Radiation hydrodynamic calculation of super-Eddington accretion disks

Abstract

We report the results of nonrelativistic radiation-hydrodynamic calculations of axisymmetric supercritical accretion disks around Newtonian quasi-black holes. Anisotropic and isotropic constant kinematic viscosity models are used, with radiation transport described by a gray Thomson scattering opacity and flux-limited diffusion. The resulting solutions have four distinct zones: (1) Centered on the disk midplane is a thick, dense region of turbulent convection. (2) Above this is an accretion zone in which low angular momentum matter rapidly flows onto the black hole. (3) The accretion zone is bounded by a photocone, in which the matter becomes optically thin. (4) Inside the photocone, surrounding the angular momentum axis, is a broad subrelativistic jet of expelled matter. We discuss applications of these results to SS 433 and to extragalactic jets.