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Astron. Astrophys. 340, 419-430 (1998)


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A simple convection model for selfgravitating fluid dynamics

Time-dependent convective energy transfer in protostars and nonlinear stellar pulsations

G. Wuchterl and M.U. Feuchtinger

Institut für Astronomie der Universität Wien, Türkenschanzstrasse 17, A-1180 Wien, Austria

Received 15 July 1998 / Accepted 2 October 1998

Abstract

We describe a relatively simple time-dependent convection model that can be coupled to the equations of radiation hydrodynamics. We show that it behaves in a physically plausible way in protostellar collapse flows and is quantitatively correct for nonlinear RR-Lyrae pulsations and the Sun. Together with the equations of radiation hydrodynamics the model closely approximates the classical stellar structure equations with mixing length convection for a set of standard assumptions.

Key words: convection – hydrodynamics – stars: formation – stars: oscillations

Send offprint requests to: M.U. Feuchtinger (fm@amok.astro.univie.ac.at)

© European Southern Observatory (ESO) 1998

Online publication: November 9, 1998

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