论文标题
在超X射线源M51 ULX-8中的中子星的自旋时期
On the Spin Period of the Neutron Star in the Ultraluminous X-Ray Source M51 ULX-8
论文作者
论文摘要
最近发现了附近星系中多个X射线源（ULX）家族的几个成员以及我们自己的星系中的定期脉动，揭示了积聚紧凑型物体的性质。目前认为，无论是否观察到脉动，中子星而不是黑洞都可以为大量的ULX提供动力。 ULX的X射线谱中的回旋型吸收线的检测提供了一种替代方法，可以将紧凑型物体识别为中子恒星。在非脉冲ULX中，据报道，M51 ULX-8频谱中的回旋共振散射特征（CRSF）的存在。在目前的工作中，从观察到的CRSF的能量中推断出M51 ULX-8中中子恒星表面的磁场强度，以估计X射线发射中的光束分数，更重要的是，在近乎即将到来的即将到来的即将到来的太空任务可以发现难以捉摸的中子星形旋转期的可观察到的范围。
The recent discovery of periodic pulsations from several members of the ultraluminous X-ray source (ULX) family in nearby galaxies as well as in our own galaxy unveiled the nature of the accreting compact object. Neutron stars rather than black holes are currently believed to power a substantial number of ULXs whether or not pulsations are observed. The detection of cyclotron absorption lines in the X-ray spectrum of a ULX provides an alternative way to identify the compact object as a neutron star. Among the non-pulsating ULXs, the presence of a cyclotron resonance scattering feature (CRSF) in the spectrum of M51 ULX-8 has been reported. In the present work, the magnetic field strength on the surface of the neutron star in M51 ULX-8 is inferred from the energy of the observed CRSF to estimate the beaming fraction in X-ray emission and more importantly the observable range for the elusive neutron-star spin period to be hopefully discovered by the forthcoming space missions in the near future.
