AI 中文总结
本综述介绍吸积中子星的吸积机制与脉冲轮廓观测技术，总结脉冲轮廓与X射线光度、能量的关联，探讨观测量与吸积机制的理论联系，并指出未来观测及理论模型发展方向。
AI 中文摘要
X射线脉冲星是具有强磁场（B~10^12 G）的中子星，通过吸积伴星物质形成。其特征性X射线辐射源于从相对论速度减速的吸积物质，这些物质在中子星的磁极附近被减速。由于我们观测磁极的视线会随中子星的自转发生变化，X射线会呈现周期性调制，进而产生X射线脉冲。脉冲轮廓的形状取决于多个因素：磁极处明亮X射线与下落物质相互作用的物理过程、磁极相对于中子星自转轴的位置，以及中子星周围的时空特性。在本综述中，我们对各类吸积中子星系统中运作的吸积机制，以及用于表征脉冲轮廓的观测技术进行了教学性介绍。我们总结了脉冲轮廓如何依赖于X射线光度和能量，并讨论了将这些观测量与物理吸积机制建立理论联系的尝试。最后，我们概述了未来的观测需求以及磁吸积理论模型的进一步发展方向。
英文摘要
X-ray pulsars are highly magnetized ($B\sim 10^{12}$ G) neutron stars accreting from a donor star. Their characteristic X-ray emission arises from accreted material decelerated from relativistic velocities near the magnetic poles of the neutron star. As our line of sight onto the magnetic poles changes with the rotation of the neutron star, the X-rays are periodically modulated, resulting in X-ray pulsations. The shape of the pulse profiles depends on the physics of the interaction between the bright X-rays from the magnetic poles with the infalling matter, the location of the magnetic poles on the neutron star with respect to its spin axis, and on the properties of the space-time around the neutron star. In this review we give a pedagogical introduction to the accretion mechanisms operating in the various types of accreting neutron star systems and the observational techniques used to characterize the pulse profiles. We summarize how the pulse profiles depend on X-ray luminosity and energy and discuss the attempts to connect theoretically these observables with the physical accretion mechanisms. We conclude with an outline of future observational needs and further developments for theoretical models of magnetic accretion.
Comments171 pages, 23 Figures, 777 references. Submitted for publication in Space Science Reviews. This is the authors' version having responded to the comments raised by the referees
