Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apjs...61..585g&link_type=abstract
Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 61, July 1986, p. 585-608.
Astronomy and Astrophysics
Astrophysics
125
Compressible Fluids, Convection, Rotating Spheres, Solar Rotation, Stellar Models, Stellar Rotation, Energy Spectra, Kinetic Energy, Radial Velocity, Spherical Shells, Stellar Models, Temperature Distribution
Scientific paper
The deeper layers of the solar or stellar convection zone are modeled in view of extensive calculations of nonlinear convection of a compressible fluid in a rotating spherical shell, using the anelastic approximation for the integrated equations. Solar values are used for the luminosity, rotation, and eddy diffusivities; the Rayleigh number for convection is then determined by the luminosity. In the cases of both model depths used, the dominant convection patterns in low latitudes are a broad spectrum of rolls with north-south axes, approximately symmetric about the equator, with more cellular patterns in high latitudes. The results obtained are similar to those of Glatzmaier (1984, 1985), who used substantially different solution techniques, and they agree with the differential rotation observed at the solar surface.
Gilman Peter A.
Miller Jason J.
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