Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ap%26ss.114..157m&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 114, no. 1, Sept. 1985, p. 157-163.
Astronomy and Astrophysics
Astrophysics
3
Anisotropy, Convective Heat Transfer, Rotating Matter, Solar Atmosphere, Turbulent Heat Transfer, Cartesian Coordinates, Coriolis Effect, Navier-Stokes Equation, Rayleigh Number, Reynolds Stress, Stellar Envelopes
Scientific paper
An estimate for the anisotropy of the turbulent viscosity s is given in a convective layer heated from below and rotating around a vertical axis. In the case of two-dimensional convection, there is a stationary regime with s of about 2 regardless of the rotation. In the case of three-dimensional convection in a slowly rotating layer (with the Taylor number equal to 1600), nonstationary turbulent regimes take place with s of about 1.6 for R = 25,000 (R is the Rayleigh number) and s is about 1.2 for R = 10,000. The parameter s plays an important role in the theory of differential rotation of the convective solar or stellar envelopes. So far, it has been evaluated empirically or semiempirically. Some prospects in the development of the theory of differential rotation are discussed here in terms of the moment theory of hydrodynamic fields. The relation between this strict approach and an anisotropic viscosity approximation is considered.
Monin Andrei S.
Rakhmanova N. K.
Ruzmaikin Aleksandr
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