Abstract
Abstract We analyzed the X-ray emission-line profiles of three early-type stars ($\zeta$ Pup, $\delta$ Ori, and $\tau$ Sco) obtained with Chandra. A phenomenological model, where X-ray sources are distributing in wind above some lower limit radius, can fit the line profiles of $\zeta$ Pup and $\delta$ Ori; however, the fitting requires a much smaller absorption than expected from the mass-loss rate. This suggests that, if this phenomenological model represents the real X-ray emission region, there is substantial ionization or clumping of the stellar wind. The parameters derived from the line profile of $\tau$ Sco indicate that the X-ray-emitting plasma is concentrated on the stellar surface, suggesting the existence of a confined plasma on the stellar surface.
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