Synthesis of Line Profiles from Models of Structured Winds
Abstract
On the basis of a a careful analysis of resonance line formation (both for singlets and doublets) in structured winds, presenttime dependent models of the line driven winds of hot stars (Owocki et al., this volume; 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 theblack andbroad troughs (without any artificial “turbulence velocity”) and the “blue edge variability” observed in saturated resonance lines; they might explain the “long lived narrow absorption components” often observed in unsaturated lines at high velocities; they predict a relation between the “edge velocity” of UV-lines and the radiation temperature of the observed X-ray emission. As a first example of the extent to which theoretical models can be constrained by comparisons between observations and profiles calculated by spectrum synthesis from structured winds, we show here that models with deep-seated onset of structure formation (≳ 1.1R * ) produce resonance lines which agreequalitatively with observational findings; in contrast, the here presented models with structure formation only well out in the wind (≳ 1.6R * ) fail in this respect.
- Publication:
-
Astrophysics and Space Science
- Pub Date:
- November 1994
- DOI:
- 10.1007/BF01091171
- Bibcode:
- 1994Ap&SS.221..409P
- Keywords:
-
- Computational Astrophysics;
- Hot Stars;
- Line Spectra;
- Resonance Lines;
- Shock Waves;
- Stellar Atmospheres;
- Stellar Mass;
- Stellar Models;
- Stellar Physics;
- Stellar Structure;
- Stellar Winds;
- Time Dependence;
- Variability;
- Mass Distribution;
- Stellar Temperature;
- Ultraviolet Radiation;
- X Ray Spectra;
- Astrophysics;
- Line: formation;
- Stars: atmospheres;
- Stars: early type;
- Stars: mass-loss