ABSTRACT
We perform two-dimensional radiation hydrodynamical simulations of accretion flows on to black holes (BHs) at the nuclei of protogalaxies, and study the impact of mechanical and radiative feedback on rapid growth of BHs. The outflows deposit mass, momentum, and energy into the surrounding medium and prevent mass accretion on to the BH, resulting in the reduction of radiative output. We find that when the BH is embedded in a dense gas core, ionizing radiation attenuated by inefficient BH feeding owing to mechanical feedback hardly affects the gas dynamics at the BH gravitational sphere of influence, from which intense inflows of neutral gas occur at rates substantially exceeding the Eddington limit without impeded by photoionization and heating. Since mechanical power of outflows driven by the rapidly accreting BH is sufficiently strong, bipolar outflows completely evacuate the surrounding gas in the polar region but mass inflows through the equatorial region maintain the BH accretion rate as high as $\sim 300\!-\!10^3~\dot{M}_{\rm Edd}$, which is reduced by one order of magnitude from those with radiative feedback alone. Furthermore, we find that the critical gas density required for rapid accretion is lower by a factor of ∼3, when mechanical feedback is considered. By studying the dependence on outflow parameters (e.g. opening angle, mass loading degree into outflows, velocity), we conclude that contrary to naive expectation, the stronger outflow leads to the transition to rapid accretion more efficiently. Rapidly growing BHs inject mechanical power with $\sim 0.1\!-\!1{{\ \rm per\ cent}}$ of the radiative luminosity into their host galaxy scales, which is used for cosmological simulations.
Merger criteria of multiple massive black holes and the impact on the host galaxy