2003/05/30 by E. L. Gomez, R. J. R. Williams · 3 citations
Physics and Astronomy · #Astro and Planetary Science #Instability #Radiation #Radiation pressure #Solar and Space Plasma Dynamics #Spectral line #Stability (learning theory) #Stellar, planetary, and galactic studies #Variable (mathematics) #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2003.06864.x
published in Monthly Notices of the Royal Astronomical Society 344(3), 725-740 (Oxford University Press) · Accepted by MNRAS, 17 pages, 15 postscript figures, 4 large figures appear as jpeg files
arxiv created 2003/05/30 · openalex publication_date 2003/09/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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.