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Methane rain on TitanThe atmosphere of Titan is characterized by means of model computations based on Voyager IRIS IR spectra and published data from laboratory determinations of absorption coefficients and cloud refractive indices. The results are presented in tables and graphs, and it is pointed out that the presence of Ar is not required in the model. Particular attention is given to the role of CH4, which is found to form patchy clouds (with particle radii of 50 microns or greater and visible/IR optical depths of 2-5) at altitudes up to about 30 km. The mechanisms by which such rain-sized particles could form are discussed, and it is suggested that the observed 500-600/cm spectrum is affected much less by the CH4 clouds than by H2 or variations in the temperature of the high-altitude haze.
Document ID
19880059139
Document Type
Reprint (Version printed in journal)
Authors
Toon, Owen B. (NASA Ames Research Center Moffett Field, CA, United States)
Mckay, Christopher P. (NASA Ames Research Center Moffett Field, CA, United States)
Courtin, Regis (NASA Ames Research Center Moffett Field, CA, United States)
Ackerman, Thomas P. (NASA Ames Research Center Moffett Field, CA, United States)
Date Acquired
August 13, 2013
Publication Date
August 1, 1988
Publication Information
Publication: Icarus
Volume: 75
ISSN: 0019-1035
Subject Category
LUNAR AND PLANETARY EXPLORATION
Distribution Limits
Public
Copyright
Other