Discovery of billion solar mass quasars at high redshift poses a challenge for modeling the initial seed black hole formation and subsequent growth history. Thus, radiation-hydrodynamic simulation for estimating growth rate of seed black holes in the range 10^2-10^5 solar mass is critical to test suggested scenarios. In this talk, I will discuss how gas accretion onto black holes is regulated by radiative feedback emphasizing the role of thermal and radiation pressure. Given the difficulty of seed black hole growth due to radiative feedback, I will present our most recent work where we show that stellar bulge component can enhance the gas accretion onto black holes when the bulge exceeds the critical mass of ~10^6 solar mass. Our results imply that heavy seed black holes (> 10^5 solar mass) that may form via direct collapse can grow efficiently coupling to the host galaxies whereas light seeds (< 10^2 solar mass) are not able to grow coevally with the host galaxies due to radiative feedback. I will also present Bondi-Hoyle type simulations with radiative feedback to show how dramatically radiative feedback changes the classical understanding of accretion onto black holes in supersonic motion.