作为X射线脉冲星的磁星  

Magnetars as X-ray Pulsars

作　　者：李向东[1] 

机构地区：[1]南京大学天文系

出　　处：《云南天文台台刊》2003年第1期1-5,共5页Publications of the Yunnan Observatoty

基　　金：This work was supported by NSFC and NKBRSF.

摘　　要：研究表明 ,与磁星模型相比较 ,反常X射线脉冲星的加速模型不能说明所观测到的自转周期的分布。为了解释熟知的最慢X射线脉冲星 2S 0 114+6 5 0的性质 ,其磁场强度必须大于 10 14 Gs ,即它诞生时即为一磁体。We have shown that,compared with the magnetar model,the accretion model for the anomalous X-ray pulsars is unable to account for the distributions of the spin periods observed.To explain the properties of the known slowest X-ray pulsar 2S 0114+650,the magnetic field strength of this pulsar must be initially 10 14 Gs,that is,it was born as a magnetar.

关 键 词：磁星 脉冲星 中子星 X射线星 磁场强度 

分 类 号：P145.6[天文地球—天体物理]