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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Spin evolution of neutron stars in wind-fed high-mass X-ray binaries
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Spin evolution of neutron stars in wind-fed high-mass X-ray binaries

机译：风送高质量X射线二进制中中子恒星的旋转演变

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摘要

The observed X-ray pulse period of OB-type high-mass X-ray binary (HMXB) pulsars is typically longer than 100 seconds. It is considered that the interaction between the strong magnetic field of a neutron star and the wind matter could cause such a long pulse period. In this study, we follow the spin evolution of neutron stars, 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 the wind properties of the donor. As a 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 a wind-fed HMXB could be more complicated than considered.
机译：OB型高质量X射线双星（HMXB）脉冲星观测到的X射线脉冲周期通常超过100秒。我们认为中子星的强磁场与风物质之间的相互作用可能导致如此长的脉冲周期。在这项研究中，我们跟踪中子星的自旋演化，考虑了磁场和风物质之间的相互作用。在这方面，作为新的挑战，我们同时解决了中子星磁场的演化问题，此外，我们还关注了施主的风特性的影响。结果，获得了中子星在出生后在喷射阶段停留一段时间，然后迅速向下旋转，达到准平衡，然后逐渐向上旋转的演化轨迹。这种演化与之前的研究类似，但我们发现其主要物理特性取决于施主风的速度。当风速很快时，由于磁抑制会发生自旋下降，而在慢风吸积中，经典螺旋桨效应和沉降吸积壳会导致快速自旋下降。由于施主的风速可能取决于辐照的X射线光度，因此在风馈送的HMXB中中子星的自旋演化轨迹可能比考虑的更复杂。

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