A study of the three-dimensional turbulent compressible convection in a deep atmosphere at various Prandtl numbers

Details A study of the three-dimensional turbulent compressible convection in a deep atmosphere at various Prandtl numbers A study of the three-dimensional turbulent compressible convection in a deep atmosphere at various Prandtl numbers

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...279..107s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 279, no. 1, p. 107-118

Astronomy and Astrophysics

Astrophysics

17

Atmospheric Models, Atmospheric Turbulence, Compressible Flow, Convective Flow, Hydrodynamics, Prandtl Number, Stellar Interiors, Stellar Models, Three Dimensional Flow, Turbulent Flow, Computerized Simulation, Correlation Coefficients, Mathematical Models, Stream Functions (Fluids), Thermodynamic Properties, Velocity Distribution

Scientific paper

Using numerical experiments, Chan & Sofia (1989) derived a set of empirical formulas/relations to describe turbulent, efficient convection with a depth about 5 pressure scale heights. Their numerical experiments covered a range of parameters including the total flux flowing through the region and the ratio of specific heats of the convecting gas. The relations they found seem to be quite independent of these parameters. In this paper, we test the dependence of these relations on another important parameter, the Prandtl number. We perform three-dimensional numerical experiments in a way similar to that of Chan and Sofia. Four sequences of solutions have been computed corresponding to four different values of the Prandtl number (Pr) viz. 0.01, 0.1, 1/3, and 1.0. The results indicate that the coefficients of the relations are dependent on the Prandtl number, but some are less sensitive than others. We list the coefficents of the relations for each of the Prandtl number and discuss the implications here.

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