极亮X射线源NGC 5907 ULX-1的磁场研究  

Study on magnetic field of pulsating ultra luminous X-ray source:NGC 5907 ULX-1

作　　者：黄飞龙 潘元月 HUANG Feilong;PAN Yuanyue(Key Laboratory of Stars and Interstellar Medium,Xiangtan University,Xiangtan Hunan 411105)

机构地区：[1]湘潭大学恒星与星际物质重点实验室,湖南湘潭411105

出　　处：《首都师范大学学报（自然科学版）》2022年第2期36-41,共6页Journal of Capital Normal University：Natural Science Edition

摘　　要：极亮X射线脉冲星的证认表明,极亮X射线源中可能存在一定数量的中子星,其拥有超爱丁顿极限光度和较高的自转周期变化率,这些特性可能与星体的磁场密切相关.NGC 5907 ULX-1是第三颗证认的极亮X射线脉冲星,其峰值光度约为爱丁顿极限的1000倍.本文计算了NGC 5907 ULX-1目前的偶极磁场强度,并模拟了其随时间的演化规律.结果显示,这颗源目前的偶极磁场约为10^(13) G,演化初期的磁场约为10^(15) G,故推断NGC 5907 ULX-1可能为吸积的磁星,其多极强磁场解释了观测的超高光度现象.同时认为,极亮X射线脉冲星极有可能是吸积的磁星,是研究磁星的相关性质及吸积演化规律的重要依据.The confirming of the pulsating ultra luminous X-ray sources(PULXs)illustrates that there should be a certain number of accretion neutron stars in ultra luminous X-ray sources.The supper Eddington limits luminosity and high spin-up rates of PULXs might be related to the magnetic field of the source.NGC 5907 ULX-1 is the third confirmed PULX,whose peak luminosity is about 1000 times the Eddington limit.In this paper,the current dipole magnetic field intensity of NGC 5907 ULX-1 is calculated and the evolution of the magnetic field decayed with the accretion time is simulated.It is found that its present dipole magnetic field and initial magnetic field of evolution are 10^(13) and 10^(15) G,respectively.Thus,it is inferred that NGC 5907 ULX-1 might be an accretion magnetar,whose multiple strong magnetic fields support the observed phenomenon of ultrahigh luminosity.At the same time,it is considered that PULXs might be the accreting magnetars,which might be an important key for studying the relative characteristic and accretion evolution of magnetars.

关 键 词：脉冲星双星 超爱丁顿光度 吸积 磁场 

分 类 号：P1[天文地球—天文学]