Numerical Simulations of Rotating Accretion Flows near a Black Hole
Abstract
We present time-dependent solutions of thin, supersonic accretion flows near a black hole and compare them with analytical solutions. Such flows of inviscid, adiabatic gas are characterized by the specific angular momentum and the specific energy. We confirm that for a wide range of above parameters a stable standing shock wave with a vortex inside it forms close to the black hole. Apart from steady state solutions, we show the existence of non-steady solutions for thin accretion flows where the accretion shock is destroyed and re-generated periodically. The unstable behavior should be caused by dynamically induced instabilities, since inviscid, adiabatic gas is considered. We discuss possible relevance of the periodic behavior on quasi-periodic oscillations (QPOs) observed in galactic and extragalactic black hole candidates.
Cite
@article{arxiv.astro-ph/9702054,
title = {Numerical Simulations of Rotating Accretion Flows near a Black Hole},
author = {Dongsu Ryu and Sandip K. Chakrabarti},
journal= {arXiv preprint arXiv:astro-ph/9702054},
year = {2007}
}
Comments
6 pages with 3 figures, uses paspconf.sty, to appear in "Computational Astrophysics", the Proceedings of the 12th Kingston Meeting ed. D. Clarke & M. West, also available upon request to [email protected]