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Thermal evolution of Titan's atmosphereThe present model of Titan's atmosphere/surface evolution assumes the presence of a kilometer-deep ethane-methane ocean at the surface that serves as a tropospheric thermal balance-determining atmospheric-gas reservoir. The evolution of the atmospheric thermal structure is driven by gas-abundance changes occurring as stratospheric photolysis irreversibly converts methane into higher hydrocarbons, whereby the ocean becomes ethane-enriched and methane-depleted. A family of evolution models is presented whose various members correspond to different present-day ocean compositions, various atmospheric hydrogen abundances, and different schemes for frequency-averaging the gas opacity. A slow evolution over several billion years is envisioned.
Document ID
19890062442
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Lunine, Jonathan I.
(Arizona Univ. Tucson, AZ, United States)
Rizk, Bashar
(Arizona, University Tucson, United States)
Date Acquired
August 14, 2013
Publication Date
August 1, 1989
Publication Information
Publication: Icarus
Volume: 80
ISSN: 0019-1035
Subject Category
Lunar And Planetary Exploration
Accession Number
89A49813
Funding Number(s)
CONTRACT_GRANT: NAGW-1039
CONTRACT_GRANT: NSG-7558
Distribution Limits
Public
Copyright
Other

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