Generating Banded Zonal Flows on Jupiter and Saturn

Details Generating Banded Zonal Flows on Jupiter and Saturn Generating Banded Zonal Flows on Jupiter and Saturn

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmed51a0011a&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #ED51A-0011

Physics

5707 Atmospheres: Structure And Dynamics, 3314 Convective Processes, 3319 General Circulation, 0343 Planetary Atmospheres (5405, 5407, 5409, 5704, 5705, 5707), 0815 Informal Education

Scientific paper

The alternating bands of Jupiter and Saturn, represent surface winds with speeds of order 100 m/s. The Galileo and Cassini sattelite missions have and will continue to provide stunning visual images and data from the surface of these gas giants. In addition to detailed spatial resolution, these satellite missions also yield information on the temporal evolution of the surface flow. Models of thermally-driven, rapidly-rotating deep spherical shell convection naturally develop strong zonal flows with alternating bands, similar to those observed on the giant planets. Here we will present images and results from numerical simulations to demonstrate how these zonal flows can be convectively generated by Reynolds stresses at low latitudes and by thermal winds processes at higher latitudes. Comparisons will be presented between our results and images and surface wind data from Jupiter and Saturn.

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