Abstract The radio spectra and resolved images of the four giant planets are compared. Bright bands across the planetary disks imply a latitudinal variation in the precise ammonia abundance. Jupiter and Saturn are very much alike: NH 3 gas is depleted by a factor of ∼ 4–5 at P ≲ 1 bar, and enhanced by 1.5- > 3 at P > 2–3 bars. Uranus and Neptune are very different from the former two planets, in that they exhibit a depletion of NH 3 gas by ∼ two orders of magnitude over a large altitude range in the atmosphere. Uranus shows a large pole-to-equator gradient in the ammonia abundance. The loss of NH 3 gas in the atmospheres of all four planets (assuming they all have an abundance ≳ solar value at deeper levels) is most likely due to the formation of NH 4 SH. This requires the H 2 S abundance in Jupiter and Saturn to be enhanced by 1 order of magnitude above the solar value and by about 2 orders of magnitude in Uranus and Neptune. The latitudinal variation in the NH 3 abundance on the planets suggests differences in the location of the NH 4 SH cloud layers and the dynamics of the planets.
A comparison of the deep atmospheres of the giant planets
Advances in Space Research ; 10 , 1 ; 79-87
01.01.1989
9 pages
Aufsatz (Zeitschrift)
Elektronische Ressource
Englisch
Seasonal thermal structure of the atmospheres of the giant planets
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