Numerical models of rotating accretion flows around black holes

Igor V. Igumenshchev

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Numerical models of rotating accretion flows around black holes

Igor V. Igumenshchev

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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 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.

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Igor V. Igumenshchev. 1999-02-18. Numerical models of rotating accretion flows around black holes. https://arxiv.org/abs/astro-ph/9902259

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