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How do massive black holes get their gas?

Hopkins, Philip F. and Quataert, Eliot (2010) How do massive black holes get their gas? Monthly Notices of the Royal Astronomical Society, 407 (3). pp. 1529-1564. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20200521-163330617

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Abstract

We use multiscale smoothed particle hydrodynamic simulations to study the inflow of gas from galactic scales (∼10 kpc) down to ≲ 0.1 pc, at which point the gas begins to resemble a traditional, Keplerian accretion disc. The key ingredients of the simulations are gas, stars, black holes (BHs), self-gravity, star formation and stellar feedback (via a subgrid model); BH feedback is not included. We use ∼100 simulations to survey a large parameter space of galaxy properties and subgrid models for the interstellar medium physics. We generate initial conditions for our simulations of galactic nuclei (≲ 300 pc) using galaxy-scale simulations, including both major galaxy mergers and isolated bar-(un)stable disc galaxies. For sufficiently gas-rich, disc-dominated systems, we find that a series of gravitational instabilities generates large accretion rates of up to ∼ 1–10 M_⊙ yr⁻¹ on to the BH (i.e. at ≲ 0.1 pc); this is comparable to what is needed to fuel the most luminous quasars. The BH accretion rate is highly time variable for a given set of conditions in the galaxy at ∼kpc. At radii of >rsim 10 pc, our simulations resemble the ‘bars-within-bars’ model of Shlosman et al., but we show that the gas can have a diverse array of morphologies, including spirals, rings, clumps and bars; the duty cycle of these features is modest, complicating attempts to correlate BH accretion with the morphology of gas in galactic nuclei. At ∼ 1–10 pc, the gravitational potential becomes dominated by the BH and bar-like modes are no longer present. However, we show that the gas can become unstable to a standing, eccentric disc or a single-armed spiral mode (m = 1), in which the stars and gas precess at different rates, driving the gas to sub-pc scales (again for sufficiently gas-rich, disc-dominated systems). A proper treatment of this mode requires including star formation and the self-gravity of both the stars and gas (which has not been the case in many previous calculations). Our simulations predict a correlation between the BH accretion rate and the star formation rate at different galactic radii. We find that nuclear star formation is more tightly coupled to active galactic nucleus activity than the global star formation rate of a galaxy, but a reasonable correlation remains even for the latter.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1111/j.1365-2966.2010.17064.xDOIArticle
https://arxiv.org/abs/0912.3257arXivDiscussion Paper
ORCID:
AuthorORCID
Hopkins, Philip F.0000-0003-3729-1684
Quataert, Eliot0000-0001-9185-5044
Additional Information:© 2010 The Authors. Journal compilation © 2010 RAS. Accepted 2010 May 18. Received 2010 May 17; in original form 2009 December 14. We thank Phil Chang, Lars Hernquist, Norm Murray and Volker Springel for helpful discussions during the development of this work and the referee for a careful reading of the text and a number of very useful suggestions. PFH and EQ were supported by the Miller Institute for Basic Research in Science, University of California Berkeley. EQ was also supported in part by NASA grant NNG06GI68G and the David and Lucile Packard Foundation.
Funders:
Funding AgencyGrant Number
Miller Institute for Basic Research in ScienceUNSPECIFIED
NASANNG06GI68G
David and Lucile Packard FoundationUNSPECIFIED
Subject Keywords:galaxies: active, galaxies: evolution, quasars: general, cosmology: theory
Issue or Number:3
Record Number:CaltechAUTHORS:20200521-163330617
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200521-163330617
Official Citation:Philip F. Hopkins, Eliot Quataert, How do massive black holes get their gas?, Monthly Notices of the Royal Astronomical Society, Volume 407, Issue 3, September 2010, Pages 1529–1564, https://doi.org/10.1111/j.1365-2966.2010.17064.x
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:103399
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:22 May 2020 18:42
Last Modified:22 May 2020 18:42

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