The atmosphere of Titan - an analysis of the Voyager 1 radio occultation measurements

Details The atmosphere of Titan - an analysis of the Voyager 1 radio occultation measurements The atmosphere of Titan - an analysis of the Voyager 1 radio occultation measurements

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...53..348l&link_type=abstract

(Saturn Conference, Tucson, AZ, May 11-15, 1982.) Icarus, vol. 53, Feb. 1983, p. 348-363. NASA-supported research.

Computer Science

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231

Atmospheric Sounding, Radio Occultation, Satellite Atmospheres, Titan, Voyager 1 Spacecraft, Atmospheric Composition, Atmospheric Models, Equatorial Atmosphere, Methane, Nitrogen, Temperature Profiles, Saturation, Models, Surface, Mixing, Formation, Saturn, Satellites, Titan, Analysis, Voyager 1, Radio Observations, Occultations, Gases, Wavelengths, Atmosphere, Equatorial Regions, Frequencies, Ionization, Layers, Density, Refractivity, Microwaves, Absorption, Troposphere, Stratosphere, Altitude, Composition

Scientific paper

The equatorial atmosphere of Titan was probed by means of two coherently related radio signals transmitted from Voyager 1 at 13.0 and 3.6 cm wavelengths during the November 12, 1980 occultation of the spacecraft by the Saturn satellite. An analysis of the differential dispersive frequency measurements did not reveal any ionization layers in the upper atmosphere of Titan. The gas refractivity data, which extend from the surface to about 200 km altitude, were interpreted in two different ways. In the first, it is assumed that N2 makes up virtually all of the atmosphere, with small amounts of CH4 and other hydrocarbons present. In the second interpretation of the refractivity data, it is assumed that the 3.5 km altitude level corresponds to the bottom of a CH4 cloud layer and that N2 and CH4 were perfectly mixed below this level.

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