Stellar turbulent convection - A new model and applications

Details Stellar turbulent convection - A new model and applications Stellar turbulent convection - A new model and applications

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...370..295c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 370, March 20, 1991, p. 295-311.

Statistics

Computation

487

Free Convection, Magnetohydrodynamic Turbulence, Mixing Length Flow Theory, Stellar Evolution, Stellar Interiors, Stellar Models, Computational Astrophysics, Energy Spectra, Globular Clusters, Stellar Structure

Scientific paper

Improvements of the mixing-length theory (MLT) of turbulent convection in stellar atmospheres are developed theoretically. It is pointed out that inaccuracies are introduced into MLT by the approximating assumptions of a single large eddy (rather than many eddies of different sizes) and of incompressibility. In the proposed new model, the full spectrum of turbulent eddies is determined using more recent turbulence models (e.g., the eddy-damped quasi-normal Markovian model of Orszag, 1977), and a new formula for the convective flux is obtained which gives values up to 10 times greater than those of the MLT at high convective efficiencies. The problem of compressibility is addressed by adding one of two new expressions (one with no free parameters) for the mixing length. Numerical results from simulations of a solar-type star and a 0.8-solar-mass globular-cluster star are presented in tables and graphs and discussed in detail; the agreement with observations is found to be better than with the MLT.

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