The Solar System at Radio Wavelengths 701
FIGURE 6 (a) Microwave spectrum of Jupiter, with superposed models for a solar composition atmosphere (dashed line), and one in
which the altitude profiles for the condensable gases were based upon theGalileoprobe data (solid line). (b) Microwave spectrum of
Uranus, with superposed models for a solar composition atmosphere (dashed line), and one in which H 2 S and H 2 O gases are enhanced
by a factor∼10 above solar values. In these models, ammonia gas is significantly depleted at higher altitudes in Uranus atmosphere
through formation of NH 4 SH, so that deeper warmer levels are probed. (c) Cloud structure in Jupiter’s atmosphere as calculated
assuming thermochemical equilibrium. The altitude profile of ammonia gas, based onGalileoand ground-based radio data, is
superposed. (d) Cloud structure in Uranus’s atmosphere as calculated assuming thermochemical equilibrium and CH 4 ,H 2 O and H 2 S
abundances 30 times solar. The altitude profiles for H 2 S and NH 3 gas are indicated. (I. de Pater and J. J. Lissauer, forthcoming,
“Planetary Sciences,” Rev. Ed., Cambridge Univ. Press.)