Non-spherical evolution of the line-driven wind instability

In this paper, we study the structure and stability of line-driven winds using numerical hydrodynamic simulations. We calculate the radiation force from an explicit non-local solution of the radiation transfer equation, rather than a Sobolev approximation, without restricting the flow to one-dimensi...

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Published inMonthly notices of the Royal Astronomical Society Vol. 344; no. 3; pp. 725 - 740
Main Authors Gomez, E. L., Williams, R. J. R.
Format Journal Article
LanguageEnglish
Published Oxford, UK Blackwell Science Ltd 21.09.2003
Subjects
hydrodynamics
instabilities
outflows
shock waves
stars: mass-loss
stars: winds
stars: winds, outflows
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Summary:In this paper, we study the structure and stability of line-driven winds using numerical hydrodynamic simulations. We calculate the radiation force from an explicit non-local solution of the radiation transfer equation, rather than a Sobolev approximation, without restricting the flow to one-dimensional symmetry. We find that the solutions that result have complex and highly variable structures, including dense condensations, which we compare with observed variable absorption features in the spectra of early-type stars.
Bibliography:ark:/67375/HXZ-B095NJFB-8
Present address: AWE plc, Aldermaston, Berks.
istex:DEB7ED8EC177C8E5D69578B82EE13AD3C306BF0B
ObjectType-Article-2
SourceType-Scholarly Journals-1
ObjectType-Feature-1
content type line 23
ISSN:0035-8711
1365-2966
DOI:10.1046/j.1365-8711.2003.06864.x