Dynamics of the Transition from a Thin Accretion Disk to an Advection-dominated Accretion Flow

Details Dynamics of the Transition from a Thin Accretion Disk to an Advection-dominated Accretion Flow Dynamics of the Transition from a Thin Accretion Disk to an Advection-dominated Accretion Flow

Jan 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...529..127m&link_type=abstract

The Astrophysical Journal, Volume 529, Issue 1, pp. 127-137.

Physics

32

Accretion, Accretion Disks, Black Hole Physics, Hydrodynamics, Turbulence

Scientific paper

We consider an optically thin advection-dominated accretion flow (ADAF) that is connected at a finite transition radius to an outer optically thick, geometrically thin disk. We include turbulent energy transport and examine ADAF models that satisfy the following boundary conditions at the transition radius: (1) the temperature of the gas is much lower than the virial temperature, (2) the rotation is super-Keplerian, and (3) the net radial flux of energy is outward. We numerically solve the height-integrated viscous hydrodynamic equations with these boundary conditions. We find that the Bernoulli parameter is positive for a wide range of radius, indicating that outflows may be possible from ADAFs. Turbulent energy transport enhances the Bernoulli parameter. We compare our numerical global solutions with two published analytical solutions. We find that the solution of Honma represents the transition region well, while the self-similar solution of Narayan & Yi works better away from the transition. However, neither analytical solution is able to represent the density or angular momentum profile in the inner region of the ADAF, where the flow makes a sonic transition.

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