This project focuses on the development of modeling techniques for the determination of radiation fields, temperatures and ionization properties for non-spherical stellar atmospheres and circumstellar envelopes. Such models are critically needed to interpret a wide variety of new high spatial and spectral resolution observations that are now available for such objects as Wolf-Rayet stars, Herbig-Haro Ae/Be stars, O- and B-type stars, and evolving asymptotic giant branch stars. In addition, the product of this research is likely to be useful in interpreting the observational properties of objects that have experienced explosive eruptions, like supernovae. The initial effort will employ a Monte Carlo (statistical) approach to approximating the radiative transfer calculations of non-equilibrium axisymmetric and 'clumpy' atmospheres. The new work builds upon a previously developed two-dimensional axisymmetric model of winds from rapidly rotating hot stars, the so-called "wind-compressed disk model."
