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We present a uniform analysis of six examples of embedded wind shock (EWS) Ostar X-ray sources observed at high resolution with the Chandra gratingspectrometers. By modeling both the hot plasma emission and the continuumabsorption of the soft X-rays by the cool, partially ionized bulk of the windwe derive the temperature distribution of the shock-heated plasma and the windmass-loss rate of each star. We find a similar temperature distribution foreach star's hot wind plasma, consistent with a power-law differential emissionmeasure, $\frac{d\log EM}{d\log T}$, with a slope a little steeper than -2, upto temperatures of only about $10^7$ K. The wind mass-loss rates, which arederived from the broadband X-ray absorption signatures in the spectra, areconsistent with those found from other diagnostics. The most notable conclusionof this study is that wind absorption is a very important effect, especially atlonger wavelengths. More than 90 per cent of the X-rays between 18 and 25Angstrom units produced by shocks in the wind of $\zeta$ Puppis are absorbed,for example. It appears that the empirical trend of X-ray hardness withspectral subtype among O stars is primarily an absorption effect.

Chandra grating spectroscopy of embedded wind shock X-ray emission from O stars shows low plasma temperatures and significant wind absorption