Variations of the stratospheric temperature along the limb of Uranus - Results of the 22 April 1982 stellar occultation

Details Variations of the stratospheric temperature along the limb of Uranus - Results of the 22 April 1982 stellar occultation Variations of the stratospheric temperature along the limb of Uranus - Results of the 22 April 1982 stellar occultation

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icar...64...88s&link_type=abstract

Icarus (ISSN 0019-1035), vol. 64, Oct. 1985, p. 88-106.

Astronomy and Astrophysics

Astronomy

17

Atmospheric Temperature, Stellar Occultation, Stratosphere, Uranus Atmosphere, Aerosols, Atmospheric Heating, Energy Dissipation, Photochemical Reactions, Solar Flux, Temperature Profiles, Uranus, Stratosphere, Temperature, Occultations, Astronomy, Observations, Telescope Methods, Pressure, Amplitude, Insolation, Methane, Abundance, Ultraviolet, Infrared, Absorption, Aerosols, Layering, Dust, Mass, Dynamics, Rings, Source, Diagrams, Lightcurves, Photometry, Energy, Calcualtions, Heating, Dissipation, Mechan

Scientific paper

Stratospheric temperature profiles of Uranus were derived from the stellar occultation of 22 April 1982 in the pressure range 5 - 30 μbar. The study of these profiles confirms that Uranus' stratosphere is warmer than had been expected from radiative models. Furthermore, the profiles exhibit a nonisothermal feature with a maximum temperature around the 8-μbar pressure level. The observed profiles may suggest that an optically thin aerosol layer distributed over one scale height is responsible for the temperature maximum at 8 μbar. The total mass of dust necessary to heat this region up significantly would be a small fraction of the Uranian ring system, which appears then as a possible reservoir of dust. However, a falling rate of ≡1 msec-1 would deplete the rings in a short time (≡2×105years) so that a dynamical process is needed to sustain the aerosol layer.

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