We present a numerical method for simulating the radiation-hydrodynamic flow of material and neutrino radiation in the post-bounce epoch of a stellar core collapse. Current generation core collapse supernovae models must deal with convective fluid flows in regions of the collapsed core that are optically thick to neutrinos. Therefore the simulations must be multi-dimensional. Our method solves the equations of radiation hydrodynamics in the multigroup flux-limited diffusion (MGFLD) approximation in 2-D polar coordinates. The technique utilizes a staggered-mesh, explicit, Eulerian hydrodynamics scheme and a fully implicit, staggered-mesh scheme for the MGFLD integro-PDEs describing neutrino transport. We reveal the details of our numerical methods and present the results of validation tests of the code that are relevant to core collapse supernovae models.This research is funded under DOE HENP SciDAC Cooperative Agreement No. DE-FC02-01ER41185. Supercomputing support was provided by the National Energy Research Scientific Computing Center.
American Astronomical Society Meeting Abstracts
- Pub Date:
- December 2003