耀变体1ES 0229+200的GeV强伽玛射线辐射  

Stronger GeV γ-rays Emission in Extreme Blazar 1ES 0229+200

作　　者：刘雨 李金 徐云冰[1,3] LIU Yu LI Jin XU Yun-bing(School of Physics and Electronic Information,Yunnan Normal University,Kunming 650500,China No 1. Middle School of Fuyuan, Fuyuan 655500, China Experimental Teaching Demons tration Center for Physics,Yunnan Normal University,Kunming 650500,China)

机构地区：[1]云南师范大学物理与电子信息学院,云南昆明650500 [2]富源县第一高级中学,云南富源655500 [3]云南师范大学物理实验教学示范中心,云南昆明650500

出　　处：《云南师范大学学报（自然科学版）》2017年第5期1-7,共7页Journal of Yunnan Normal University:Natural Sciences Edition

基　　金：云南省教育厅基金资助项目(2016ZZX066)

摘　　要：利用次级伽玛射线辐射模型解释耀变体1ES 0229+200的GeV强伽玛射线辐射.在该模型中,源内初级光子和源外次级光子都对观测到的高能伽玛射线辐射有贡献.假定一个合适的电子能谱和星际磁场(IGMF),获得了耀变体1ES 0229+200的能谱.研究结果表明:GeV强伽玛射线辐射来源于正负电子对(e±)散射宇宙微波背景(CMB)光子产生的次级伽玛射线.In this paper,we consider a secondaryγ-rays emission component to an extreme blazar 1ES 0229 ＋200 for the stronger GeV emission.In the model,both the primary photons produced in the source and secondary photons produced outside the source contribute to the observed high energyγ-rays emission.Assuming a suitable electron spectra and intergalactic magnetic fields（IGMF）,we obtain the spectrum of 1ES 0229＋200.The results indicated that the stronger GeV emission derived from secondaryγ-rays produced in the scattering of e±pairs with the cosmic microwave background （CMB） photons.

关 键 词：星系 BL Lac天体 1ES 0229+200 辐射机制 非热 

分 类 号：P14[天文地球—天体物理]