Numerical models of rotating accretion flows around black holes
Astrophysics
2009-09-25 v1
Abstract
Numerical, two-dimensional, time-dependent hydrodynamical models of geometrically thick accretion discs around black holes are presented. Accretion flows with non-effective radiation cooling (ADAFs) can be both convectively stable or unstable depending on the value of the viscosity parameter \alpha. The high viscosity flows (\alpha~1) are stable and have a strong equatorial inflow and bipolar outflows. The low viscosity flows (\alpha<0.1) are convectively unstable and this induces quasi-periodic variability.
Keywords
Cite
@article{arxiv.astro-ph/9902259,
title = {Numerical models of rotating accretion flows around black holes},
author = {Igor V. Igumenshchev},
journal= {arXiv preprint arXiv:astro-ph/9902259},
year = {2009}
}
Comments
6 pages, 2 figures, presented at the workshop "High Energy Processes in Accreting Black Holes", 1998, eds. J. Poutanen & R. Svensson, ASP Conf. Series, Vol. 161