Two-dimensional simulations of the line-driven instability in hot-star winds

Details Two-dimensional simulations of the line-driven instability in hot-star winds Two-dimensional simulations of the line-driven instability in hot-star winds

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003a%26a...406l...1d&link_type=abstract

Astronomy and Astrophysics, v.406, p.L1-L4 (2003)

Astronomy and Astrophysics

Astrophysics

41

Line: Formation, Radiative Transfer, Stars: Atmospheres, Stars: Early Type, Stars: Mass Loss

Scientific paper

We report initial results of two-dimensional simulations of the nonlinear evolution of the line-driven instability (LDI) in hot-star winds. The method is based on the Smooth Source Function (SSF) formalism for nonlocal evaluation of the radial line-force, implemented separately within each of a set of radiatively isolated azimuthal grid zones. The results show that radially compressed ``shells'' that develop initially from the LDI are systematically broken up by Rayleigh-Taylor or thin-shell instabilities as these structures are accelerated outward. Through radial feedback of backscattered radiation, this leads ultimately to a flow structure characterized by nearly complete lateral incoherence, with structure extending down to the lateral grid scale, which here corresponds to angle sizes of order a fifth of a degree. We briefly discuss the implications for interpreting various observational diagnostics of wind structure, but also emphasize the importance of future extensions to include lateral line-drag effects of diffuse radiation, which may set a minimum lateral scale for break-up of flow structure.

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