The Accretion Disc Particle Method for Simulations of Black Hole Feeding and Feedback

TL;DR

This paper introduces a new sub-grid model for black hole accretion in galaxy simulations that accounts for angular momentum, improving physical realism over traditional Bondi-Hoyle methods and impacting galaxy evolution predictions.

Contribution

The paper presents an accretion disc particle method that models black hole feeding considering angular momentum, offering a more self-consistent approach for galaxy formation simulations.

Findings

The new model is more physically self-consistent than Bondi-Hoyle.

It predicts an offset in the M_BH-sigma relation for rotationally supported systems.

Controlled experiments validate the model's effectiveness.

Abstract

Black holes grow by accreting matter from their surroundings. However, angular momentum provides an efficient natural barrier to accretion and so only the lowest angular momentum material will be available to feed the black holes. The standard sub-grid model for black hole accretion in galaxy formation simulations - based on the Bondi-Hoyle method - does not account for the angular momentum of accreting material, and so it is unclear how representative the black hole accretion rate estimated in this way is likely to be. In this paper we introduce a new sub-grid model for black hole accretion that naturally accounts for the angular momentum of accreting material. Both the black hole and its accretion disc are modelled as a composite accretion disc particle. Gas particles are captured by the accretion disc particle if and only if their orbits bring them within its accretion radius R_acc, at which point their mass is added to the accretion disc and feeds the black hole on a viscous timescale t_visc. The resulting black hole accretion rate (dM/dt)_BH powers the accretion luminosity L_acc ~ (dM/dt)_BH, which drives black hole feedback. Using a series of controlled numerical experiments, we demonstrate that our new accretion disc particle method is more physically self-consistent than the Bondi-Hoyle method. We also discuss the physical implications of the accretion disc particle method for systems with a high degree of rotational support, and we argue that the M_BH-sigma relation in these systems should be offset from the relation for classical bulges and ellipticals, as appears to be observed.