Modeling Jupiter's cloud bands and decks

摘要: Abstract A simple jovian cloud scheme has been developed for the Oxford Planetary Unified model System (OPUS). NH 3 -ice, 4 SH-solid, H 2 O-ice and O-liquid clouds have modeled in Southern hemisphere limited area simulations of Jupiter. We found that either three or four condensates existed model. For a deep atmospheric water abundance close to solar composition, an -ice deck above 0.7 bar, SH-solid 2.5 bar with base at about 7.5 frozen tops formed. If depleted is assumed, however, very compact structure develops, where forms by direct sublimation bar. The constitute good tracers motion, we confirmed zonal velocities determined from manual feature tracking layers agree reasonably well velocities. Dense elevated form over latitudes strong upwelling exist areas downwelling. In this leads bands zones domain thin belts, which consistent observationally deduced distribution. Due changes vertical velocity pattern deeper atmosphere, decks are more uniform. This thus includes possibility frequent observations as could be easily detected under clouds. Large scale vortices appeared spontaneously were characterized clouds, expected observations. These eddies leave most discernible imprint on lighter condensate particles uppermost layer.