Models of accretion disk coronae in high luminosity systems

We present results from a potentially powerful new method for modeling two‐dimensional radiative transfers in anisotropic systems. The method is highly efficient, allowing inclusion of radiative attenuation in dynamical simulations. Comparisons are made with a detailed radiative transfer code. As a first application, we compute self‐consistent models of Compton‐heated coronae in systems with luminosities up to 0.6 LEdd. Lower luminosity models are used to compare with the results of earlier work.We present results from a potentially powerful new method for modeling two‐dimensional radiative transfers in anisotropic systems. The method is highly efficient, allowing inclusion of radiative attenuation in dynamical simulations. Comparisons are made with a detailed radiative transfer code. As a first application, we compute self‐consistent models of Compton‐heated coronae in systems with luminosities up to 0.6 LEdd. Lower luminosity models are used to compare with the results of earlier work.