Physics
Scientific paper
Apr 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...52..191b&link_type=abstract
Solar Physics, vol. 52, Apr. 1977, p. 191-198. Research supported by the Consiglio Nazionale delle Ricerche of Italy.
Physics
4
Convective Flow, Energy Transfer, Solar Physics, Solar Rotation, Angular Velocity, Boussinesq Approximation, Equations Of Motion, Numerical Integration, Rayleigh Number, Stream Functions (Fluids)
Scientific paper
The possibility is investigated that large flux differences between the poles and the equator at the bottom of the solar convection zone are compatible with the small differences observed at the surface. The consequences of increasing the depth of the convection zone due to overshooting are explored. A Boussinesq model is used for the convection zone, and it is assumed that the interaction of global convection with rotation is modeled through a convective flux coefficient whose perturbed part is proportional to the local Taylor number. Numerical integration of the equations of motion and energy shows that coexistence between large pole-equator flux differences at the bottom and small ones at the surface is possible if the solar convection zone extends to a depth of 0.4 solar radius. The angular-velocity distribution inside the convection zone is in agreement with the alpha-omega-dynamo theories of the solar cycle.
Belvedere Gaetano
Paterno' Lucio
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