Numerical Simulations of Optically Thick Accretion Onto a Black Hole. Ii. Rotating Flow

In this paper, we report on recent upgrades to our general relativistic radiation magnetohydrodynamics code, Cosmos++ , including the development of a new primitive inversion scheme and a hybrid implicit–explicit solver with a more general M 1 closure relation for the radiation equations. The new hybrid solver helps stabilize the treatment of the radiation source terms, while the new closure allows for a much broader range of optical depths to be considered. These changes allow us to expand by orders of magnitude the range of temperatures, opacities, and mass accretion rates, and move a step closer toward our goal of performing global simulations of radiation-pressure-dominated black hole accretion disks. In this work, we test and validate the new method against an array of problems. We also demonstrate its ability to handle super-Eddington, quasi-spherical accretion. Even with just a single proof-of-principle simulation, we already see tantalizing hints of the interesting phenomenology associated with the coupling of radiation and gas in super-Eddington accretion flows.