Meridional circulation in rotating stars. VI - The effects of anisotropic eddy viscosity

Details Meridional circulation in rotating stars. VI - The effects of anisotropic eddy viscosity Meridional circulation in rotating stars. VI - The effects of anisotropic eddy viscosity

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...271..315t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 271, Aug. 1, 1983, p. 315-320.

Astronomy and Astrophysics

Astrophysics

37

Early Stars, Eddy Viscosity, Hydrodynamics, Stellar Models, Stellar Rotation, Anisotropy, Energy Transfer, Stellar Envelopes, Stellar Mass Accretion, Turbulence Effects

Scientific paper

In this paper we discuss the problem of large-scale meridional streaming and differential rotation in the chemically homogeneous envelope of a nonmagnetic, early-type star, while taking into account the anisotropy of turbulence in the radiative zone. It is shown that the large-scale meridional currents remain unaffected by this anisotropy. It is also shown that the turbulent heat transport and the dissipation of mechanical energy into heat and turbulence are negligible everywhere when compared to the transport of energy by radiation. Hence, Sweet's standard formula provides an adequate solution in the bulk of a radiative zone, so that the time scale of meridional circulation is indeed the Eddington-Sweet time. The effects of anisotropic eddy viscosity on the mean rotation law are also discussed. Finally, it is pointed out that baroclinic instability may be the ultimate cause of turbulent motions in an accretion disc.

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