Multiscale model equations for turbulent convection and convective overshoot

Details Multiscale model equations for turbulent convection and convective overshoot Multiscale model equations for turbulent convection and convective overshoot

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267..795m&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 267, April 15, 1983, p. 795-821.

Physics

25

Convective Flow, Flow Theory, Solar Physics, Turbulence Models, Turbulent Flow, Advection, Boundary Value Problems, Buoyancy, Navier-Stokes Equation, Viscosity, Vortices

Scientific paper

Most calculations of stellar or solar evolution take the boundaries of a convection zone to be where the radiative temperature gradient changes from super to subdiabatic (or vice versa) and take the interior thermal structure of a convection zone to be that given by standard mixing-length theory. Shortcomings of mixing-length theory arise because it is not a full physical theory, following from the Navier Stokes equations by formal manipulation. The approach proposed involves an elimination of the physical uncertainties associated with mixing-length theory. The set of time-dependent equations obtained models the multiscale and nonlocal effects of convective overshoot, location of the convective interface, time-dependent convection, and turbulent mixing.

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