Statistics – Computation
Scientific paper
Dec 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..127f&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 1, Dec. 1991, p. 127-136. Research supported by FNRS.
Statistics
Computation
6
Compressible Fluids, Convection, Stellar Convection, Stellar Models, Asymptotic Giant Branch Stars, Computational Astrophysics, Main Sequence Stars, Mixing Length Flow Theory, Pre-Main Sequence Stars, Stellar Physics
Scientific paper
A new stellar convection model is presented that can reproduce the main features of the convective motions in compressible fluids revealed by multidimensional simulations. In contrast to MLT, this model can account for the asymmetry between the upward and downward motions in strongly stratified convective regions. The model explicitly takes into account a velocity dispersion around the mean value which is the only quantity entering the MLT. Only two new free parameters are introduced in a formalism that is otherwise similar to the MLT. The model is readily workable in stellar evolution codes and can be treated analytically in the limit of negligible kinetic fluxes. A hydrodynamical stellar evolution code is used to evaluate the effects of the model on the structure and evolution of premain sequence (PMS), main sequence (MS), and asymptotic giant branch (AGB) stars of low and intermediate mass. It is found that the model has no significant effect on the structure of PMS or MS stars, but modifications of the HR diagrams and structure are found in the case of AGB stars.
Arnould Marcel
Forestini Manuel
Lumer E.
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