A Model of the Atmospheric Convection Zone with a Large Increase of Rotation Velocity Between its Bottom and Top
Abstract
A simple model of a slowly rotating stellar or planetary atmospheric convection zone is considered supposing that only growing convective perturbations contribute to the value of nonlinear azimuthal force maintaining the differential rotation of the zone. Besides, the angular velocity of rotation is assumed to be dependent only on the distance to the center. It turns out that in this model some resonance phenomenon is possible, due to which a structure can be formed with a large rotation velocity gradient. This is caused by the interaction of two different azimuthal forces, one being proportional to either the angular velocity or its derivatives, while the other being determined by some mean value of the same velocity. The latter force appears in consequence of different timedependence of the perturbations in rotating versus nonrotating convective zones. A hypothesis is put forward that fast rotation of the upper atmosphere of Venus is due to such resonance interaction.
 Publication:

Astrophysics and Space Science
 Pub Date:
 April 1982
 DOI:
 10.1007/BF00648543
 Bibcode:
 1982Ap&SS..83..105V
 Keywords:

 Angular Velocity;
 Atmospheric Circulation;
 Atmospheric Models;
 Convection;
 Planetary Atmospheres;
 Stellar Atmospheres;
 Azimuth;
 Computational Fluid Dynamics;
 Perturbation Theory;
 Rotating Fluids;
 Astrophysics