Spectrophotometric gradients, spectral variations of albedo, and the limb darkening coefficient of Saturn's disk.

Details Spectrophotometric gradients, spectral variations of albedo, and the limb darkening coefficient of Saturn's disk. Spectrophotometric gradients, spectral variations of albedo, and the limb darkening coefficient of Saturn's disk.

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993sosyr..27..223t&link_type=abstract

Solar System Research, Vol. 27, No. 3, p. 223 - 230

Computer Science

Saturn: Albedo, Saturn: Limb Darkening, Saturn: Spectrophotometry, Saturn Atmosphere: Clouds

Scientific paper

By computer processing and analysis of spectrograms of the central meridian and intensity equator of Saturn obtained in 1979, 1988, 1990, and 1991, the authors determine the spectrophotometric gradients relative to the Sun's spectrum at different planetary latitudes. The spectral gradients at λλ430 - 530 nm (G1) and 540 - 640 nm (G2) differ significantly, and these differences depend on latitude. One possible cause of these differences could be latitudinal variations of the optical depth of the above-cloud atmosphere with Rayleigh scattering: the upper boundary of the clouds or haze lies deeper at temperate latitudes and higher in the equatorial zone. The authors note some peculiarities of the spectral reflectivity in 1991 at temperate latitudes. After correcting the intensity equator spectrograms for the inclination of Saturn's equator and the image quality, they find the limb darkening coefficient as a function of wavelength for the equatorial zone. The relationship between the limb darkening coefficients and the brightness coefficients supports the conclusions that the asymmetry of the scattering function in the clouds or haze is small, and that significant back scattering occurs.

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