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Atmospheric Dynamics of the Outer Planets

Ingersoll, Andrew P. (1990) Atmospheric Dynamics of the Outer Planets. Science, 248 (4953). pp. 308-315. ISSN 0036-8075. doi:10.1126/science.248.4953.308.

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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.

Item Type:Article
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Ingersoll, Andrew P.0000-0002-2035-9198
Additional Information:© 1990 American Association for the Advancement of Science. This work was supported by the NASA Planetary Atmospheres Program and by Voyager Project funds. Contribution number 4824 from the Division of Geological and Planetary Sciences, California Institute of Technology.
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Caltech Division of Geological and Planetary Sciences4824
Issue or Number:4953
Record Number:CaltechAUTHORS:20150126-101414414
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Official Citation:Atmospheric Dynamics of the Outer Planets Andrew P. Ingersoll Science 20 April 1990: 248 (4953), 308-315. [DOI:10.1126/science.248.4953.308]
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:54072
Deposited By: Tony Diaz
Deposited On:26 Jan 2015 19:01
Last Modified:10 Nov 2021 20:28

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