Thermal infrared constraints on ammonia ice particles as candidates for clouds in the atmosphere of Saturn

Details Thermal infrared constraints on ammonia ice particles as candidates for clouds in the atmosphere of Saturn Thermal infrared constraints on ammonia ice particles as candidates for clouds in the atmosphere of Saturn

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...53..293o&link_type=abstract

(Saturn Conference, Tucson, AZ, May 11-15, 1982.) Icarus, vol. 53, Feb. 1983, p. 293-300.

Astronomy and Astrophysics

Astronomy

11

Ammonia, Clouds, Ice, Saturn Atmosphere, Atmospheric Models, Constraints, Equatorial Atmosphere, Infrared Astronomy, Thermal Emission, Saturn, Atmosphere, Clouds, Ice, Particles, Ammonia, Thermal Effects, Infrared, Gases, Pioneer, Irr, Pressure, Stratosphere, Emissions, Brightness, Temperature, Radio Observations, Occultations, Opacity, Iris, Infrared Radiometer Spectrometer, Voyager 2, Distribution, Physical Properties

Scientific paper

Saturn atmosphere thermal IR emission observations have uncovered two phenomena that may be accounted for by large ammonia ice particles: the depression of thermal brightness near the equator, and inconsistent IR and radio occultation results. Ammonia ice particles yield the opacity that can account for the contrast between the equatorial region and a brighter area near 15 deg S, and may also reconcile the 45-micron brightness of these two regions with the mean temperature structure of Voyager 2 radio occultation results. A cloud model whose ice particles are distributed in an equal ratio with gas particles up to the 100 mbar pressure level is found to fit the equatorial data, while a thinner cloud, or one that does not extend higher than the 400 mbar limit of the convective region matches the 15 deg S data.

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