论文标题
具有辐射驱动流出的超临界积聚磁盘
A supercritical accretion disk with radiation-driven outflows
论文作者
论文摘要
如果黑洞（BH）重力的垂直分量无法抵抗辐射力，则流出不可避免地会从磁盘上驱动。我们通过求解磁盘中垂直气体运动的动态方程来得出流出中流出的质量损失率。用径向能量对流计算超临界磁盘的结构。我们发现，如果磁盘以中等的埃德丁顿（Eddington）标准速率（最高$ \ sim 100 $）吸收，即在其外边缘的中等速度（即，仅BH只有一小部分的气体）在几个Eddington的高高率左右散发出来，则大多数流入气体都会流出流出。 （$ \ dot {m} \ equiv \ dot {m}/\ dot {m} _ {\ rm edd} \ sim 1000 $）。与正常的细盘相比，由于流出的质量损失，磁盘光度受到了大大抑制。我们将模型应用于潮汐破坏事件（TDES）的光线曲线，并发现磁盘光度随时间而下降也很慢，即使典型的积聚率$ \ dot {m} \ propto {m} \ propto t^{ - 5/3} $在磁盘的外边缘进行了有效的范围，并在磁盘的外边缘进行了范围，并在磁盘的外部有帮助，并在某些情况下限制了一些柔和的现象。在TDES中。超临界磁盘的强大外流围绕超质量BHS的超急诊磁盘可能会在其宿主星系上扮演至关重要的角色，这可以在机械反馈模型中作为成分。还讨论了结果对晚餐BHS生长的含义。
Outflows are inevitably driven from the disk if the vertical component of the black hole (BH) gravity cannot resist the radiation force. We derive the mass loss rate in the outflows by solving a dynamical equation for the vertical gas motion in the disk. The structure of a supercritical accretion disk is calculated with the radial energy advection included. We find that most inflowing gas is driven into outflows if the disk is accreting at a moderate Eddington-scaled rate (up to $\sim 100$) at its outer edge, i.e., only a small fraction of gas is accreted by the BH, which is radiating at several Eddington luminosities, while it reaches around ten for extremely high accretion rate cases ($\dot{m}\equiv\dot{M}/\dot{M}_{\rm Edd}\sim 1000$). Compared with a normal slim disk, the disk luminosity is substantially suppressed due to the mass loss in the outflows. We apply the model to the light curves of the tidal disruption events (TDEs), and find that the disk luminosity declines very slowly with time even if a typical accretion rate $\dot{m}\propto t^{-5/3}$ is assumed at the outer edge of the disk, which is qualitatively consistent with the observed light curves in some TDEs, and helps understanding the energy deficient phenomenon observed in the TDEs. Strong outflows from supercritical accretion disks surrounding super massive BHs may play crucial roles on their host galaxies, which can be taken as an ingredient in the mechanical feedback models. The implications of the results on the growth of supper-massive BHs are also discussed.
