Institutional Repository System Of Yunnan Observatories, CAS
| Variations of secondary particle arrival time detected by LHAASO-KM2A during thunderstorms | |
Chen, Xuejian1; Zhou, Xunxiu1; Yang, Ci1; Huang, Daihui1; Cao, Zhen2,3,4; Aharonian, F.5,6; An, Q7,8; Axikegu9; Bai,Y.X.2,4; Bao,Y.W.10; Bastieri,D.11; Bi,X.J.2,3,4; Bi,Y.J.2,4; Cai,J.T.11; Cao, Q.12; Cao, W.Y.8; Cao, Zhe7,8; Chang, J.13; Chang, J.F.2,4,7; Chen, A.M.14; Chen, E.S.2,3,4; Chen, Liang15; Chen, Lin9; Chen, Long9; Chen, M.J.2,4; Chen, M.L.2,4,7; Chen, Q.H.9; Chen, S.H.2,3,4; Chen, S.Z.2,4; Chen, T.L.16; Chen,Y.10; Cheng, N.2,4; cheng, Y.D.2,4; Cui, M.Y.13; Cui, S.W.12; Cui,X.H.17; Cui,Y.D.18,19,20; Dai, B.Z.21; Dai, H.L.2,4,7; Dai, Z.G.8; Danzengluobu16; della volpe, D.22; Dong, X.Q.2,3,4; Duan, K.K.13; Fan, J.H.1; Fan, Y.Z.13; Fang,J.21; Fang, K.2,4; Feng, C.F.23; Feng, L.13; Feng, S.H.2,4; Feng, X.T.23; Feng,Y.L.16; Gabici,s.24; Gao, B.2,4; Gao, C.D.23; Guo, L.Q.2,3,4; Goo,Q.16; Guo, W.2,4; Gao, W.K.2,3,4; Ge, M.M.21; Geng, L.s.2,4; Giacinti, G.14; Gong, G.H.25; Gou, Q.B.2,4; Gu, M.H.2,4,7; Guo, F.L.15; Guo, X.L.9; Guo, Y.Q.2,4; Guo, Y.Y.,13; Han, Y.A.26; He,H.H.2,3,4; He, H.N.13; He,J.Y.13; He, X.B.18,19,20; He, Y.9; Heller, M.22; Hor, Y.K.18,19,20; Hou, B.W.2,3,4; Hou, C.2,4; Hou X(侯贤)27 ; Hu, H.B.2,3,4; Hu,Q.8,13; Hu,S.C.2,3,4; Huang, D.H.9; Huang, T.Q.2,4; Huang, W.J.18,19,20; Huang, X.T.23; Huang,X.13; Huang,Y.2,3,4; Huang,Z.C.9; Ji,X.L.2,4,7; Jia,H.Y.9; Jia,K.23; Jiang,K.7,8; Jiang, X.W.2,4; Jiang, Z.J.21; Jin, M.9; Kang, M.M.28; Ke, T.2,4; Kuleshov, D.29; Kurinov,K.29; Li, B.B.12; Li, Cheng7,8; Li, Cong2,4; Li, D.2,3,4; Li, F.2,4,7; Li, H.B.2,4; Li, H.C.2,4; Li, H.Y.8,13; Li, J.8,13; Li, Jian8; Li,Jie2,4,7; Li, K.2,4; Li, W.L.23; Li, W.L.14; Li, X.R.2,4; Li, Xin7,8; Li, Y.Z.2,3,4; Li, zhe2,4; Li, Zhuo30; Liang, E.W.31; Liang, Y.F.31; Lin, S.J.18,19,20; Liu, B.8; Liu,C.2,4; Liu, D.23; Liu,H.9; Liu, H.D.26; Liu,).2,4; Liu,J.L.2,4; Liu,J.Y.2,4; Liu,M.Y.16; Liu,R.Y.10; Liu,S.M.9; Liu,W.2,4; Liu,Y.1; Liu, Y.N.25; Lu,R.21; Luo,Q.18,19,20; Lv,H.K.2,4; Ma, B.Q.30; Ma,L.L.2,4; Ma,X.H.2,4; Mao JR(毛基荣)27; Min, Z.2,4; Mitthumsiri, W.32; Mu, H.J.26; Nan,Y.C.2,4; Neronov, A.24; Ou, Z.W.18,19,20; Pang, B.Y.9; Pattarakijwanich, P32; Pei, Z.Y.11; Qi, M.Y.2,4; Qi, Y.Q.12; Qiao, B.Q.2,4; Qin, J.J.8; Ruffolo, D.32; Sáiz, A.32; Semikoz,D.24; Shao, C.Y.18,19,20; Shao, L.12; Shchegolev, O.29,33; Sheng, X.D.2,4; Shu, F.W.34; Song, H.C.30; Stenkin, Yu.V.29,33; Stepanov, V.29; Su, Y.13; Sun, Q.N.9; Sun, X.N.31
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| 会议录名称 | Proceedings of Science |
| 2024-09-27 | |
| 卷号 | 444 |
| DOI | 10.22323/1.444.0182 |
| 产权排序 | 第27完成单位 |
| 收录类别 | EI |
| 会议名称 | 38th International Cosmic Ray Conference, ICRC 2023 |
| 会议日期 | 2023-07-26 |
| 会议地点 | Nagoya, Japan |
| 会议赞助商 | et al.; Institute for Cosmic Ray Research (ICRR) Univeristy of Tokyo; International Union of Pure and Applied Physics (IUPAP); JPS; Nagoya Convention and Visitors Bureau; Nagoya University |
| 摘要 | A sub-array of the Large High Altitude Air Shower Observatory (LHAASO), KM2A contains 5216 electromagnetic particle detectors (EDs) and 1188 muon detectors (MDs). For each shower event that meets the trigger conditions (at least 20 fired EDs within a time window of 400 ns) in KM2A array, there are many signals from ED and MD detectors. The information on the arrival time and location of each signal are recorded, and the ED hits are used for shower reconstruction. Due to the acceleration and deflection by the atmospheric electric field (AEF) during a thunderstorm, the arrival time and position of the ground-level particles are modified, resulting in the changes in the inferred shower detection. To understand the shower event variation during thunderstorms, the particle arrival time is studied by analyzing the KM2A data. We can measure the distribution of changes of arrival time in the thunderstorm electric field. The variation amplitude is not only dependent on the AEF, but also highly correlated with the direction of the shower event. With the increase of the AEF strength and the zenith angle, the variation in amplitude of the arrival time becomes larger. Our results are useful in understanding the variation of shower rate detected by LHAASO-KM2A, and will also provide important information for shower reconstruction during thunderstorms. © Copyright owned by the author(s) under the terms of the Creative Commons. |
| 资助项目 | National Natural Science Foundation of China[U2031101];National Key Research and Development Program of China[2018YFA0404201] |
| 项目资助者 | National Natural Science Foundation of China[U2031101] ; National Key Research and Development Program of China[2018YFA0404201] |
| 语种 | 英语 |
| 学科领域 | 天文学 ; 天体物理学 ; 高能天体物理学 ; 星系与宇宙学 |
| 文章类型 | Conference article (CA) |
| URL | 查看原文 |
| EI入藏号 | 20245117556277 |
| EI主题词 | Thunderstorms |
| EI分类号 | 1301.1.3 - 443.1 Atmospheric Properties - 714.1 Electron Tubes - 801 Chemistry - 942.1.12 |
| 引用统计 | |
| 文献类型 | 会议论文 |
| 条目标识符 | http://ir.ynao.ac.cn/handle/114a53/27929 |
| 专题 | 星系类星体研究组 |
| 作者单位 | 1.School of Physical Science and Technology, Southwest Jiaotong University, Chengdu, 610031, China; 2.Key Laboratory of Particle Astrophyics, Experimental Physics Division, Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, 100049, China; 3.University of Chinese Academy of Sciences, Beijing, 100049, China; 4.TIANFU Cosmic Ray Research Center, Sichuan, Chengdu, China; 5.Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland; 6.Max-Planck-Institut for Nuclear Physics, P.O. Box 103980, Heidelberg, 69029, Germany; 7.State Key Laboratory of Particle Detection and Electronics, China; 8.University of Science and Technology of China, Anhui, Hefei, 230026, China; 9.School of Physical Science and Technology, School of Information Science and Technology, Southwest Jiaotong University, Sichuan, Chengdu, 610031, China; 10.School of Astronomy and Space Science, Nanjing University, Jiangsu, Nanjing, 210023, China; 11.Center for Astrophysics, Guangzhou University, Guangdong, Guangzhou, 510006, China; 12.Hebei Normal University, Hebei, Shijiazhuang, 050024, China; 13.Key Laboratory of Dark Matter and Space Astronomy, Key Laboratory of Radio Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Jiangsu, Nanjing, 210023, China; 14.Tsung-Dao Lee Institute, School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai, 200240, China; 15.Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, 200030, China; 16.Key Laboratory of Cosmic Rays, Tibet University, Ministry of Education, Tibet, Lhasa, 850000, China; 17.National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China; 18.School of Physics and Astronomy, Sun Yat-sen University, Zhuhai, 519000, China; 19.School of Physics, Sun Yat-sen University, Guangdong, Guangzhou, 510275, China; 20.Sino-French Institute of Nuclear Engineering and Technology, Sun Yat-sen University, Zhuhai, 519000, China; 21.School of Physics and Astronomy, Yunnan University, Yunnan, Kunming, 650091, China; 22.Département de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de Genève, 24 Quai Ernest Ansermet, Geneva, 1211, Switzerland; 23.Institute of Frontier and Interdisciplinary Science, Shandong University, Shandong, Qingdao, 266237, China; 24.APC, Université Paris Cité, CNRS, IN2P3, CEA, IRFU, Observatoire de Paris, Paris, 119 75205, France; 25.Department of Engineering Physics, Tsinghua University, Beijing, 100084, China; 26.School of Physics and Microelectronics, Zhengzhou University, Henan, Zhengzhou, 450001, China; 27.Yunnan Observatories, Chinese Academy of Sciences, Yunnan, Kunming, 650216, China; 28.College of Physics, Sichuan University, Sichuan, Chengdu, 610065, China; 29.Institute for Nuclear Research, Russian Academy of Sciences, Moscow, 117312, Russia; 30.School of Physics, Peking University, Beijing, 100871, China; 31.School of Physical Science and Technology, Guangxi University, Guangxi, Nanning, 530004, China; 32.Department of Physics, Faculty of Science, Mahidol University, Bangkok, 10400, Thailand; 33.Moscow Institute of Physics and Technology, Moscow, 141700, Russia; 34.Center for Relativistic Astrophysics and High Energy Physics, School of Physics and Materials Science, Institute of Space Science and Technology, Nanchang University, Jiangxi, Nanchang, 330031, China; 35.National Space Science Center, Chinese Academy of Sciences, Beijing, 100190, China |
| 推荐引用方式 GB/T 7714 | Chen, Xuejian,Zhou, Xunxiu,Yang, Ci,et al. Variations of secondary particle arrival time detected by LHAASO-KM2A during thunderstorms[C],2024. |
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| 文件名称/大小 | 文献类型 | 版本类型 | 开放类型 | 使用许可 | ||
| Variations of second（1762KB） | 会议论文 | 开放获取 | CC BY-NC-SA | 浏览 请求全文 | ||
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