Rotating accretion flows around black holes: convection and variability

Details Rotating accretion flows around black holes: convection and variability Rotating accretion flows around black holes: convection and variability

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.303..309i&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 303, Issue 2, pp. 309-320.

Physics

121

Accretion, Accretion Discs, Black Hole Physics, Convection, Hydrodynamics, Instabilities, Methods: Numerical

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, with typical time-scales in the observed range of quasi-periodic oscillations.

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