Numerical Simulations of Optically Thick Accretion onto a Black Hole. II. Rotating Flow
Aug 19, 201418 pages
Published in:
- Astrophys.J. 796 (2014) 1, 22
- Published: Oct 30, 2014
e-Print:
- 1408.4460 [astro-ph.IM]
Citations per year
Abstract: (IOP)
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.Note:
- 18 pages, 9 figures
- radiative transfer
- methods: numerical
- magnetohydrodynamics
- black hole physics
- accretion, accretion disks
References(30)
Figures(12)