| Title | Long-term Evolution of Supercritical Black Hole Accretion with Outflows: A Subgrid Feedback Model for Cosmological Simulations |
| Authors | Hu, Haojie Inayoshi, Kohei Haiman, Zoltan Quataert, Eliot Kuiper, Rolf |
| Affiliation | Peking Univ, Kavli Inst Astron & Astrophys, 5 Yiheyuan Rd, Beijing 100871, Peoples R China Peking Univ, Sch Phys, Dept Astron, 5 Yiheyuan Rd, Beijing 100871, Peoples R China Columbia Univ, Dept Astron, New York, NY 10027 USA Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany |
| Keywords | DARK-MATTER HALOES HIGH-Z EXPLORATION SLIM-DISK MODEL EDDINGTON ACCRETION GALAXY FORMATION AGN DISCS FLOWS REDSHIFT QUASARS STAR |
| Issue Date | 1-Aug-2022 |
| Publisher | ASTROPHYSICAL JOURNAL |
| Abstract | We study the long-term evolution of the global structure of axisymmetric accretion flows onto a black hole (BH) at rates substantially higher than the Eddington value ((sic)(Edd)), performing 2D hydrodynamical simulations with and without radiative diffusion. In the high-accretion optically thick limit, where the radiation energy is efficiently trapped within the inflow, the accretion flow becomes adiabatic and comprises turbulent gas in the equatorial region and strong bipolar outflows. As a result, the mass inflow rate decreases toward the center as (sic)(in) proportional to r(p) with p similar to 0.5-0.7 and a small fraction of the inflowing gas feeds the nuclear BH. Thus, super-Eddington accretion is sustained only when a larger amount of gas is supplied from larger radii at greater than or similar to 100-1000 (sic)(Edd). The global structure of the flow settles down to a quasi-steady state in millions of the orbital timescale at the BH event horizon, which is greater than or similar to 10-100 times longer than that addressed in previous (magneto-)RHD simulation studies. Energy transport via radiative diffusion accelerates the outflow near the poles in the inner region but does not change the overall properties of the accretion flow compared to the cases without diffusion. Based on our simulation results, we provide a mechanical feedback model for super-Eddington accreting BHs. This can be applied as a subgrid model in large-scale cosmological simulations that do not sufficiently resolve galactic nuclei, and to the formation of the heaviest gravitational-wave sources via accretion in dense environments. |
| URI | http://hdl.handle.net/20.500.11897/650034 |
| ISSN | 0004-637X |
| DOI | 10.3847/1538-4357/ac75d8 |
| Indexed | SCI(E) |
| Appears in Collections: | 科维理天文与天体物理研究所 物理学院 |
