The Outer Evolution of Structure in Radiatively Driven Stellar Winds

Details The Outer Evolution of Structure in Radiatively Driven Stellar Winds The Outer Evolution of Structure in Radiatively Driven Stellar Winds

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003rmxac..15..217r&link_type=abstract

Winds, Bubbles, and Explosions: a conference to honor John Dyson, Pátzcuaro, Michoacán, México, September 9-13, 2002 (Eds. S. J.

Statistics

Computation

Hydrodynamics, Instabilities, Stars: Early-Type, Stars: Mass Loss, Stars: Winds, Outflows

Scientific paper

We present a new method to study the evolution of instability-generated structure in the outer winds of hot stars. We coin this method a pseudo-planar moving periodic box technique. It makes use of the fact that the outer evolution of structure can be simplified to a pure gasdynamical problem. It follows a box moving out at a constant speed, containing a representative portion of the structure generated by a radiatively driven model. The method allows us to follow structure out to more than a thousand stellar radii, at relatively low computational cost. We have used a less artificial line-strength cut-off than previous models. We also make a first attempt at improving the treatment of the energy balance in the wind.

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