【作者】
庞彬宇；
阿布都沙拉木·阿布都克力木；
薄子豪；
陈葳；
谌勋；
程晨；
成兆侃；
崔祥仪；
樊英杰；
方德清；
符长波；
付孟婷；
耿立升；
Karl Giboni；
顾琳慧；
郭绪元；
韩晨成；
韩柯；
何昶达；
何金荣；
黄迪；
黄彦霖；
黄俊挺；
黄周；
侯汝全；
侯钰；
季向东；
巨永林；
李晨翔；
李家富；
李名川；
李帅杰；
李涛；
林箐；
刘江来；
陆聪聪；
芦晓盈；
罗棱尹；
罗云阳；
马文博；
马余刚；
冒亚军；
孟月；
宁旭阳；
祁宁春；
钱志成；
任祥祥；
Nasir Shaheed；
尚晓凤；
邵熙元；
申国防；
司琳；
孙文良；
谈安迪；
陶奕；
王安庆；
王萌；
王秋红；
王少博；
王思广；
王为；
王秀丽；
王舟；
魏月环；
武蒙蒙；
邬维浩；
夏经铠；
肖梦姣；
肖翔；
谢鹏伟；
燕斌斌；
颜玺雨；
杨继军；
杨勇；
姚玉坤；
喻纯旭；
袁影；
苑哲；
曾鑫宁；
张丹；
张敏桢；
张鹏；
张世博；
张澍；
张涛；
张洋；
张瀛心；
张园园；
赵力；
郑其斌；
周济芳；
周宁；
周小朋；
周永；
周钰博；
【Author】
Binyu Pang;Abdusalam Abdukerim;Zihao Bo;Wei Chen;Xun Chen;Chen Cheng;Zhaokan Cheng;Xiangyi Cui;Yingjie Fan;Deqing Fang;Changbo Fu;Mengting Fu;Lisheng Geng;Karl Giboni;Linhui Gu;Xuyuan Guo;Chencheng Han;Ke Han;Changda He;Jinrong He;Di Huang;Yanlin Huang;Junting Huang;Zhou Huang;Ruquan Hou;Yu Hou;Xiangdong Ji;Yonglin Ju;Chenxiang Li;Jiafu Li;Mingchuan Li;Shuaijie Li;Tao Li;Qing Lin;QiJianglaing Liu;Congcong Lu;Xiaoying Lu;Lingyin Luo;Yunyang Luo;Wenbo Ma;Yugang Ma;Yajun Mao;Yue Meng;Xuyang Ning;Ningchun Qi;Zhicheng Qian;Xiangxiang Ren;Nasir Shaheed;Xiaofeng Shang;Xiyuan Shao;Guofang Shen;Lin Si;Wenliang Sun;Andi Tan;Yi Tao;Anqing Wang;Meng Wang;Qiuhong Wang;Shaobo Wang;Siguang Wang;Wei Wang;Xiuli Wang;Zhou Wang;Yuehuan Wei;Mengmeng Wu;Weihao Wu;Jingkai Xia;Mengjiao Xiao;Xiang Xiao;Pengwei Xie;Binbin Yan;Xiyu Yan;Jijun Yang;Yong Yang;Yukun Yao;Chunxu Yu;Ying Yuan;Zhe Yuan;Xinning Zeng;Dan Zhang;Minzhen Zhang;Peng Zhang;Shibo Zhang;Shu Zhang;Tao Zhang;Yang Zhang;Yingxin Zhang;Yuanyuan Zhang;Li Zhao;Qibin Zheng;Jifang Zhou;Ning Zhou;Xiaopeng Zhou;Yong Zhou;Yubo Zhou;Research Center for Particle Science and Technology,Institute of Frontier and Interdisciplinary Science,Shandong University;Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education,Shandong University;School of Physics and Astronomy,Shanghai Jiao Tong University,Key Laboratory for Particle Astrophysics and Cosmology (MoE),Shanghai Key Laboratory for Particle Physics and Cosmology;Shanghai Jiao Tong University Sichuan Research Institute;School of Physics,Sun Yat-Sen University;Sino-French Institute of Nuclear Engineering and Technology,Sun Yat-Sen University;New Cornerstone Science Laboratory,Tsung-Dao Lee Institute,Shanghai Jiao Tong University;Key Laboratory of Nuclear Physics and Ion-beam Application (MOE),Institute of Modern Physics,Fudan University;School of Physics,Peking University;School of Physics,Beihang University;International Research Center for Nuclei and Particles in the Cosmos & Beijing Key Laboratory of Advanced Nuclear Materials and Physics,Beihang University;School of Physics and Microelectronics,Zhengzhou University;Yalong River Hydropower Development Company,Ltd.;School of Medical Instrument and Food Engineering,University of Shanghai for Science and Technology;School of Mechanical Engineering,Shanghai Jiao Tong University;Department of Physics,University of Maryland,College Park;Department of Physics,Yantai University;State Key Laboratory of Particle Detection and Electronics,University of Science and Technology of China;Department of Modern Physics,University of Science and Technology of China;School of Physics,Nankai University;SJTU Paris Elite Institute of Technology,Shanghai Jiao Tong University;School of Physics and Astronomy,Sun Yat-Sen University;
【通讯作者】
张洋;
【机构】
Research Center for Particle Science and Technology,Institute of Frontier and Interdisciplinary Science,Shandong University；
Key Laboratory of Particle Physics and Particle Irradiation of Ministry of Education,Shandong University；
School of Physics and Astronomy,Shanghai Jiao Tong University,Key Laboratory for Particle Astrophysics and Cosmology (MoE),Shanghai Key Laboratory for Particle Physics and Cosmology；
Shanghai Jiao Tong University Sichuan Research Institute；
School of Physics,Sun Yat-Sen University；
Sino-French Institute of Nuclear Engineering and Technology,Sun Yat-Sen University；
New Cornerstone Science Laboratory,Tsung-Dao Lee Institute,Shanghai Jiao Tong University；
Key Laboratory of Nuclear Physics and Ion-beam Application (MOE),Institute of Modern Physics,Fudan University；
School of Physics,Peking University；
School of Physics,Beihang University；
International Research Center for Nuclei and Particles in the Cosmos & Beijing Key Laboratory of Advanced Nuclear Materials and Physics,Beihang University；
School of Physics and Microelectronics,Zhengzhou University；
Yalong River Hydropower Development Company,Ltd.；
School of Medical Instrument and Food Engineering,University of Shanghai for Science and Technology；
School of Mechanical Engineering,Shanghai Jiao Tong University；
Department of Physics,University of Maryland,College Park；
Department of Physics,Yantai University；
State Key Laboratory of Particle Detection and Electronics,University of Science and Technology of China；
Department of Modern Physics,University of Science and Technology of China；
School of Physics,Nankai University；
SJTU Paris Elite Institute of Technology,Shanghai Jiao Tong University；
School of Physics and Astronomy,Sun Yat-Sen University；
【摘要】 Neutrinos from core-collapse supernovae are essential for understanding neutrino physics and stellar evolution. Dual-phase xenon dark matter detectors can be used to track explosions of galactic supernovae by detecting neutrinos through coherent elastic neutrino-nucleus scatterings. In this study, a variation of progenitor masses and explosion models are assumed to predict neutrino fluxes and spectra, which result in the number of expected neutrino events ranging from 6.6 to 13.7 at a distance of 10 kpc over a 10-s duration with negligible backgrounds at PandaX-4T. Two specialized triggering alarms for monitoring supernova burst neutrinos are built. The efficiency of detecting supernova explosions at various distances in the Milky Way is estimated. These alarms will be implemented in the real-time supernova monitoring system at PandaX-4T in the near future, which will provide supernova early warnings for the astronomical community.更多还原
【Abstract】 Neutrinos from core-collapse supernovae are essential for understanding neutrino physics and stellar evolution. Dual-phase xenon dark matter detectors can be used to track explosions of galactic supernovae by detecting neutrinos through coherent elastic neutrino-nucleus scatterings. In this study, a variation of progenitor masses and explosion models are assumed to predict neutrino fluxes and spectra, which result in the number of expected neutrino events ranging from 6.6 to 13.7 at a distance of 10 kpc over a 10-s duration with negligible backgrounds at PandaX-4T. Two specialized triggering alarms for monitoring supernova burst neutrinos are built. The efficiency of detecting supernova explosions at various distances in the Milky Way is estimated. These alarms will be implemented in the real-time supernova monitoring system at PandaX-4T in the near future, which will provide supernova early warnings for the astronomical community.更多还原
【基金】 This project is Supported in part by the National Natural Science Foundation of China (12090060, 12090063, 12105052, 12005131, 11905128, 11925502);the Office of Science and Technology,Shanghai Municipal Government,China (22JC1410100)
