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    Diverse Properties of Electron Forbush Decreases Revealed by the Dark Matter Particle Explorer

    F. Alemanno1,2, Q. An3,4, P. Azzarello5, F. C. T. Barbato6,7, P. Bernardini1,2, X. J. Bi8,9, H. Boutin5, I. Cagnoli6,7, M. S. Cai10,11 et al. (DAMPE Collaboration††)

    X. Luo18

    M. S. Cai10,11, E. Casilli6,7, J. Chang10,11, D. Y. Chen10, J. L. Chen12, Z. F. Chen12, Z. X. Chen12,8, P. Coppin5, M. Y. Cui10, T. S. Cui13, I. De Mitri6,7, F. de Palma1,2, A. Di Giovanni6,7, T. K. Dong10, Z. X. Dong13, G. Donvito14, J. L. Duan12, K. K. Duan10, R. R. Fan9, Y. Z. Fan10,11, F. Fang12, K. Fang9, C. Q. Feng3,4, L. Feng10, S. Fogliacco6,7, J. M. Frieden5,*, P. Fusco14,15, M. Gao9, F. Gargano14, E. Ghose1,2, K. Gong9, Y. Z. Gong10, D. Y. Guo9, J. H. Guo10,11, S. X. Han13, Y. M. Hu10, G. S. Huang3,4, X. Y. Huang10,11, Y. Y. Huang10, M. Ionica16, L. Y. Jiang10, W. Jiang10, Y. Z. Jiang16,†, J. Kong12, A. Kotenko5, D. Kyratzis6,7, S. J. Lei10, B. Li10,11, W. L. Li13, W. H. Li10, X. Li10,11, X. Q. Li13, Y. M. Liang13, C. M. Liu16, H. Liu10, J. Liu12, S. B. Liu3,4, Y. Liu10, F. Loparco14,15, M. Ma13, P. X. Ma10, T. Ma10, X. Y. Ma13, G. Marsella1,2,‡, M. N. Mazziotta14, D. Mo12, Y. Nie3,4, X. Y. Niu12, A. Parenti6,7,§, W. X. Peng9, X. Y. Peng10, C. Perrina5,*, E. Putti-Garcia5, R. Qiao9, J. N. Rao13, Y. Rong3,4, A. Ruina5, R. Sarkar6,7, P. Savina6,7, Z. Shangguan13, W. H. Shen13, Z. Q. Shen10, Z. T. Shen3,4, L. Silveri6,7,∥, J. X. Song13, M. Stolpovskiy5, H. Su12, M. Su17, H. R. Sun3,4, Z. Y. Sun12, A. Surdo2, X. J. Teng13, A. Tykhonov5, G. F. Wang3,4, J. Z. Wang9, L. G. Wang13, S. Wang10, X. L. Wang3,4, Y. F. Wang3,4, D. M. Wei10,11, J. J. Wei10, Y. F. Wei3,4, D. Wu9, J. Wu10,11, S. S. Wu13, X. Wu5, Z. Q. Xia10, Z. Xiong6,7, E. H. Xu3,4, H. T. Xu13, J. Xu10, Z. H. Xu12, Z. Z. Xu3,4, Z. L. Xu10, G. F. Xue13, M. Y. Yan3,4, H. B. Yang12, P. Yang12, Y. Q. Yang12, H. J. Yao12, Y. H. Yu12, Q. Yuan10,11, C. Yue10, J. J. Zang10,¶, S. X. Zhang12, W. Z. Zhang13, Yan Zhang10, Y. P. Zhang12, Yi Zhang10,11, Y. J. Zhang12, Y. Q. Zhang10, Y. L. Zhang3,4, Z. Zhang10, Z. Y. Zhang3,4, C. Zhao3,4, H. Y. Zhao12, X. F. Zhao13, C. Y. Zhou13, X. Zhu10,**, and Y. Zhu13 (DAMPE Collaboration††)

    • 1Dipartimento di Matematica e Fisica E. De Giorgi, Università del Salento, I-73100, Lecce, Italy
    • 2Istituto Nazionale di Fisica Nucleare (INFN) - Sezione di Lecce, I-73100, Lecce, Italy
    • 3State Key Laboratory of Particle Detection and Electronics, University of Science and Technology of China, Hefei 230026, China
    • 4Department of Modern Physics, University of Science and Technology of China, Hefei 230026, China
    • 5Department of Nuclear and Particle Physics, University of Geneva, Geneva CH-1211, Switzerland
    • 6Gran Sasso Science Institute (GSSI), Via Iacobucci 2, I-67100 L’Aquila, Italy
    • 7Istituto Nazionale di Fisica Nucleare (INFN) - Laboratori Nazionali del Gran Sasso, I-67100 Assergi, L’Aquila, Italy
    • 8University of Chinese Academy of Sciences, Beijing 100049, China
    • 9Particle Astrophysics Division, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
    • 10Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China
    • 11School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China
    • 12Institute of Modern Physics, Chinese Academy of Sciences, Lanzhou 730000, China
    • 13National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
    • 14Istituto Nazionale di Fisica Nucleare, Sezione di Bari, via Orabona 4, I-70126 Bari, Italy
    • 15Dipartimento di Fisica “M. Merlin,” dell’Università e del Politecnico di Bari, via Amendola 173, I-70126 Bari, Italy
    • 16Istituto Nazionale di Fisica Nucleare (INFN) - Sezione di Perugia, I-06123 Perugia, Italy
    • 17Department of Physics and Laboratory for Space Research, University of Hong Kong, Hong Kong SAR 999077, China
    • 18Shandong Institute of Advanced Technology, Jinan 250100, China

    • *Present address: Institute of Physics, Ecole Polytechnique Fédérale de Lausanne (EPFL), CH-1015 Lausanne, Switzerland.
    • †Also at Dipartimento di Fisica e Geologia, Università degli Studi di Perugia, I-06123 Perugia, Italy.
    • ‡Present address: Dipartimento di Fisica e Chimica “E. Segrè,” Università degli Studi di Palermo, I-90128 Palermo, Italy.
    • §Present address: Inter-university Institute for High Energies, Universitè Libre de Bruxelles, B-1050 Brussels, Belgium.
    • ∥Present address: New York University Abu Dhabi, Saadiyat Island, Abu Dhabi 129188, United Arab Emirates.
    • Also at School of Physics and Electronic Engineering, Linyi University, Linyi 276000, China.
    • **Also at School of Computing, Nanjing University of Posts and Telecommunications, Nanjing 210023, China.
    • ††Contact author: dampe@pmo.ac.cn

    Phys. Rev. Lett. 136, 101004 – Published 13 March, 2026

    DOI: https://doi.org/10.1103/6dyq-9v81

    Abstract

    The Forbush decrease of cosmic rays is an important probe of the interplanetary environment disturbed by solar activities. In this Letter, we study the properties of eight Forbush decreases’ electrons (including positrons) between 2 and 20 GeV from January 2016 to March 2024 with the Dark Matter Particle Explorer. The maximum decrease amplitudes of these events are about 30%–15%, and the amplitudes reduce with energy. The recovery time of these events shows diverse behaviors of their energy dependence. Some of them show strong energy dependence, while some have a nearly constant recovery time. It has been shown that such diverse behaviors could be related to the geometry of the regions of the interplanetary space disturbed by coronal mass ejections, which can be characterized by the combined effect of the coronal mass ejection velocity, angular spread, and ejection direction.

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