2015/12/10 by Kwangho Park, KwangHo Park, Massimo Ricotti +4 · 3 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Bulge #Galaxies: Formation, Evolution, Phenomena #Materials science #Physics #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.3847/0004-637x/818/2/184
10 pages, 10 Figures, 1 Table, submitted to ApJ
arxiv created 2015/12/10 · openalex publication_date 2016/02/18 · arxiv updated 2016/03/09 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
ABSTRACT We examine radiation-regulated accretion onto intermediate-mass and massive black holes (BHs) embedded in a bulge component. Using spherically symmetric one-dimensional radiation-hydrodynamics simulations, we track the growth of BHs accreting from a cold, neutral gas reservoir with temperature K. We find that the accretion rate of BHs embedded in bulges is proportional to , where r B,eff is the increased effective Bondi radius that includes the gravitational potential of the bulge, and r B is the Bondi radius of the BH. The radiative feedback from the BH suppresses the cold accretion rate to ∼1% of the Bondi rate when a bulge is not considered. However, we find that the BH fueling rate increases rapidly when the bulge mass M bulge is greater than the critical value of ∼10 6 M ☉ and is proportional to , where is the BH mass. Since the critical bulge mass is independent of the central BH mass, the growth rate of BHs with masses , 10 4 , and 10 6 M ☉ exhibits distinct dependencies on the bulge-to-BH mass ratio. Our results imply that light seed BHs (≲10 2 M ☉ ), which might be the remnants of the Pop III stars, cannot grow through accretion coevally with the early assembly of the bulge of the host galaxies until the bulge reaches the critical mass. However, massive BH seeds (≳10 5 M ☉ ), which may form via direct collapse, are more likely to be embedded in a supercritical bulge, and thus can grow efficiently coupling to the host galaxies and driving the early evolution of the M BH – σ relationship.