Numerical Simulations of Optically Thick Accretion onto a Black Hole - I. Spherical Case

Understand

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.