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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Relativistic radiation hydrodynamical accretion-disk winds
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Relativistic radiation hydrodynamical accretion-disk winds

机译：相对论辐射流体动力吸积盘风

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摘要

Accretion-disk winds blowing off perpendicular to a luminous disk are examined within the framework of fully special relativistic radiation hydrodynamics. The wind is assumed to be steady, vertical, and isothermal. Using a velocity-dependent variable Eddington factor, we can solve the rigorous equations of relativistic radiative hydrodynamics, and can obtain radiatively driven winds accelerated up to relativistic speeds. For less-luminous cases, disk winds are transonic types passing through saddle-type critical points, and the final speeds of the winds increase as the disk flux and/or the isothermal sound speed increase. For luminous cases, on the other hand, disk winds are always supersonic, since the critical points disappear due to the characteristic nature of the disk gravitational fields. The boundary between the transonic and supersonic types is located at around F-c similar to 0.6 (epsilon + p)/(rho c(2))/gamma(c), where, is the radiative flux at the critical point normalized by the local Eddington luminosity, (epsilon + p)/(rho c(2)) is the enthalpy of the gas divided by the rest-mass energy, and gamma(c) is the Lorentz factor of the wind velocity at the critical point. In transonic winds, the final speed becomes 0.4-0.8c for typical parameters, while it can reach similar to c in supersonic winds.
机译：在完全相对论的辐射流体动力学框架内研究了垂直于发光盘的吸积盘风。假定风为稳定，垂直和等温。使用速度相关的可变爱丁顿因子，我们可以求解相对论的辐射流体动力学的严格方程，并可以获得加速到相对论速度的辐射驱动风。对于较少发光的情况，圆盘风是跨鞍型临界点的跨音速类型，并且风的最终速度随着圆盘通量和/或等温声速的增加而增加。另一方面，对于发光的情况，圆盘风总是超音速的，因为临界点由于圆盘重力场的特征而消失了。跨音速和超音速类型之间的边界位于Fc附近，类似于0.6（ε+ p）/（rho c（2））/γ（c），其中，是通过局部爱丁顿归一化的临界点处的辐射通量发光度（ε+ p）/（rho c（2））是气体的焓除以静止质量能，而γ（c）是临界点处风速的洛伦兹因子。在跨音速风中，典型参数的最终速度变为0.4-0.8c，而在超音速风中其最终速度可达到c。

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