Bulge-driven fueling of seed black holes

Journal Article · Sat Feb 20 04:00:00 EST 2016 · Astrophysical Journal

DOI:https://doi.org/10.3847/0004-637X/818/2/184· OSTI ID:22887013

Park, KwangHo; Bogdanović, Tamara; Wise, John H. ^[1]; Ricotti, Massimo ^[2]; Natarajan, Priyamvada ^[3]

---

1. Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, Atlanta, GA 30332 (United States)
2. Department of Astronomy, University of Maryland, College Park, MD 20740 (United States)
3. Department of Astronomy, Yale University, New Haven, CT 06520 (United States)

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 T{sub ∞}=10{sup 4} K. We find that the accretion rate of BHs embedded in bulges is proportional to r{sub B,eff}/r{sub B}, where r{sub B,eff} is the increased effective Bondi radius that includes the gravitational potential of the bulge, and r{sub 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{sub bulge} is greater than the critical value of ∼10{sup 6} M{sub ☉} and is proportional to r{sub B,eff}/r{sub B}≃M{sub bulge}/M{sub BH}, where M{sub BH} is the BH mass. Since the critical bulge mass is independent of the central BH mass, the growth rate of BHs with masses M{sub BH}=10{sup 2}, 10{sup 4}, and 10{sup 6} M{sub ☉} exhibits distinct dependencies on the bulge-to-BH mass ratio. Our results imply that light seed BHs (≲10{sup 2} M{sub ☉}), 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{sup 5} M{sub ☉}), 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{sub BH}–σ relationship.

• OSTI ID: 22887013
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 818; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United Kingdom
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ACCRETION DISKS
BLACK HOLES
COMPUTERIZED SIMULATION
CRITICAL MASS
GALACTIC EVOLUTION
GALAXIES
HYDRODYNAMICS
ONE-DIMENSIONAL CALCULATIONS
PARTICLE TRACKS
RADIANT HEAT TRANSFER
STARS
SYMMETRY
UNIVERSE