To examine the structure and dynamics of thick accretion disks, we use a two-dimensional viscous hydrodynamic code coupled with radiation transport. The α-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 a 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 ≥ 5 × 10 -7 M⊙yr-1, and the formation of the X-ray iron emission lines.

• TORU OKUDA(Hakodate College, Hokkaido University of Education)