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Flux variations of cosmic ray air showers detected by LHAASO-KM2A during a thunderstorm on June 10, 2021

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【作者】 F.Aharonian安琪阿西克古白立新白云翔包逸炜D.Bastieri毕效军毕玉江蔡金庭曹喆曹臻常进常劲帆陈恩生陈良陈亮陈龙陈明君陈玛丽陈素弘陈松战陈天禄陈学健陈阳程皓麟程宁程耀东崔树旺崔晓红崔昱东戴本忠代洪亮戴子高单增罗布D.della Volpe段凯凯樊军辉范一中范志香方军方堃冯存峰封莉冯少辉丰晓婷冯有亮高博高川东高林青高启高卫高伟康葛茂茂耿利斯龚光华苟全补顾旻皓郭福来郭俊广郭晓磊郭义庆郭莹莹韩毅昂何会海贺昊宁何思乐何新波何钰M.Heller贺远强侯超侯贤胡红波胡铨胡森胡世聪呼晓军黄代绘黄文昊黄性涛黄晓渊黄勇黄志成季筱璐贾焕玉贾康江琨姜泽军金敏康明铭柯通D.Kuleshov李兵兵李澄李骢李飞李海波李会财李华阳李军李剑李捷李凯李文龙李秀荣李昕李新李一卓李哲黎卓梁恩维梁云峰林苏杰刘冰刘成刘栋刘虎刘海东刘佳刘江来刘佳松刘金艳刘茂元柳若愚刘四明刘伟刘怡刘以农龙文杰鲁睿罗晴吕洪魁马伯强马玲玲马欣华毛基荣A.Masood闵振W.Mitthumsiri南云程区子维庞彬宇P.Pattarakijwanich裴致远齐孟尧祁业情乔冰强秦家军D.RuffoloA.Sáiz邵澄宇邵琅O.Shchegolev盛祥东石京燕宋慧超Yu.V.StenkinV.Stepanov苏扬孙秦宁孙晓娜孙志斌谭柏轩唐泽波田文武王博东王超王辉王洪光王建成王界双王利苹王玲玉王冉王润娜王为王祥高王祥玉王阳王玉东王岩谨王亚平王忠海王仲翔王振王铮韦大明魏俊杰魏永健文韬吴超勇吴含荣武莎吴雪峰吴雨生席邵强夏捷夏君集项光漫肖迪泫肖刚辛广广辛玉良邢祎熊峥徐东莲徐仁新薛良闫大海颜景志杨朝文杨冯帆杨何文杨佳盈杨莉莉杨明洁杨睿智杨深邦姚玉华姚志国叶一锰尹丽巧尹娜游晓浩游智勇于艳红袁强岳华曾厚敦曾婷轩曾玮曾宗康查敏翟徐徐张彬彬张丰张海明张恒英张建立张丽霞张力张路张鹏飞张佩佩张瑞张少博张少如张寿山张潇张笑鹏张云峰张月雷张毅张勇赵兵赵静赵雷赵立志赵世平郑福郑应周斌周浩周佳能周平周荣周勋秀祝成光祝凤荣朱辉朱科军左雄

【Author】 F.Aharonian;Q.An;Axikegu;L.X.Bai;Y.X.Bai;Y.W.Bao;D.Bastieri;X.J.Bi;Y.J.Bi;J.T.Cai;Zhe Cao;Zhen Cao;J.Chang;J.F.Chang;E.S.Chen;Liang Chen;Liang Chen;Long Chen;M.J.Chen;M.L.Chen;S.H.Chen;S.Z.Chen;T.L.Chen;X.J.Chen;Y.Chen;H.L.Cheng;N.Cheng;Y.D.Cheng;S.W.Cui;X.H.Cui;Y.D.Cui;B.Z.Dai;H.L.Dai;Z.G.Dai;Danzengluobu;D.della Volpe;K.K.Duan;J.H.Fan;Y.Z.Fan;Z.X.Fan;J.Fang;K.Fang;C.F.Feng;L.Feng;S.H.Feng;X.T.Feng;Y.L.Feng;B.Gao;C.D.Gao;L.Q.Gao;Q.Gao;W.Gao;W.K.Gao;M.M.Ge;L.S.Geng;G.H.Gong;Q.B.Gou;M.H.Gu;F.L.Guo;J.G.Guo;X.L.Guo;Y.Q.Guo;Y.Y.Guo;Y.A.Han;H.H.He;H.N.He;S.L.He;X.B.He;Y.He;M.Heller;Y.K.Hor;C.Hou;X.Hou;H.B.Hu;Q.Hu;S.Hu;S.C.Hu;X.J.Hu;D.H.Huang;W.H.Huang;X.T.Huang;X.Y.Huang;Y.Huang;Z.C.Huang;X.L.Ji;H.Y.Jia;K.Jia;K.Jiang;Z.J.Jiang;M.Jin;M.M.Kang;T.Ke;D.Kuleshov;B.B.Li;Cheng Li;Cong Li;F.Li;H.B.Li;H.C.Li;H.Y.Li;J.Li;Jian Li;Jie Li;K.Li;W.L.Li;X.R.Li;Xin Li;Xin Li;Y.Z.Li;Zhe Li;Zhuo Li;E.W.Liang;Y.F.Liang;S.J.Lin;B.Liu;C.Liu;D.Liu;H.Liu;H.D.Liu;J.Liu;J.L.Liu;J.S.Liu;J.Y.Liu;M.Y.Liu;R.Y.Liu;S.M.Liu;W.Liu;Y.Liu;Y.N.Liu;W.J.Long;R.Lu;Q.Luo;H.K.Lv;B.Q.Ma;L.L.Ma;X.H.Ma;J.R.Mao;A.Masood;Z.Min;W.Mitthumsiri;Y.C.Nan;Z.W.Ou;B.Y.Pang;P.Pattarakijwanich;Z.Y.Pei;M.Y.Qi;Y.Q.Qi;B.Q.Qiao;J.J.Qin;D.Ruffolo;A.Sáiz;C.Y.Shao;L.Shao;O.Shchegolev;X.D.Sheng;J.Y.Shi;H.C.Song;Yu.V.Stenkin;V.Stepanov;Y.Su;Q.N.Sun;X.N.Sun;Z.B.Sun;P.H.T.Tam;Z.B.Tang;W.W.Tian;B.D.Wang;C.Wang;H.Wang;H.G.Wang;J.C.Wang;J.S.Wang;L.P.Wang;L.Y.Wang;R.Wang;R.N.Wang;W.Wang;X.G.Wang;X.Y.Wang;Y.Wang;Y.D.Wang;Y.J.Wang;Y.P.Wang;Z.H.Wang;Z.X.Wang;Zhen Wang;Zheng Wang;D.M.Wei;J.J.Wei;Y.J.Wei;T.Wen;C.Y.Wu;H.R.Wu;S.Wu;X.F.Wu;Y.S.Wu;S.Q.Xi;J.Xia;J.J.Xia;G.M.Xiang;D.X.Xiao;G.Xiao;G.G.Xin;Y.L.Xin;Y.Xing;Z.Xiong;D.L.Xu;R.X.Xu;L.Xue;D.H.Yan;J.Z.Yan;C.W.Yang;F.F.Yang;H.W.Yang;J.Y.Yang;L.L.Yang;M.J.Yang;R.Z.Yang;S.B.Yang;Y.H.Yao;Z.G.Yao;Y.M.Ye;L.Q.Yin;N.Yin;X.H.You;Z.Y.You;Y.H.Yu;Q.Yuan;H.Yue;H.D.Zeng;T.X.Zeng;W.Zeng;Z.K.Zeng;M.Zha;X.X.Zhai;B.B.Zhang;F.Zhang;H.M.Zhang;H.Y.Zhang;J.L.Zhang;L.X.Zhang;Li Zhang;Lu Zhang;P.F.Zhang;P.P.Zhang;R.Zhang;S.B.Zhang;S.R.Zhang;S.S.Zhang;X.Zhang;X.P.Zhang;Y.F.Zhang;Y.L.Zhang;Yi Zhang;Yong Zhang;B.Zhao;J.Zhao;L.Zhao;L.Z.Zhao;S.P.Zhao;F.Zheng;Y.Zheng;B.Zhou;H.Zhou;J.N.Zhou;P.Zhou;R.Zhou;X.X.Zhou;C.G.Zhu;F.R.Zhu;H.Zhu;K.J.Zhu;X.Zuo;Dublin Institute for Advanced Studies;Max-Planck-Institut for Nuclear Physics;State Key Laboratory of Particle Detection and Electronics;University of Science and Technology of China;School of Physical Science and Technology & School of Information Science and Technology,Southwest Jiaotong University;College of Physics, Sichuan University;Key Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center, Institute of High Energy Physics, Chinese Academy of Sciences;TIANFU Cosmic Ray Research Center;School of Astronomy and Space Science, Nanjing University;Center for Astrophysics, Guangzhou University;University of Chinese Academy of Sciences;Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences;Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory,Chinese Academy of Sciences;Key Laboratory of Cosmic Rays (Tibet University), Ministry of Education;National Astronomical Observatories, Chinese Academy of Sciences;Hebei Normal University;School of Physics and Astronomy (Zhuhai) & School of Physics (Guangzhou) & Sino-French Institute of Nuclear Engineering and Technology (Zhuhai), Sun Yat-sen University;School of Physics and Astronomy, Yunnan University, Kunming 650091, China;D’epartement de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de Genève;Institute of Frontier and Interdisciplinary Science, Shandong University;School of Physics and Astronomy, Yunnan University;Department of Engineering Physics, Tsinghua University;School of Physics and Microelectronics, Zhengzhou University;Yunnan Observatories, Chinese Academy of Sciences;Institute for Nuclear Research of Russian Academy of Sciences;School of Physics, Peking University;School of Physical Science and Technology, Guangxi University;Tsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong University;Department of Physics, Faculty of Science, Mahidol University;Moscow Institute of Physics and Technology;National Space Science Center, Chinese Academy of Sciences;

【机构】 Dublin Institute for Advanced StudiesMax-Planck-Institut for Nuclear PhysicsState Key Laboratory of Particle Detection and ElectronicsUniversity of Science and Technology of ChinaSchool of Physical Science and Technology & School of Information Science and Technology,Southwest Jiaotong UniversityCollege of Physics, Sichuan UniversityKey Laboratory of Particle Astrophyics & Experimental Physics Division & Computing Center, Institute of High Energy Physics, Chinese Academy of SciencesTIANFU Cosmic Ray Research CenterSchool of Astronomy and Space Science, Nanjing UniversityCenter for Astrophysics, Guangzhou UniversityUniversity of Chinese Academy of SciencesKey Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy, Purple Mountain Observatory, Chinese Academy of SciencesKey Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory,Chinese Academy of SciencesKey Laboratory of Cosmic Rays (Tibet University), Ministry of EducationNational Astronomical Observatories, Chinese Academy of SciencesHebei Normal UniversitySchool of Physics and Astronomy (Zhuhai) & School of Physics (Guangzhou) & Sino-French Institute of Nuclear Engineering and Technology (Zhuhai), Sun Yat-sen UniversitySchool of Physics and Astronomy, Yunnan UniversityD’epartement de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de GenèveInstitute of Frontier and Interdisciplinary Science, Shandong UniversityDepartment of Engineering Physics, Tsinghua UniversitySchool of Physics and Microelectronics, Zhengzhou UniversityYunnan Observatories, Chinese Academy of Sciences, Kunming 650216, ChinaInstitute for Nuclear Research of Russian Academy of SciencesSchool of Physics, Peking UniversitySchool of Physical Science and Technology, Guangxi UniversityTsung-Dao Lee Institute & School of Physics and Astronomy, Shanghai Jiao Tong UniversityDepartment of Physics, Faculty of Science, Mahidol UniversityMoscow Institute of Physics and TechnologyNational Space Science Center, Chinese Academy of Sciences

【摘要】 The Large High Altitude Air Shower Observatory(LHAASO) has three sub-arrays, KM2A, WCDA, and WFCTA. The flux variations of cosmic ray air showers were studied by analyzing the KM2A data during a thunderstorm on June 10, 2021. The number of shower events that meet the trigger conditions increases significantly in atmospheric electric fields, with a maximum fractional increase of 20%. The variations in trigger rates(increases or decreases) were found to be strongly dependent on the primary zenith angle. The flux of secondary particles increased significantly, following a trend similar to that of shower events. To better understand the observed behavior,Monte Carlo simulations were performed with CORSIKA and G4KM2A(a code based on GEANT4). We found that the experimental data(in saturated negative fields) were in good agreement with the simulations, assuming the presence of a uniform electric field of-700 V/cm with a thickness of 1500 m in the atmosphere above the observation level. Due to the acceleration/deceleration by the atmospheric electric field, the number of secondary particles with energy above the detector threshold was modified, resulting in the changes in shower detection rate.

【Abstract】 The Large High Altitude Air Shower Observatory(LHAASO) has three sub-arrays, KM2A, WCDA, and WFCTA. The flux variations of cosmic ray air showers were studied by analyzing the KM2A data during a thunderstorm on June 10, 2021. The number of shower events that meet the trigger conditions increases significantly in atmospheric electric fields, with a maximum fractional increase of 20%. The variations in trigger rates(increases or decreases) were found to be strongly dependent on the primary zenith angle. The flux of secondary particles increased significantly, following a trend similar to that of shower events. To better understand the observed behavior,Monte Carlo simulations were performed with CORSIKA and G4KM2A(a code based on GEANT4). We found that the experimental data(in saturated negative fields) were in good agreement with the simulations, assuming the presence of a uniform electric field of-700 V/cm with a thickness of 1500 m in the atmosphere above the observation level. Due to the acceleration/deceleration by the atmospheric electric field, the number of secondary particles with energy above the detector threshold was modified, resulting in the changes in shower detection rate.

【基金】 Supported in China by National Key R&D program of China (2018YFA0404201, 2018YFA0404202, 2018YFA0404203, 2018YFA0404204);NSFC (U2031101,11475141, 12147208);in Thailand by RTA6280002 from Thailand Science Research and Innovation
  • 【文献出处】 Chinese Physics C ,中国物理C , 编辑部邮箱 ,2023年01期
  • 【分类号】P426.62;P172.4
  • 【下载频次】3
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