Numerical simulations of relativistic wind accretion on to black holes using Godunov-type methods

Simple item page
dc.creatorFont, Jose A.
dc.creatorIbanez, Jose M.
dc.creatorPapadopoulos, Philippos
dc.date1999-10-23
dc.date.accessioned2026-07-07T02:34:01Z
dc.date.available2026-07-07T02:34:01Z
dc.descriptionWe have studied numerically the so-called Bondi-Hoyle (wind) accretion on to a rotating (Kerr) black hole in general relativity. We have used the Kerr-Schild form of the Kerr metric, free of coordinate singularities at the black hole horizon. The `test-fluid' approximation has been adopted, assuming no dynamical evolution of the gravitational field. We have used a recent formulation of the general relativistic hydrodynamic equations which casts them into a first-order hyperbolic system of conservation laws. Our studies have been performed using a Godunov-type scheme based on Marquina's flux-formula. We find that regardless of the value of the black hole spin the final accretion pattern is always stable, leading to constant accretion rates of mass and momentum. The flow is characterized by a strong tail shock which is increasingly wrapped around the central black hole as the hole angular momentum increases. The rotation induced asymmetry in the pressure field implies that besides the well known drag, the black hole will experience also a lift normal to the flow direction.
dc.description6 pages, 2 figures, to appear in the proceedings of the conference "Godunov methods: theory and applications", Oxford, October 1999
dc.identifierhttps://arxiv.org/abs/astro-ph/9910433
dc.identifierhttp://arxiv.org/abs/astro-ph/9910433
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/15078
dc.subjectAstrophysics
dc.titleNumerical simulations of relativistic wind accretion on to black holes using Godunov-type methods
dc.typetext

Files

Collections

arXiv