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J. P. Aufdenberg (Arizona State University), P. H. Hauschildt (University of Georgia), E. Baron (University of Oklahoma)
We present preliminary atmospheric structures and synthetic spectra for hot luminous OB stars with winds. We use the latest version of our multi-purpose stellar atmosphere and radiative transfer code PHOENIX. In these steady-state expanding model atmospheres, we assume a beta-law velocity structure for the wind and solve the spherical co-moving frame radiative transfer equation with full non-LTE metal-line blanketing. In these models the solution of the radiation transfer equation treats both the static photosphere and the expanding wind components as a single structure. The temperature structure is solved for iteratively by satisfying energy conservation. These models provide predictions for the ionization structure within the wind and allow us to calculate synthetic spectra which include the extreme ultraviolet ionizing flux distribution and detailed line profiles. We acknowledge partial support from NASA and NSF grants to our respective institutions.
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