Numerical models of rotating accretion flows around black holes

Details Numerical models of rotating accretion flows around black holes Numerical models of rotating accretion flows around black holes

1999-02-18

arxiv.org/abs/astro-ph/9902259v1

Astronomy and Astrophysics

Astrophysics

6 pages, 2 figures, presented at the workshop "High Energy Processes in Accreting Black Holes", 1998, eds. J. Poutanen & R. Sv

Scientific paper

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.

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