Radiation Hydrodynamics of 2-D Accretion Disks

Details Radiation Hydrodynamics of 2-D Accretion Disks Radiation Hydrodynamics of 2-D Accretion Disks

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001jkas...34..251o&link_type=abstract

Journal of the Korean Astronomical Society, vol. 34, no. 4, pp. 251-254

Astronomy and Astrophysics

Astronomy

Accretion Disks, Hydrodynamics, Radiation, X-Ray Source: Individual (Ss 433)

Scientific paper

To examine the structure and dynamics of thick accretion disks, we use a two-dimensional viscous hydrodynamic code coupled with radiation transport. The alpha-model and the full viscous stress-tensor description for the kinematic viscosity are used. The radiation transport is treated in the gray, flux-limited diffusion approximation. The finite difference methods used are based on an explicit-implicit method. We apply the numerical code to the Super-Eddington black-hole model for SS 433. The result for a very small viscosity parameter alpha reproduces well the characteristic features of SS 433, such as the relativistic jets with ~ 0.26c, the small collimation degree of the jets, the mass-outflow rate of >= 5e-7 Msun/yr, and the formation of the X-ray iron emission lines.

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