Vertical distribution of scattering hazes in Titan's upper atmosphere

Details Vertical distribution of scattering hazes in Titan's upper atmosphere Vertical distribution of scattering hazes in Titan's upper atmosphere

Jul 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...55...50r&link_type=abstract

Icarus (ISSN 0019-1035), vol. 55, July 1983, p. 50-62. NASA-supported research.

Physics

83

Atmospheric Scattering, Haze, Satellite Atmospheres, Titan, Extinction, Light Scattering, Limbs, Vertical Distribution, Voyager 2 Spacecraft, Saturn, Satellites, Titan, Distribution, Scattering, Atmosphere, Voyager 2, Intensity, Particles, Density, Latitudes, Altitude, Data, Optical Properties, Depth, Equatorial Regions, Polar Regions, Haze

Scientific paper

Radial intensity scans of a Voyager 2 high phase angle image of Titan have been inverted to yield vertical extinction profiles at 1° intervals around the limb. A detached haze layer with peak particle number densities ≡0.2 cm-3 exists at all latitudes south of ≡45°N, and at an altitude of 300 - 350 km. The optical depth 0.01 level lies at a radius of 2932±5 km at the equator and at a radius of 2915±10 km over the poles (altitudes of 357±5 and 340±10 km, respectively). In addition to the haze layer at 300 - 350 km, there is a small enhancement in the extinction at ≡450 km which exists at all latitudes between 75°S and ≡60°N.

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