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- W2009478631 abstract "We present the results of two simulations of the convection zone, obtained by solving the full hydrodynamic equations in a section of a spherical shell. The first simulation has cylindrical rotation contours (parallel to the rotation axis) and a strong meridional circulation, which traverses the entire depth. The second simulation has isorotation contours about mid-way between cylinders and cones, and a weak meridional circulation, concentrated in the uppermost part of the shell.We show that the solar differential rotation is directly related to a latitudinal entropy gradient, which pervades into the deep layers of the convection zone. We also offer an explanation of the angular velocity shear found at low latitudes near the top. A non-zero correlation between radial and zonal velocity fluctuations produces a significant Reynolds stress in that region. This constitutes a net transport of angular momentum inwards, which causes a slight modification of the overall structure of the differential rotation near the top. In essence, the thermodynamics controls the dynamics through the Taylor–Proudman momentum balance. The Reynolds stresses only become significant in the surface layers, where they generate a weak meridional circulation and an angular velocity ‘bump’." @default.
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- W2009478631 date "2001-03-11" @default.
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- W2009478631 title "A large-eddy simulation of turbulent compressible convection: differential rotation in the solar convection zone" @default.
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- W2009478631 doi "https://doi.org/10.1046/j.1365-8711.2001.04036.x" @default.
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