The Year-scale X-Ray Variations in the Core of M87

作     者：Yu-Lin Cheng Fei Xiang Heng Yu Shu-Mei Jia Xiang-Hua Li Cheng-Kui Li Yong Chen Wen-Cheng Feng Yu-Lin Cheng;Fei Xiang;Heng Yu;Shu-Mei Jia;Xiang-Hua Li;Cheng-Kui Li;Yong Chen;Wen-Cheng Feng

作者机构：Department of AstronomyYunnan UniversityKunming 650091China Department of AstronomyBeijing Normal UniversityBeijing 100875China Key Laboratory of Particle AstrophysicsInstitute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Department of Physics and Institute of Theoretical PhysicsNanjing Normal UniversityNanjing 210023China 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2023年第23卷第6期

页      面：203-211页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：supported by the National Natural Science Foundation of China(Grant Nos.11863006,U1838203,and U2038104) the Science&Technology Department of Yunnan Province—Yunnan University Joint Funding(2019FY003005) the Bureau of International Cooperation,Chinese Academy of Sciences under the grant GJHZ1864 

主　　题：X-rays:galaxies galaxies:clusters:individual(M87) accretion accretion disks 

摘      要：The analysis of light variation of M87 can help us understand the disk *** the past decade,M87 has experienced several short-term light variabilities related to *** also find that there are year-scale X-ray variations in the core of *** light variability properties are similar to *** re-analyzing 56Chandra observations from 2007 to 2019,we distinguish the“non-flaring statefrom“flaring statein the light *** removing flaring state data,we identify four gas clumps in the nucleus and all of them can be well fitted by the clumpy-ADAF *** average mass accretion rate is~0.16M⊙yr^(-1).We analyze the photon index(Γ)-flux(2-10 keV)correlation between the non-flaring state and flaring *** the non-flaring states,the flux is inversely proportional to the photon *** the flaring states,we find no obvious correlation between the two *** addition,we find that the flare always occurs at a high mass accretion rate,and after the luminosity of the flare reaches the peak,it will be accompanied by a sudden decrease in *** results can be explained as that the energy released by magnetic reconnection destroys the structure of the accretion disk,thus the luminosity decreases rapidly and returns to normal levels thereafter.