Revisit the γ-Ray Flare Associated with Blazar Mrk 421  

作　　者：Xiang-Tao Zeng Ze-Yuan Tang Jun-Hui Fan 

机构地区：[1]Center for Astrophysics,Guangzhou University,Guangzhou 510006,China [2]Greater Bay Brand Center of the National Astronomical Data Center,Guangzhou 510006,China [3]Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province,Guangzhou 510006,China

出　　处：《Research in Astronomy and Astrophysics》2024年第12期53-60,共8页天文和天体物理学研究(英文版)

基　　金：partially supported by the National Natural Science Foundation of China (NSFC, grant Nos. 12433004, U2031201, and 11733001);Guangdong Major Project of Basic and Applied Basic Research (grant No. 2019B030302001);the science research grants from the China Manned Space Project with No. CMS-CSST-2021-A06;the support for Astrophysics Key Subjects of Guangdong Province and Guangzhou City;The Key Laboratory for Astronomical Observation and Technology of Guangzhou also supports the work。

摘　　要：A Very High-energy(VHE) flare was observed by Major Atmospheric Gamma Imaging Cherenkov Telescopes on MJD 57788. This VHE flare was characterized by increased VHE flux and short timescales. In this study, we used one-zone synchrotron self-Compton, two-zone, and spine/layer models to explore this VHE flare's origin. The results indicate that this γ-ray flare can be explained by Inverse Compton Scattering radiation from the layer contributed gamma radiation and results in the γ-ray flare in a different way than the two-zone model. The difference between the two models lies in the performance of spectral energy distribution after γ-ray flare as well as a possible difference in the timescales of the flare.

关 键 词：radiation mechanisms non-thermal-(galaxies) BL Lacertae objects individual(Mrk 421)-galaxies jets 

分 类 号：P157.6[天文地球—天文学]