Structures around supermassive black holes and their evolution - feedback and feeding

我们从理论上研究了星系中超大质量黑洞周围的ISM的结构和动力学。通过三维辐射流体动力学模拟，我们证实了由于辐射压力和加热而产生的非稳定和非均匀流出。这种外流并不能阻止物质向银河系中心聚集。我们还发现，一部分失败的流出物自然形成一个模糊的环面，这被认为可以解释观测到的agn特性。辐射驱动的外流在很大的动态范围内无处不在，例如，我们发现强烈的线驱动风是由吸积盘形成的，这一致地解释了宽吸收线类星体。

We have theoretically investigated structures and dynamics of the ISM around supermassive black holes in galaxies. Using three-dimensional radiation-hydrodynamics simulations, we confirmed that non-steady and non-uniform outflows are generated due to the radiation pressure and heating. This outflow does not prevent from accreting materials toward the galactic center. We also found that a part of failed outflows naturally form an obscuring torus, which has been postulated to explain observed properties of AGNs. The radiation-driven outflows are ubiquitous over a large dynamic range, for example, we found that strong line-driven winds are formed from the accretion disk, and this consistently explains broad-absorption line quasars.