Computer Science
Scientific paper
Aug 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...59..133s&link_type=abstract
Icarus (ISSN 0019-1035), vol. 59, Aug. 1984, p. 133-161. Previously announced in STAR as N82-33311.
Computer Science
140
Altitude, Atmospheric Composition, Cosmic Rays, Dissociation, Earth Magnetosphere, Rotating Plasmas, Satellite Atmospheres, Solar Radiation, Solar Wind, Titan, Clouds, Condensates, Organic Materials, Saturn, Satellites, Titan, Condensation, Organic Compounds, Gases, Atmosphere, Altitude, Dissociation, Calculations, Solar Wind, Clouds, Ultraviolet, Protons, Electrons, Magnetosphere, Particles, Cosmic Rays, Synthesis, Hydrocarbons, Production Rates, Optical Properties, Depth, Scattering, Mesosphere, Phases, H
Scientific paper
The 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.
Reid Thompson W.
Sagan Carl
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