[en] Analysis of thick, radiation pressure dominated (super-Eddington) accretion disks has proven to be difficult. Purely analytical methods have not yet been adequate to determine the structure of the disk and associated jet. The work presented here circumvents the analytical problems by using a numerical method; the results are based on a series of numerical simulations of disk accretion onto a three solar mass black hole. The computer code used in the analysis solves the coupled radiation gas dynamic equations for axisymmetric accretion onto a black hole. Newtonian mechanics is used, since relativistic corrections are essential only very near the black hole. The accretion is assumed to be driven by a macroscopic viscous stress tensor. The range of parameters used in the analysis was chosen to conform to expectations for a realistic disk. The conclusions are valid for disks in which the viscous stress magnitude is a significant fraction (∼1) of the disk pressure, and for accretion rate M ≤ 10 times from Eddington rate. Primary conclusions are presented