论文标题
中子星的自旋演变在风馈高质量X射线二进制中
Spin evolution of neutron stars in wind-fed high mass X-ray binaries
论文作者
论文摘要
观察到的OB型高质量X射线二进制（HMXB）的X射线脉冲周期通常长于100秒。据认为，中子恒星的强磁场与风质之间的相互作用可能会导致如此长的脉冲周期。 在这项研究中，我们遵循NS的自旋演变，考虑到磁场和风质之间的相互作用。在这一线中，作为新挑战，我们同时解决了中子恒星的磁场的演变，此外，我们集中于供体风能的影响。结果，获得了进化轨道，其中中子恒星在出生后在喷出器阶段花费了一段时间，然后迅速旋转，变为准平衡，并逐渐旋转。这种进化类似于以前的研究，但我们发现它的主要物理学取决于供体风的速度。当风速快速时，由于磁性抑制而发生旋转，而经典的螺旋桨效应和沉降积聚壳会导致在慢速促进的速度积聚中迅速旋转。由于供体的风速可能取决于受照射的X射线发光度，因此在风馈HMXB中中子星的自旋进化轨道可能比考虑的要复杂。
The observed X-ray pulse period of OB-type high-mass X-ray binary (HMXB) pulsars are typically longer than 100 seconds. It is considered that the interaction between the strong magnetic field of neutron star and the wind matter could cause such a long pulse period. In this study, we follow the spin evolution of NS, taking into account the interaction between the magnetic field and wind matter. In this line, as new challenges, we solve the evolution of the magnetic field of the neutron star at the same time, and additionally we focus on the effects of wind properties of the donor. As the result, evolutionary tracks were obtained in which the neutron star spends some duration in the ejector phase after birth, then rapidly spins down, becomes quasi-equilibrium, and gradually spins up. Such evolution is similar to previous studies, but we found that its dominant physics depends on the velocity of the donor wind. When the wind velocity is fast, the spin-down occurs due to magnetic inhibition, while the classical propeller effect and settling accretion shell causes rapid spin-down in the slow wind accretion. Since the wind velocity of the donor could depend on the irradiated X-ray luminosity, the spin evolution track of the neutron star in wind-fed HMXB could be more complicated than considered.
