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Production and condensation of organic gases in the atmosphere of TitanThe rates and altitudes for the dissociation of atmospheric constituents on Titan are calculated for solar ultraviolet radiation, the solar wind, Saturn magnetospheric particles, the Saturn co-rotating plasma, and cosmic rays. Laboratory experiments show that a variety of simple gas phase organic molecules and more complex organic solids called tholins are produced by such irradiations of simulated Titanian atmospheres. Except for ultraviolet wavelengths longward of the methane photodissociation continuum, most dissociation events occur between about 3100 and 3600 km altitude, corresponding well to the region of EUV opacity detected by Voyager. For a wide variety of simple to moderately complex organic gases in the Titanian atmosphere, condensation occurs below the top of the main cloud deck at about 2825 km. It is proposed that such condensates, begining with CH4 at about 2615 km comprise the principal mass of the Titan clouds. There is a distinct tendency for the atmosphere of Titan to act as a fractional distillation device, molecules of greater complexity condensing out at higher altitudes.
Document ID
19840063895
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Sagan, C.
(Cornell Univ. Ithaca, NY, United States)
Thompson, W. R.
(Cornell University Ithaca, NY, United States)
Date Acquired
August 12, 2013
Publication Date
August 1, 1984
Publication Information
Publication: Icarus
Volume: 59
ISSN: 0019-1035
Subject Category
Lunar And Planetary Exploration
Accession Number
84A46682
Funding Number(s)
CONTRACT_GRANT: NGR-33-010-082
CONTRACT_GRANT: NGR-33-010-101
Distribution Limits
Public
Copyright
Other

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