类星体辐射下旋转吸积流的动力学
Dynamics of Rotating Accretion Flows Irradiated by a Quasar
摘要：
本文研究了在超大质量黑洞引力和黑洞周围的吸积盘辐射影响下的轴对称、含时旋转流的流体动力学。这项工作是由Proga提出的早期工作的延伸，其中研究了非旋转流。在这里，我们考虑旋转的影响，一个位置依赖的辐射温度，在大半径的密度，和均匀的X射线背景辐射。与非旋转情况一样，旋转流形成具有两个分量的构型：（1）赤道流入和（2）双极流入/流出，流出沿极点离开系统。然而，随着旋转，流动并不总是达到稳定状态。此外，旋转减小了流出准直以及质量和动能的向外通量。此外，旋转增加了热能的向外通量，并可导致流出的碎片化和时间可变性。我们还表明，位置相关的辐射温度可以显着改变流动的解决方案。特别地，赤道区域中的流入可以由热驱动的流出代替。一般来说，正如过去所讨论和显示的那样，我们发现自洽地确定的类星体辐射的预热/冷却可以显着降低中央BH被馈送物质的速率。然而，我们的结果也强调了一点值得赞赏的功能。也就是说，类星体辐射驱动着一种非球形的、多温度的、非常动态的流动。这些效应在超过爱丁顿光度的0.01的光度下成为主导。
英文摘要：
We study the axisymmetric, time-dependent hydrodynamics of rotating flows that are under the influence of supermassive black hole gravity and radiation from an accretion disk surrounding the black hole. This work is an extension of the earlier work presented by Proga, where nonrotating flows were studied. Here, we consider effects of rotation, a position-dependent radiation temperature, density at large radii, and uniform X-ray background radiation. As in the non-rotating case, the rotating flow settles into a configuration with two components (1) an equatorial inflow and (2) a bipolar inflow/outflow with the outflow leaving the system along the pole. However, with rotation the flow does not always reach a steady state. In addition, rotation reduces the outflow collimation and the outward flux of mass and kinetic energy. Moreover rotation increases the outward flux of the thermal energy and can lead to fragmentation and time-variability of the outflow. We also show that a position-dependent radiation temperature can significantly change the flow solution. In particular, the inflow in the equatorial region can be replaced by a thermally driven outflow. Generally, as it have been discussed and shown in the past, we find that self-consistently determined preheating/cooling from the quasar radiation can significantly reduce the rate at which the central BH is fed with matter. However, our results emphasize also a little appreciated feature. Namely, quasar radiation drives a non-spherical, multi-temperature and very dynamic flow. These effects become dominant for luminosities in excess of 0.01 of the Eddington luminosity.
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