【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.Ruffolo;
A.Sáiz;
邵澄宇;
邵琅;
O.Shchegolev;
盛祥东;
石京燕;
宋慧超;
Yu.V.Stenkin;
V.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 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;
D’epartement de Physique Nucléaire et Corpusculaire, Faculté de Sciences, Université de Genève;
Institute of Frontier and Interdisciplinary Science, Shandong University;
Department of Engineering Physics, Tsinghua University;
School of Physics and Microelectronics, Zhengzhou University;
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China;
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;
【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.更多还原
【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.更多还原
【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