Meridional circulation in rotating stars. VII - The effects of chemical inhomogeneities

Details Meridional circulation in rotating stars. VII - The effects of chemical inhomogeneities Meridional circulation in rotating stars. VII - The effects of chemical inhomogeneities

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...279..384t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 279, April 1, 1984, p. 384-393.

Astronomy and Astrophysics

Astrophysics

41

Atmospheric Circulation, Atmospheric Composition, Chemical Composition, Meridional Flow, Stellar Atmospheres, Stellar Rotation, Abundance, Baroclinic Instability, Hydrodynamics, Stellar Evolution, Stellar Structure, Vortices

Scientific paper

The effects of a gradient of mean molecular weight mu on the rotationally driven currents that pervade the radiative zone of a single, nonmagnetic, main-sequence star are discussed. Detailed numerical calculations are made for the hydrogen-burning core of a solar-type star, assuming that departures from spherical symmetry are not too large. It is found that meridional streaming virtually dies out from the center outward as the mu-gradient grows in a leisurely fashion. This prevents a substantial mixing of matter between the inner (inhomogeneous) and outer (homogeneous) regions in the radiative zone, although the inner region may be penetrated to some degree. To first order in the ratio of the centrifugal force to gravity at the equator, this pattern of circulation is independent of the mean angular velocity. To this order, then, there is no critical rotation rate above which unimpeded mixing may take place.

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