Three-dimensional simulations of advective, sub-Keplerian accretion flow on to non-rotating black holes

Abstract

ABSTRACT We study the time evolution of sub-Keplerian transonic accretion flow on to a non-rotating black hole using a three-dimensional, inviscid hydrodynamics simulation code. Prior two-dimensional simulations show that centrifugal barrier in the accreting matter may temporarily halt the nearly free-falling matter and produce a stable, geometrically thick disc that may contain turbulent eddies. Our goal in this work is to investigate whether the disc develops any instability because of this turbulence when we dynamically activate all three dimensions. We find that the disc remains stable and axisymmetric even close to the central black hole. However, if we explicitly apply non-axisymmetric azimuthal perturbation, the axisymmetric structure of the disc is destroyed and instability is developed.