Interactions of type I X-ray bursts with thin accretion disks
Interactions of type I X-ray bursts with thin accretion disks
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DOI：
10.1038/s41550-019-0987-5
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发表时间：
2020-01
期刊：
影响因子：
14.1
通讯作者：
P. C. Fragile;D. Ballantyne;Aidan Blankenship
中科院分区：
文献类型：
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作者：
P. C. Fragile;D. Ballantyne;Aidan Blankenship
在I型X射线爆发期间对X射线光谱的仔细观测已经暗示了在双星系统的中子星组件周围的吸积盘的内部区域发生的变化。在这里，我们进行了一组数值实验研究薄，Shakura-Sunyaev型吸积盘的相互作用，这样的爆发。我们现在清楚地证明了一些关键的影响，同时发生，包括弱的证据，辐射驱动的外流沿着表面的磁盘;大量的坡印廷-罗伯逊（PR）阻力，导致增强吸积;和突出的加热盘，这增加了高度，同时降低密度和光学深度。PR阻力导致盘的内边缘从中子星表面向更大的半径撤退，然后在爆发的时间尺度上恢复。我们的结论是，丰富的相互作用的X射线爆发与周围的磁盘提供了一种新的方式来研究物理吸积到紧凑的对象。
Careful observations of X-ray spectra during type I X-ray bursts have hinted at changes occurring in the inner regions of the accretion disks around the neutron-star component of the binary system. Here, we perform a set of numerical experiments studying the interaction of such bursts with thin, Shakura–Sunyaev-type accretion disks. We now clearly demonstrate a number of key effects that take place simultaneously, including evidence for weak, radiation-driven outflows along the surface of the disk; substantial levels of Poynting–Robertson (PR) drag, leading to enhanced accretion; and prominent heating in the disk, which increases the height, while lowering the density and optical depth. The PR drag causes the inner edge of the disk to retreat from the neutron-star surface toward larger radii and then recover on the timescale of the burst. We conclude that the rich interaction of an X-ray burst with the surrounding disk provides a novel way to study the physics of accretion onto compact objects.