Nonlinear hydrodynamical models of stellar convective zones

Details Nonlinear hydrodynamical models of stellar convective zones Nonlinear hydrodynamical models of stellar convective zones

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.118..223u&link_type=abstract

(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),

Statistics

Computation

2

Computational Astrophysics, Convective Flow, Hydrodynamics, Stellar Models, Stellar Structure, Diffusivity, Nonlinearity, Prandtl Number, Reynolds Number, Turbulent Diffusion

Scientific paper

Large-eddy simulation (LES) of turbulent convection is discussed in various versions (mixing-length theory, modal theory and spectral theory) in respect to the application to stellar convective zones. For the model construction, the non-local mixing-length formalism is suitable. However, for the determination of basic flow patterns and of mixing-length, the quasi-linear and nonlinear modal theories are useful. The eddy diffusivities are essential in these theories, and the nonlinear treatment of convection consistent with turbulent diffusivities (of effective Reynolds number of about 20 and Prandtl number of 0.4) offers a simple method of constructing stellar models without the use of the mixing-length.

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