General relativistic radiation hydrodynamics of accretion flows: II. Treating stiff source terms and exploring physical limitations

TL;DR

This paper introduces an advanced numerical scheme for simulating general relativistic radiation hydrodynamics in accretion flows, demonstrating improved handling of stiff source terms and exploring physical effects like radiation pressure in black hole accretion.

Contribution

The authors implement an IMEX Runge-Kutta scheme into GR-hydrodynamics codes to better simulate optically thick radiation fields, enabling more accurate modeling of astrophysical accretion processes.

Findings

Radiation pressure significantly reduces accretion rates.

Luminosity approaches the Eddington limit in simulations.

Effective adiabatic index shifts towards 4/3 in radiation-dominated flows.

Abstract

We present the implementation of an implicit-explicit (IMEX) Runge-Kutta numerical scheme for general relativistic hydrodynamics coupled to an optically thick radiation field in two existing GR-hydrodynamics codes. We argue that the necessity of such an improvement arises naturally in astrophysically relevant regimes where the optical thickness is high as the equations become stiff. By performing several 1D tests we verify the codes' new ability to deal with this stiffness and show consistency. Then, still in 1D, we compute a luminosity versus accretion rate diagram for the setup of spherical accretion onto a Schwarzschild black hole and find good agreement with previous work. Lastly, we revisit the supersonic Bondi Hoyle Lyttleton (BHL) accretion in 2D where we can now present simulations of realistic temperatures, down to T~10^6 K. Here we find that radiation pressure plays an important role, but also that these highly dynamical set-ups push our approximate treatment towards the limit of physical applicability. The main features of radiation hydrodynamics BHL flows manifest as (i) an effective adiabatic index approaching gamma_effective ~ 4/3; (ii) accretion rates two orders of magnitude lower than without radiation pressure; (iii) luminosity estimates around the Eddington limit, hence with an overall radiative efficiency as small as eta ~ 10^{-2}; (iv) strong departures from thermal equilibrium in shocked regions; (v) no appearance of the flip-flop instability. We conclude that the current optically thick approximation to the radiation transfer does give physically substantial improvements over the pure hydro also in set-ups departing from equilibrium, and, once accompanied by an optically thin treatment, is likely to provide a fundamental tool for investigating accretion flows in a large variety of astrophysical systems.