脉冲星磁球层中的非热光子谱  

Non-Thermal Photon Spectra from Pulsar Magneto Spheresin

作　　者：吴云飞[1] 白金泉[1] 曹亚杰[1] 吴春雷 周海明[1] 

机构地区：[1]佳木斯大学理学院,黑龙江佳木斯154007 [2]海伦市第一中学,黑龙江海伦152300

出　　处：《佳木斯大学学报（自然科学版）》2016年第4期627-629,632,共4页Journal of Jiamusi University：Natural Science Edition

基　　金：佳木斯大学2013科学技术研究面上项目(L2013-081)

摘　　要：应用全电磁级联模型计算五颗正常脉冲星和两颗毫秒脉冲星的非热光子谱。该模型下五颗正常脉冲星和一颗毫秒脉冲星的模拟结果与Vela和Geminga做了比较,描述结果相对吻合,其它的三颗伽玛射线脉冲星则部分吻合。相比较正常脉冲星,应用离散相关函数方法来计算毫秒脉冲星的流量,得出这颗颗脉冲星在70Ge V附近有一个高能截断。在X射线能段,起主要作用的是电子对产生的同步辐射,而电子对逆康普顿散射的贡献则可忽略,模拟非热光子谱和Harding的结果粗略一致。The non -thermal photon spectrum of five normal pulsars and two millisecond pulsars is calculated by using the observed data. Using the frame of full polar cap cascade scenario, and compare the model resuits for six pulsars with the result from Vela and Geminga, the result description is identical, and part of the other three Gamma Ray pulsars is identical. The millisecond pulsars are calculated by using the method of discrete correlation function （DCF）, the high energy cutoff appears on 70GeV. The synchrotron radiation plays a major role in X - ray band, and the effect of inverse Compton scatter could be neglected. The simulated non - thermal photon spectra effect is roughly same with Harding.

关 键 词：脉冲星 非热光子谱 辐射 

分 类 号：P141.5[天文地球—天体物理]