Super-Eddington accretion of dusty gas onto seed black holes: metallicity-dependent efficiency of mass growth

Understand

The super-Eddington accretion onto intermediate seed BHs is a potential formation mode of supermassive black holes exceeding $10^9~M_\odot$ in the early universe.

• We here investigate how such rapid accretion may occur with finite amounts of heavy elements contained in the gas and dust.
• In our 1D radiation-hydrodynamics simulations, the radiative transfer is solved for both the direct UV lights emitted by an accretion disk and the diffuse IR lights thermally emitted by dust grains.
• Our results show that the radiative force by the IR lights causes a strong feedback to regulate the mass accretion.