Spectral Modeling of X-rays from Hot Star Winds

We attempt to determine the mass-loss rates of several O stars using x-ray spectra from Chandra’s archive. Models of x-ray production in hot star winds predict broad, asymmetric emission lines, but observed lines tend to be much more symmetric. Such symmetry can be explained by either lowering the values of the mass-loss rate for these winds, or by reassessing the commonly accepted models of x-ray production. Previous explorations of the trade-offs of these two options have been largely qualitative in nature. In our research, we thus seek to quantify the amount of asymmetry present in the data and to find the reductions in mass-loss rate values needed to explain the data.