Computer Science
Scientific paper
Aug 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989icar...80..370l&link_type=abstract
Icarus (ISSN 0019-1035), vol. 80, Aug. 1989, p. 370-389.
Computer Science
16
Atmospheric Composition, Atmospheric Models, Chemical Evolution, Satellite Atmospheres, Titan, Atmospheric Chemistry, Ethane, Methane, Ocean Models, Photolysis, Planetary Environments, Saturn, Satellites, Titan, Thermal Properties, Evolution, Atmosphere, Models, Ethane, Methane, Gases, Abundance, Enrichment, Composition, Parameters, Surface, Temperature, Photolysis, Hydrogen, Calculations, Diagrams, Thermodynamics, Photochemistry, Depletion
Scientific paper
The 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.
Lunine Jonathan I.
Rizk Bashar
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