响因子：
7.9
通讯作者：
De Bene
De Bene
中科院分区：
物理与天体物理2区
文献类型：
--
作者：
Alemanno Francesca;An Qi;Azzarello Philipp;Barbato Felicia Carla Tiziana;Bernardini Paolo;Bi XiaoJun;Cai MingSheng;Casilli Elisabetta;Catanzani Enrico;Chang Jin;Chen DengYi;Chen JunLing;Chen ZhanFang;Cui MingYang;Cui TianShu;Cui YuXing;Dai HaoTing;De Bene

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Forbush下降（FD）是伴随着日冕物质抛射或冕洞高速流的带电粒子强度的快速下降。主要利用地基中子监测网络进行探索，该网络通过对大气原子与宇宙射线相互作用产生的次级中子进行计数，间接测量所有种类宇宙射线的综合强度。天基实验可以分辨粒子的种类，但能量范围受到相对较小的接受度的限制，除了最丰富的粒子，如质子和氦。因此，宇宙线电子和正电子的FD仅在PAMELA实验中在低能范围（<5 GeV）进行了有限的统计研究。本文利用暗物质粒子探测器记录的电子和正电子数据研究了2017年9月发生的FD事件。给出了能量从2GeV到20GeV，时间分辨率为6小时的FD的演化过程。在宇宙线强度的时间剖面上，我们观测到两个太阳高能粒子事件，一个较早，一个较弱，一个在中子监测数据中没有显示出来。此外，电子和正电子通量的幅度和恢复时间都表现出明显的能量依赖性，这对于探测日冕物质抛射对行星际环境的扰动是很重要的。
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.
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