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Science 20 April 1990:
Vol. 248. no. 4953, pp. 308 - 315
DOI: 10.1126/science.248.4953.308
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Articles

Atmospheric Dynamics of the Outer Planets

Andrew P. Ingersoll 1

1 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125

Despite major differences in the solar and internal energy inputs, the atmospheres of the four Jovian planets all exhibit latitudinal banding and high-speed jet streams. Neptune and Saturn are the windiest planets, Jupiter is the most active, and Uranus is a tipped-over version of the others. Large oval storm systems exhibit complicated time-dependent behavior that can be simulated in numerical models and laboratory experiments. The largest storm system, the Great Red Spot of Jupiter, has survived for more than 300 years in a chaotic shear zone where smaller structures appear and dissipate every few days. Future space missions will add to our understanding of small-scale processes, chemical composition, and vertical structure. Theoretical hypotheses about the interiors provide input for fluid dynamical models that reproduce many observed features of the winds, temperatures, and cloud patterns. In one set of models the winds are confined to the thin layer where clouds form. In other models, the winds extend deep into the planetary fluid interiors. Hypotheses will be tested further as observations and theories become more exact and detailed comparisons are made.


THIS ARTICLE HAS BEEN CITED BY OTHER ARTICLES:
Temperature and Composition of Saturn's Polar Hot Spots and Hexagon.
L. N. Fletcher, P. G. J. Irwin, G. S. Orton, N. A. Teanby, R. K. Achterberg, G. L. Bjoraker, P. L. Read, A. A. Simon-Miller, C. Howett, R. de Kok, et al. (2008)
Science 319, 79-81
   Abstract »    Full Text »    PDF »
.
(1996)
Science 274, 377-385
   Abstract »    Full Text »    PDF »
High Winds of Neptune: A Possible Mechanism.
V. E. SUOMI, S. S. LIMAYE, and D. R. JOHNSON (1991)
Science 251, 929-932
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