SYNTHESIS OF LINE-PROFILES FROM MODELS OF STRUCTURED WINDS

On the basis of a a careful analysis of resonance line formation (both for singlets and doublets) in structured winds, present time dependen t models of the line driven winds of hot stars (Owocki et al., this vo lume; Feldmeier, this volume) are shown to be able to explain a number of observational features with respect to variability and structure: they are (in principle) able to reproduce the black and broad troughs (without any artificial ''turbulence velocity'') and the ''blue edge v ariability'' observed in saturated resonance lines; they might explain the ''long lived narrow absorption components'' often observed in uns aturated lines Fit high velocities; they predict a relation between th e ''edge velocity'' of UV-lines and the radiation temperature of the o bserved X-ray emission. As a first example of the extent to which theo retical models can be constrained by comparisons between observations and profiles calculated by spectrum synthesis from structured winds, w e show here that models with deep-seated onset of structure formation (greater than or similar to 1.1R) produce resonance lines which agree qualitatively with observational findings; in contrast, the here pres ented models with structure formation only well out in the wind (great er than or similar to 1.6R) fail in this respect.