Chapter 6 Multimessenger Physics  

作　　者：Zhuo Li Giuseppe Di Sciascio Quan-Bu Gou Yi-Qing Guo Hao-Ning He Ruo-Yu Liu Kai Wang 黎卓;Giuseppe Di Sciascio;苟全补;郭义庆;贺昊宁;柳若愚;王凯(INFN-Roma Tor Vergata,Via della Ricerca Scientifica 1,00133 Rome,Italy;Key Laboratory of Particle Astrophysics,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China;Key Laboratory of Dark Matter and Space Astronomy,Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,China;Department of Astronomy,School of Physics,Peking University,Beijing 100871,China;Kavli Institute for Astronomy and Astrophysics,Peking University,Beijing 100871,China;School of Astronomy and Space Science,Nanjing University,Nanjing 210023,China;Key laboratory of Modern Astronomy and Astrophysics(Nanjing University),Ministry of Education,Nanjing 210023,China;Department of Astronomy,School of Physics,Huazhong University of Science and Technology,Wuhan 430074,China)

机构地区：[1]INFN-Roma Tor Vergata,Via della Ricerca Scientifica 1,00133 Rome,Italy [2]Key Laboratory of Particle Astrophysics,Institute of High Energy Physics,Chinese Academy of Sciences,Beijing 100049,China [3]Key Laboratory of Dark Matter and Space Astronomy,Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210023,China [4]Department of Astronomy,School of Physics,Peking University,Beijing 100871,China [5]Kavli Institute for Astronomy and Astrophysics,Peking University,Beijing 100871,China [6]School of Astronomy and Space Science,Nanjing University,Nanjing 210023,China [7]Key laboratory of Modern Astronomy and Astrophysics(Nanjing University),Ministry of Education,Nanjing 210023,China [8]Department of Astronomy,School of Physics,Huazhong University of Science and Technology,Wuhan 430074,China

出　　处：《Chinese Physics C》2022年第3期139-152,共14页中国物理C（英文版）

基　　金：Supported by the Natural Science Foundation of China(11773003,11875264,12003007,12173091,U1931201,U2031105);the Fundamental Research Funds for the Central Universities(2020kfyXJJS039)。

摘　　要：Combining observations of multi-messengers help in boosting the sensitivity of astrophysical source searches,and probe various aspects of the source physics.In this chapter we discuss how LHAASO observations of very high energy(VHE)gamma rays in combination with telescopes for the other messengers can help in solving the origins of VHE neutrinos and galactic and extragalactic cosmic rays.

关 键 词：Cosmic ray GAMMA-RAY NEUTRINO LHAASO 

分 类 号：P172.4[天文地球—天文学]