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Astrophysics and Space Science

, Volume 221, Issue 1–2, pp 409–426 | Cite as

Synthesis of line profiles from models of structured winds

  • J. Puls
  • A. Feldmeier
  • U. W. E. Springmann
  • S. P. Owocki
  • A. W. Fullerton
Session 8 Hydrodynamical Simulations of the Evolution of Wind Structure

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.

Key words

Line: formation Stars: atmospheres Stars: early type Stars: mass-loss 

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Copyright information

© Kluwer Academic Publishers 1994

Authors and Affiliations

  • J. Puls
    • 1
  • A. Feldmeier
    • 1
  • U. W. E. Springmann
    • 1
  • S. P. Owocki
    • 2
  • A. W. Fullerton
    • 2
  1. 1.Institut für Astronomie und AstrophysikUniversität MünchenMünchenGermany
  2. 2.Bartol Research InstituteThe University of DelawareNewarkUSA

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