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arXiv 2209.08540astro-ph.SRastro-ph.HE
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磁约束星风激波

Magnetically confined wind shock

Asif ud-Doula, Stan Owocki

备注：
Accepted for publication invited chapter of the Handbook of X-ray and Gamma-ray Astrophysics published by Nature Springer. arXiv admin note: text overlap with arXiv:1509.06482, arXiv:1605.04979
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AI总结：

本文综述了大质量恒星磁约束星风激波的理论研究，涵盖磁场对星风的捕获、激波产生X射线机制、热等离子体性质、MHD建模及Hα发射控制机制。

摘要：

各类恒星中，许多恒星拥有足够强的磁场，能够影响其表面物质流动。对于大质量恒星（O型和B型），约10%具有强且全局有序（多为偶极）的磁场。在闭合磁环中，星风的捕获与引导导致磁约束星风激波（MCWS），激波前流速为星风终端速度的几分之一，可达每秒数千公里。这些激波产生热等离子体，是X射线的来源。过去十年取得多项进展，特别是利用XMM和Chandra测定大样本热等离子体性质，以及完全自洽的MHD建模和弱风中激波后退效应的识别。此外，这些天体常是Hα发射源，其发射由足够高的质量损失率或离心突破控制。本文综述此类磁性大质量恒星星风动力学的理论方面。

英文摘要：

Many stars across all classes possess strong enough magnetic fields to influence dynamical flow of material off the stellar surface. For the case of massive stars (O and B types), about 10\% of them harbour strong, globally ordered (mostly dipolar) magnetic fields. The trapping and channeling of their stellar winds in closed magnetic loops leads to {\it magnetically confined wind shocks} (MCWS), with pre-shock flow speeds that are some fraction of the wind terminal speed that can be a few thousand km s$^{-1}$. These shocks generate hot plasma, a source of X-rays. In the last decade, several developments took place, notably the determination of the hot plasma properties for a large sample of objects using \xmm\ and \ch, as well as fully self-consistent MHD modelling and the identification of shock retreat effects in weak winds. In addition, these objects are often sources of H$α$ emission which is controlled by either sufficiently high mass loss rate or centrifugal breakout. Here we review the theoretical aspects of such magnetic massive star wind dynamics.

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