软γ射线重爆GB790107的辐射机制  

The Radiation Mechanism for the Soft Gamma Ray Repeater GB790107

作　　者：詹善群 史天一[2] 赵平波 

机构地区：[1]安徽师范大学物理系芜湖,241000 [2]北京师范大学物理系 [3]湖南师范大学物理系

出　　处：《天体物理学报》1993年第4期342-346,共5页

基　　金：国家自然科学基金

摘　　要：本文在中子星吸积彗星云模型的基础上，认为软重爆ＧＢ７９０１０７起源于弱磁化中子星，其阵雨式地吸积彗星云将在中子星表面形成一光厚辐射区，该辐射区的温度分布由激波模型确定，这一辐射区中的高温等离子体产生的黑体辐射将很好地拟合ＧＢ７９０１０７的观测能谱，且获得爆源距离为（１．３５－１３．５）ｐｃ。On the basis of the model that a neutron star accretes the comet clouds around it, we put forward that the soft gamma ray repeater GB790107 originates from the weak magnetic field (~108G) old neutron star. The accretion on the neutron star forms an optically thick radiation region, whose temperature distribution is determined by shock wave model proposed by Munt, and whose blackbody emission can fit the observational spectrum of GB790107 well. We find that the source distance is between 1.35 pc and 13.5 pc.

关 键 词：中子星 Γ射线爆 辐射机制 

分 类 号：P145.6[天文地球—天体物理]