1999/02/18 by Igor V. Igumenshchev, I. V. Igumenshchev, Igumenshchev, Igor V.
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics (astro-ph) #FOS: Physical sciences #Fluid Dynamics and Turbulent Flows #Heat Transfer Mechanisms #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9902259
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
arxiv created 1999/02/18 · openalex publication_date 1999/02/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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 α. The high viscosity flows (α~1) are stable and have a strong equatorial inflow and bipolar outflows. The low viscosity flows (α<0.1) are convectively unstable and this induces quasi-periodic variability.