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Numerical simulation of the circulation of the atmosphere of TitanA three dimensional General Circulation Model (GCM) of Titan's atmosphere is described. Initial results obtained with an economical two dimensional (2D) axisymmetric version of the model presented a strong superrotation in the upper stratosphere. Because of this result, a more general numerical study of superrotation was started with a somewhat different version of the GCM. It appears that for a slowly rotating planet which strongly absorbs solar radiation, circulation is dominated by global equator to pole Hadley circulation and strong superrotation. The theoretical study of this superrotation is discussed. It is also shown that 2D simulations systemically lead to instabilities which make 2D models poorly adapted to numerical simulation of Titan's (or Venus) atmosphere.
Document ID
19920023117
Document Type
Conference Paper
Authors
Hourdin, F. (Ecole Normale Superieure Paris, France)
Levan, P. (Ecole Normale Superieure Paris, France)
Talagrand, O. (Ecole Normale Superieure Paris, France)
Courtin, Regis (Observatoire de Paris-Meudon Moffett Field, CA, United States)
Gautier, Daniel (Observatoire de Paris-Meudon)
Mckay, Christopher P. (NASA Ames Research Center)
Date Acquired
September 6, 2013
Publication Date
April 1, 1992
Publication Information
Publication: ESA, Symposium on Titan
Subject Category
LUNAR AND PLANETARY EXPLORATION
Distribution Limits
Public
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