Feedback from supercritical disk accretion flows; Two-dimensional radiation-hydrodynamic simulations of stable and unstable disks with radiatively driven outflows

摘要

The supercritical disk accretion flow with radiatively driven outflows isstudied based on two-dimensional radiation-hydrodynamic simulations for a widerange of the mass input rate, $\dot{M}_{\rm input}$, which is the mass suppliedfrom the outer region to the disk per unit time. The $\alpha$-prescription isadopted for the viscosity. We employ $\alpha=0.5$, as well as $\alpha=0.1$ for$\dot{M}_{\rm input}\ge 3\times 10^2L_{\rm E}/c^2$ and only $\alpha=0.5$ for$\dot{M}_{\rm input}\le 10^2L_{\rm E}/c^2$, where $L_{\rm E}$ is the Eddingtonluminosity and $c$ is the speed of light. The quasi-steady disk and radiatelydriven outflows form in the case in which the mass input rate highly exceedsthe critical rate, $\dot{M}_{\rm input}>3\times 10^2 L_{\rm E}/c^2$. Then, thedisk luminosity as well as the kinetic energy output rate by the outflowexceeds the Eddington luminosity. The moderately supercritical disk,$\dot{M}_{\rm input}\sim 10-10^2 L_{\rm E}/c^2$, exhibits limit-cycleoscillations. The disk luminosity goes up and down across the Eddingtonluminosity, and the radiatively driven outflows intermittently appear. The timeaveraged mass, momentum, and kinetic energy output rates by the outflow as wellas the disk luminosity increase with increase of the mass input rate, $\propto\dot{M}_{\rm input}^{0.7-1.0}$ for $\alpha=0.5$ and $\propto \dot{M}_{\rminput}^{0.4-0.6}$ for $\alpha=0.1$. Our numerical simulations show that theradiatively driven outflow model for the correlation between black hole massand bulge velocity dispersion proposed by \citeauthor{SR98} and\citeauthor{King03} is successful if $\dot{M}_{\rm input}c^2/L_{\rm E} \sim$ afew 10 ($\alpha=0.5$) or $\gsim$ a few ($\alpha=0.1$).