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Saturn: UBV photoelectric pinhole scans of the disk,II
Authors:Michael J Pricez  Otto G Franz
Institution:Science Applications, Inc., 5055 E. Broadway, Suite A-214, Tucson, Arizona 85711 USA;Lowell Observatory, P.O. Box 1269, Flagstaff, Arizona 86002, USA
Abstract:During the 1980 Saturn apparition, calibrated UBV pinhole scans of the disk were obtained with a photoelectric area-scanning photometer. Point spread function data were also taken. Equatorial and polar scans were used to investigate the structure of the Satur atmosphere. The observational geometry was optimum. Not only was Saturn at opposition, but the ring system was essentially edge on to both the Sun and Earth. Our analysis indicates that the atmosphere of Saturn can be represented by a finite clear H2 layer overlaying a semi-infinite absorbent aerosol haze. The extent of the clear H2 region appears to be latitude dependent. The H2 column density varies systematically from ~15 km-am over the equatorial and polar regions to ~ 31 km-am at temperate latitudes. The hemispheres of the planet are similar. Our earlier conclusion, that the aerosol haze is strongly absorbent in the ultraviolet, is confirmed; its effective U-band single-scattering albedo is ~0.4. Latitudinal disk structure at visual wavelengths appears to be the result of local variations in the volume density of absorbent particles in the aerosol layer.
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