Cookies

We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.


Durham Research Online
You are in:

The impact of angular momentum on black hole accretion rates in simulations of galaxy formation.

Rosas-Guevara, Y. M. and Bower, R. G. and Schaye, J. and Furlong, M. and Frenk, C. S. and Booth, C. M. and Crain, R. A. and Dalla Vecchia, C. and Schaller, M. and Theuns, T. (2015) 'The impact of angular momentum on black hole accretion rates in simulations of galaxy formation.', Monthly notices of the Royal Astronomical Society., 454 (1). pp. 1038-1057.

Abstract

Feedback from energy liberated by gas accretion on to black holes (BHs) is an attractive mechanism to explain the exponential cut-off at the massive end of the galaxy stellar mass function. Most previous implementations of BH accretion in hydrodynamical simulations of galaxy formation have assumed that BHs grow at an accretion rate that is proportion to the Bondi rate. A major concern is that the Bondi accretion rate is inappropriate when the accreting material has significant angular momentum. We present an improved accretion model that takes into account the circularization and subsequent viscous transport of infalling material, and implemented as a ‘subgrid’ model in hydrodynamic simulations. The resulting accretion rates are generally low in low mass (≲ 1011.5 M⊙) haloes, but show outbursts of Eddington-limited accretion during galaxy mergers. During outbursts these objects strongly resemble quasars. In higher mass haloes, gas accretion peaks at ∼10 per cent of the Eddington rate, which is thought to be conducive to the formation of radio jets. The resulting accretion rate depends strongly on the effective pressure of the gas surrounding the BH, which in turn depends strongly on halo mass. This induces a sharp transition in the importance of BH feedback. In small haloes, the growth of galaxies is regulated by star formation and supernova feedback, but above a halo mass of 1011.5 M⊙, rapid BH growth leads to the suppression of star formation and reduced growth of stellar mass with increasing halo mass.

Item Type:Article
Keywords:Black hole physics, Methods: numerical, Galaxies: active, Galaxies: evolution, Galaxies: formation, Quasars: general.
Full text:(VoR) Version of Record
Download PDF
(4705Kb)
Status:Peer-reviewed
Publisher Web site:http://dx.doi.org/10.1093/mnras/stv2056
Publisher statement:This article has been accepted for publication in Monthly notices of the Royal Astronomical Society ©: 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Date accepted:02 September 2015
Date deposited:19 February 2016
Date of first online publication:30 September 2015
Date first made open access:No date available

Save or Share this output

Export:
Export
Look up in GoogleScholar