Super-Eddington Mass Growth of Intermediate-mass Black Holes Embedded in Dusty Circumnuclear Disks

摘要: We perform the first three-dimensional radiation hydrodynamical simulations that investigate growth of intermediate-mass BHs (IMBHs) embedded in massive self-gravitating, dusty nuclear accretion disks. explore dependence mass efficiency on gas metallicity $Z$ and injection at super-Eddington rates from outer galactic disk $\dot{M}_{\rm in}$, find central BH can be fed exceeding Eddington rate only when becomes sufficiently optically thick to ionizing radiation. In this case, outflows owing photoevaporation is suppressed thus a large fraction ($\gtrsim 40\%$) feed BH. The conditions are expressed as in} > 2.2\times 10^{-1}~M_\odot ~{\rm yr}^{-1} (1+Z/10^{-2}~Z_\odot)^{-1}(c_{\rm s}/10~{\rm km~s}^{-1})$, where $c_{\rm s}$ sound speed gaseous disk. With increasing numerical resolution, vigorous fragmentation reduces surface density dynamical heating by formed clumps makes thickness higher. As result, photoevaorative mass-loss rises critical increases for fixed metallicity. This process enables until reaches $M_{\rm BH} \sim 10^{7-8}~M_\odot$, depending properties host dark-matter halo metal-enrichment history. assembly protogalaxies, seed form overdense regions with variance 3-4$\sigma$ $z\sim 15-20$ able undergo short periods their rapid transits into Eddington-limited phase afterwards supermassive observed $z>6-7$.