Statistics – Computation
Scientific paper
Apr 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ap%26ss..83..105v&link_type=abstract
Astrophysics and Space Science, vol. 83, no. 1-2, Apr. 1982, p. 105-116.
Statistics
Computation
1
Angular Velocity, Atmospheric Circulation, Atmospheric Models, Convection, Planetary Atmospheres, Stellar Atmospheres, Azimuth, Computational Fluid Dynamics, Perturbation Theory, Rotating Fluids
Scientific paper
A simple model of a slowly rotating stellar or planetary atmospheric convection zone is considered, which supposes that only growing convective perturbations contribute to the value of nonlinear azimuthal force maintaining the differential rotation of the zone. It is assumed that the angular velocity of rotation is dependent on only the distance to the center. Some resonance phenomenon is possible, and thus a structure can be formed with a large rotation velocity gradient. This is caused by the interaction of two different azimuthal forces, and since the two forces are expected to be present whenever the nonstationary phenomena of perturbation growth and decay are of importance, it is expected that the resonance interaction can take place in many convective zones. It is suggested that the resonance action is responsible for the fast rotation of the upper atmosphere of Venus.
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