Statistics – Computation
Scientific paper
Nov 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.221..409p&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 221, no. 1-2, p. 409-426
Statistics
Computation
2
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
Scientific paper
On the basis of a careful analysis of resonance line formation (both for singlets and doublets) in structured winds, present time dependent models of the line driven winds of hot stars 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 variability' observed in saturate 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 (approximately greater than 1.1 R*) produce resonance lines which agree qualitatively with observational findings; in contrast, the here presented models with structure formation only well out in the wind (approximately greater than 1.6 R* fail in this respect.
Feldmeier Achim
Fullerton Alex W.
Owocki Stanley P.
Puls Jason
Springmann W. E. U.
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