热磁转子星周围的原盘
Protodiscs around Hot Magnetic Rotator Stars
摘要：
我们开发的方程，并获得解决方案的结构和演化的原盘区域，最初形成的没有径向运动和超开普勒旋转速度时，风材料从一个热的旋转恒星被引导向其赤道面的偶极型磁场。它的温度约为$10^7$ K，这是因为激波加热和风物质的流入导致其赤道密度随时间增加。离心力和热压力相对于磁力增加，并且材料在其外边缘处逃逸。匀速旋转恒星的原盘区域几乎是匀速旋转的，除非有不稳定性介入，否则会径向收缩。在一颗角速度沿其表面向赤道方向增加的恒星中，原盘区域的角速度径向向外减小，磁旋转不稳定性（MRI）可以在几小时或几天内发生。MRI产生的粘度将重新调整原椎间盘材料的角速度分布，并可能有助于形成准稳定的椎间盘。因此，在均匀旋转恒星的数值模拟中发现的离心爆发并不意味着具有缓慢流出的准稳定盘不能在具有太阳型差异旋转的磁转子恒星周围形成。
英文摘要：
We develop equations and obtain solutions for the structure and evolution of a protodisc region that is initially formed with no radial motion and super-Keplerian rotation speed when wind material from a hot rotating star is channelled towards its equatorial plane by a dipole-type magnetic field. Its temperature is around $10^7$K because of shock heating and the inflow of wind material causes its equatorial density to increase with time. The centrifugal force and thermal pressure increase relative to the magnetic force and material escapes at its outer edge. The protodisc region of a uniformly rotating star has almost uniform rotation and will shrink radially unless some instability intervenes. In a star with angular velocity increasing along its surface towards the equator, the angular velocity of the protodisc region decreases radially outwards and magnetorotational instability (MRI) can occur within a few hours or days. Viscosity resulting from MRI will readjust the angular velocity distribution of the protodisc material and may assist in the formation of a quasi-steady disc. Thus, the centrifugal breakout found in numerical simulations for uniformly rotating stars does not imply that quasi-steady discs with slow outflow cannot form around magnetic rotator stars with solar-type differential rotation.
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