论文标题
磁冲击
Magnetically confined wind shock
论文作者
论文摘要
所有类别的许多恒星都具有足够强的磁场，以影响恒星表面的材料动态流。对于巨大的恒星（O和B类型），其中约有10 \％具有强烈的，全球有序的（主要是偶极）的磁场。其恒星风在封闭的磁路中的捕获和沟通导致{\ IT磁性限制的风冲}（MCWS），前冲程流速是风端速度的一定程度，可能是几千公里S $^{ - 1} $。这些冲击产生热等离子体，X射线源。在过去的十年中，发生了一些发展，特别是使用\ xmm \ and \ ch的大量物体确定热等离子体特性，以及完全自洽的MHD建模以及在弱风中识别冲击效应的鉴定。此外，这些对象通常是H $α$排放的来源，它由足够高的质量损失率或离心分解控制。在这里，我们回顾了这种磁性巨大恒星风力动力学的理论方面。
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.
