Thin accretion disks near the critical luminosity: the effect of turbulent energy transport

Details Thin accretion disks near the critical luminosity: the effect of turbulent energy transport Thin accretion disks near the critical luminosity: the effect of turbulent energy transport

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286..338h&link_type=abstract

Astronomy and Astrophysics 286, 338-343 (1994)

Astronomy and Astrophysics

Astrophysics

1

Accretion Disks, Galaxies: Active, Hydrodynamics, Turbulence

Scientific paper

The vertical structure of accretion disks around supermassive black holes is calculated with the inclusion of the turbulent heat flux parametrized by the Prandtl number Pr. It is shown that the structure of the innermost radiation pressure dominated region strongly depends on the value of Pr. In this region the efficiency of turbulent energy transport increases with increasing surface temperature. It is found that in the inner parts of the disk for values of Pr=~O(1) the turbulent heat flux carries up to nearly 100 % of the dissipated energy. While for large values of Pr density inversions occur, the density profiles are nearly Gaussian for values of Pr=~O(1). In some models an efficient turbulent energy transport leads to a considerable reduction of the disk thickness.

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