  Modeling the radiation generated by accreting matter is an important step
towards realistic simulations of black hole accretion disks, especially at high
accretion rates. To this end, we have recently added radiation transport to the
existing general relativistic magnetohydrodynamic code, Cosmos++. However,
before attempting to model radiative accretion disks, we have tested the new
code using a series of shock tube and Bondi (spherical inflow) problems. The
four radiative shock tube tests, first presented by Farris et al. (2008), have
known analytic solutions, allowing us to calculate errors and convergence rates
for our code. The Bondi problem only has an analytic solution when radiative
processes are ignored, but is pertinent because it is closer to the physics we
ultimately want to study. In our simulations, we include Thomson scattering and
thermal bremsstrahlung in the opacity, focusing exclusively on the
super-Eddington regime. Unlike accretion onto bodies with solid surfaces,
super-Eddington accretion onto black holes does not produce super-Eddington
luminosity. In our examples, despite accreting at up to 300 times the Eddington
rate, our measured luminosity is always several orders of magnitude below
Eddington.
