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

TitleObservations of Forbush Decreases of Cosmic-Ray Electrons and Positrons with the Dark Matter Particle Explorer
Authors
Issue Date2021
PublisherAmerican Astronomical Society. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
The Astrophysical Journal Letters, 2021, v. 920 n. 2, p. article no. L43 How to Cite?
AbstractThe 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.
Persistent Identifierhttp://hdl.handle.net/10722/308172
ISSN
2020 Impact Factor: 7.413
2020 SCImago Journal Rankings: 3.639
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorAlemanno, F-
dc.contributor.authorAn, Q-
dc.contributor.authorAzzarello, P-
dc.contributor.authorCarla Tiziana Barbato, F-
dc.contributor.authorBernardini, P-
dc.contributor.authorBi, XJ-
dc.contributor.authorCai, MS-
dc.contributor.authorCasilli, E-
dc.contributor.authorCatanzani, E-
dc.contributor.authorChang, J-
dc.contributor.authorChen, DY-
dc.contributor.authorWang, S-
dc.contributor.authorWang, SX-
dc.contributor.authorWang, XL-
dc.contributor.authorWang, Y-
dc.contributor.authorWang, YF-
dc.contributor.authorWang, YZ-
dc.contributor.authorWei, DM-
dc.contributor.authorWei, JJ-
dc.contributor.authorWei, YF-
dc.contributor.authorWu, D-
dc.contributor.authorChen, JL-
dc.contributor.authorWu, J-
dc.contributor.authorWu, LB-
dc.contributor.authorWu, SS-
dc.contributor.authorWu, X-
dc.contributor.authorXia, ZQ-
dc.contributor.authorXu, EH-
dc.contributor.authorXu, HT-
dc.contributor.authorXu, ZH-
dc.contributor.authorXu, ZL-
dc.contributor.authorXue, GF-
dc.contributor.authorChen, ZF-
dc.contributor.authorXu, ZZ-
dc.contributor.authorYang, HB-
dc.contributor.authorYang, P-
dc.contributor.authorYang, YQ-
dc.contributor.authorJun Yao, H-
dc.contributor.authorYu, YH-
dc.contributor.authorYuan, GW-
dc.contributor.authorYuan, Q-
dc.contributor.authorYue, C-
dc.contributor.authorZang, JJ-
dc.contributor.authorCui, MY-
dc.contributor.authorZhang, SX-
dc.contributor.authorZhang, WZ-
dc.contributor.authorZhang, Y-
dc.contributor.authorZhang, Y-
dc.contributor.authorZhang, YJ-
dc.contributor.authorZhang, YL-
dc.contributor.authorZhang, YP-
dc.contributor.authorZhang, YQ-
dc.contributor.authorZhang, ZY-
dc.contributor.authorZhang, Z-
dc.contributor.authorCui, TS-
dc.contributor.authorZhao, C-
dc.contributor.authorZhao, HY-
dc.contributor.authorZhao, XF-
dc.contributor.authorZhou, CY-
dc.contributor.authorZhu, Y-
dc.contributor.authorChen, W-
dc.contributor.authorFeng, L-
dc.contributor.authorLuo, X-
dc.contributor.authorZhu, CR-
dc.contributor.authorCui, YX-
dc.contributor.authorDai, HT-
dc.contributor.authorDe Benedittis, A-
dc.contributor.authorDe Mitri, I-
dc.contributor.authorde Palma, F-
dc.contributor.authorDeliyergiyev, M-
dc.contributor.authorDi Santo, M-
dc.contributor.authorDing, Q-
dc.contributor.authorDong, TK-
dc.contributor.authorDong, ZX-
dc.contributor.authorDonvito, G-
dc.contributor.authorDroz, D-
dc.contributor.authorDuan, JL-
dc.contributor.authorDuan, KK-
dc.contributor.authorD’Urso, D-
dc.contributor.authorFan, RR-
dc.contributor.authorFan, YZ-
dc.contributor.authorFang, F-
dc.contributor.authorFang, K-
dc.contributor.authorFeng, CQ-
dc.contributor.authorFeng, L-
dc.contributor.authorFusco, P-
dc.contributor.authorGao, M-
dc.contributor.authorGargano, F-
dc.contributor.authorGong, K-
dc.contributor.authorGong, YZ-
dc.contributor.authorGuo, DY-
dc.contributor.authorGuo, JH-
dc.contributor.authorHan, SX-
dc.contributor.authorHu, YM-
dc.contributor.authorHuang, GS-
dc.contributor.authorHuang, XY-
dc.contributor.authorHuang, YY-
dc.contributor.authorIonica, M-
dc.contributor.authorJiang, W-
dc.contributor.authorKong, J-
dc.contributor.authorKotenko, A-
dc.contributor.authorKyratzis, D-
dc.contributor.authorLi, S-
dc.contributor.authorLi, SJ-
dc.contributor.authorLi, WH-
dc.contributor.authorLi, WL-
dc.contributor.authorLi, X-
dc.contributor.authorLi, XQ-
dc.contributor.authorLiang, YM-
dc.contributor.authorLiu, CM-
dc.contributor.authorLiu, H-
dc.contributor.authorLiu, J-
dc.contributor.authorLiu, SB-
dc.contributor.authorLiu, Y-
dc.contributor.authorLoparco, F-
dc.contributor.authorLuo, CN-
dc.contributor.authorMa, M-
dc.contributor.authorMa, PX-
dc.contributor.authorMa, T-
dc.contributor.authorMa, XY-
dc.contributor.authorMarsella, G-
dc.contributor.authorMazziotta, MN-
dc.contributor.authorMo, D-
dc.contributor.authorNiu, XY-
dc.contributor.authorPan, X-
dc.contributor.authorParenti, A-
dc.contributor.authorPeng, WX-
dc.contributor.authorPeng, XY-
dc.contributor.authorPerrina, C-
dc.contributor.authorQiao, R-
dc.contributor.authorRao, JN-
dc.contributor.authorRuina, A-
dc.contributor.authorSalinas, M-
dc.contributor.authorShangguan, Z-
dc.contributor.authorShen, WH-
dc.contributor.authorShen, ZQ-
dc.contributor.authorShen, ZT-
dc.contributor.authorSilveri, L-
dc.contributor.authorSong, JX-
dc.contributor.authorStolpovskiy, M-
dc.contributor.authorSu, H-
dc.contributor.authorSu, M-
dc.contributor.authorSun, HR-
dc.contributor.authorSun, ZY-
dc.contributor.authorSurdo, A-
dc.contributor.authorTeng, XJ-
dc.contributor.authorTykhonov, A-
dc.contributor.authorWang, JZ-
dc.contributor.authorWang, LG-
dc.date.accessioned2021-11-12T13:43:30Z-
dc.date.available2021-11-12T13:43:30Z-
dc.date.issued2021-
dc.identifier.citationThe Astrophysical Journal Letters, 2021, v. 920 n. 2, p. article no. L43-
dc.identifier.issn2041-8205-
dc.identifier.urihttp://hdl.handle.net/10722/308172-
dc.description.abstractThe 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.-
dc.languageeng-
dc.publisherAmerican Astronomical Society. The Journal's web site is located at http://iopscience.iop.org/2041-8205-
dc.relation.ispartofThe Astrophysical Journal Letters-
dc.rightsThis work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.-
dc.titleObservations of Forbush Decreases of Cosmic-Ray Electrons and Positrons with the Dark Matter Particle Explorer-
dc.typeArticle-
dc.identifier.authoritySu, M=rp02150-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.3847/2041-8213/ac2de6-
dc.identifier.scopuseid_2-s2.0-85118162277-
dc.identifier.hkuros330331-
dc.identifier.volume920-
dc.identifier.issue2-
dc.identifier.spagearticle no. L43-
dc.identifier.epagearticle no. L43-
dc.identifier.isiWOS:000709975200001-
dc.publisher.placeUnited Kingdom-

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