Convection in a rotating deep compressible spherical shell - Application to the sun

Details Convection in a rotating deep compressible spherical shell - Application to the sun Convection in a rotating deep compressible spherical shell - Application to the sun

Oct 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...54..289b&link_type=abstract

Solar Physics, vol. 54, Oct. 1977, p. 289-312.

Physics

31

Atmospheric Circulation, Atmospheric Models, Convection, Energy Transfer, Solar Atmosphere, Solar Rotation, Angular Velocity, Meridional Flow, Mixing Length Flow Theory, Numerical Integration, Spherical Shells, Stream Functions (Fluids)

Scientific paper

Effects of rotation on a deep compressible spherical shell representing the sun's convection zone are investigated. Ways in which rotation can affect energy transport and large-scale motions are examined, the hypothesis that the solar convection zone is unstable toward global convection is evaluated, and the way in which large-scale meridional circulation establishes latitudinal and depth variations of angular velocity is studied. The convection zone is modeled as a compressible spherical shell with a thickness of 0.2 solar radius on the assumptions that the interaction of convection with rotation is the basic mechanism producing differential rotation, energy transport through the convection zone is by convection only, mixing-length theory adequately represents the convective transport, and rotation acts as a perturbation on the turbulent convective flux through its transport coefficient. The basic equations of the zero-order model are integrated numerically in the limit of large viscosity and slow rotation. Results are obtained which show that the large-scale circulation in the convection zone occurs in three radial cells extending from the poles to the equator, that the radial motion of this circulation is typically a few tenths cm/s, and that the angular velocity increases inward by about 6 percent, with a significant variation only in the lower half of the convection zone.

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