Variations of the stratospheric temperature along the limb of Uranus: Results of the 22 April 1982 stellar occultation - Sicardy, B.; Combes, M.; Lecacheux, J.; Bouchet, P.; Brahic, A.; Laques, P.; Perrier, C.; Vapillon, L.; Zeau, Y. (Elsevier)
Stratospheric temperature profiles of Uranus were derived from the stellar occultation of 22 April 1982 in the pressure range 5-30 μbar. The observations were made at the European Southern Observatory, Chile, and at the Observatoire du Pic du Midi et de Toulouse, France with two telescopes in both sites. The study of these profiles confirms that Uranus' stratosphere is warmer than had been expected from radiative models (J. F. Appleby, 1980, Atmospheric Structures of the Giant Planets from Radiative-Convective Equilibrium Models. PhD. Thesis, State University of New York at Stony Brook) and that there has been a general increase of temperature since 1977 (R. G. French, J. L. Elliot, E. W. Dunham, D. A. Allen, J. H. Elias, J. A. Frogel, and W. Liller, 1983, Icarus 53, 399-414). Furthermore, the profiles exhibit a nonisothermal feature with a maximum temperature around the 8-μbar pressure level. The amplitude of this feature increases linearly with the diurnally averaged insolation 〈D〉 up to the observed value 〈D〉 ~ 0.15. Moreover, the temperature at 8 μbar, as well as the mean stratospheric temperature, reaches a plateau around the equator of the planet which is far from maximum insolation. For a nominal abundance of methane η"C"H"4 ~ 3 x 10^-^5 and normal incidence, the UV absorption could compete with the IR methane absorption bands at the pressure level 8 μbar. However, the high temperatures observed even at grazing incidence imply important circulation phenomena to isothermalize distant regions of the planet. Alternatively, 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 (6 x 10^1^0 g vs 5 x 10^1^8 g) 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 x 10^5 years) so that a dynamical process is needed to sustain the aerosol layer.
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Keywords: U