In this two-part study, we made several rudimental considerations of the Jovian atmospheres as a step to achieve a comprehensive understanding of the Jovian fluid systems.
In Part I, we address the two basic problems:
(1) The depth of mean zonal flows alternating between eastward and westward directions, and of the vortex-spot motions such as the Great Red Spot, whether they are extending into the deep interior of the molecular fluid layer or are confined to a thin atmospheric layer.
(2) The relative importance of the two energy sources, the solar energy and the internal heat energy, as driving forces of the atmospheric motions. The following results are obtained:
(1) The only possible configuration of the steady flow in the barotropic molecular fluid interior is the axisymmetric zonal flow, as long as a baroclinic upper part of the molecular fluid layer is thin enough compared to the radius of the planet. Because both the mean zonal flows and the vortex-spot motions are almost steady flows, the vortex-spot motions must be confiend to a baroclinic atmospheric layer, while the mean zonal flows may extend deep into the interior.
(2) By extending the formulation of the available potential energy to the convectively unstable condition, it is shown that the main driving force of the Jovian fluid systems is the internal heat energy.
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