Physics
Scientific paper
Oct 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986joat.conf..156i&link_type=abstract
In NASA. Goddard Inst. for Space Studies The Jovian Atmospheres p 156-162 (SEE N87-17598 09-91)
Physics
Baroclinity, Barotropic Flow, Convective Flow, Eddy Viscosity, Heat Flux, Planetary Cores, Ekman Layer, Geostrophic Wind, Jupiter (Planet), Saturn (Planet)
Scientific paper
In the theory of hydrostatic quasi-geostrophic flow in the Earth's atmosphere the principal results do not depend on the eddy viscosity. This contrasts with published theories of convection in deep rotating fluid spheres, where the wavelength of the fastest growing disturbance varies as E1/3, where E, the Ekman number, is proportional to the eddy viscosity. A new theory of quasi-columnar motions in stably stratified fluid spheres attempts to capture the luck of the meteorologists. The theory allows one to investigate the stability of barotropic and baroclinic zonal flows that extend into the planetary interior. It is hypothesized that the internal heat Jupiter and Saturn comes out not radially but on sloping surfaces defined by the internal entropy distribution. To test the hypothesis one searches for basic states in which the wavelength of the fastest-growing disturbance remains finite as E tends to zero, and is which the heat flux vector is radially outward and poleward.
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