Interferometry of Saturn and its rings at 1.30-cm wavelength

Details Interferometry of Saturn and its rings at 1.30-cm wavelength Interferometry of Saturn and its rings at 1.30-cm wavelength

Apr 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...42..125s&link_type=abstract

Icarus, vol. 42, Apr. 1980, p. 125-135.

Computer Science

3

Brightness Temperature, Microwave Interferometers, Particle Emission, Saturn Rings, Thermal Radiation, Atmospheric Models, Curve Fitting, Data Reduction, Limb Darkening, Optical Thickness, Superhigh Frequencies, Saturn, Rings, Interferometry, Wavelengths, Observations, Analysis, Brightness Temperature, Optical Properties, Thickness, Depth, Particles, Scattering, Albedo, Limbs, Darkening, Models, Radius, Ammonia, Data, Atmosphere, Maps, Comparisons, Microwaves, Composition, Ice, Size, Procedure, Flux Density

Scientific paper

Interferometric observations of Saturn and its rings at a wavelength of 1.30 cm are presented in an attempt to place constraints upon the amount of thermal radiation emitted by the ring particles. Model-fitting and aperture synthesis techniques were used to analyze the data obtained on nine baselines at a frequency of 23 GHz. Ring optical depth is found to be close to that observed at visible wavelengths, while ring brightness temperature is only 7 + or - 1 K, requiring the ring particles to be nearly conservative scatterers at this wavelength and implying an upper limit of 2.4 m to the radius of a typical ring particle with a lower limit of 0.95 to its single scattering albedo. An observed difference between planetary radii observed at 1.30 and 3.71 cm is interpreted in terms of limb darkening and found to be marginally different from the predictions of atmospheric models in which NH3 is the principal source of microwave opacity.

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