A Study of Saturn's Ring Phase Curves from HST Observations |
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| Authors: | F PouletJN Cuzzi RG FrenchL Dones |
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| Institution: | a NASA Ames Research Center, MS 245/3, Moffett Field, California, 94035, f1poulet@vimstlm.obspm.frf1b NASA Ames Research Center, MS 245/3, Moffett Field, California, 94035c Astronomy Department, Wellesley College, Wellesley, Massachusetts, 02481d Southwest Research Institute, 1050 Walnut Street, Boulder, Colorado, 80302 |
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| Abstract: | Solar phase curves between 0.3° and 6.0° and color ratios at wavelengths λ=0.336 μm and λ=0.555 μm for Saturn's rings are presented using recent Hubble Space Telescope observations. We test the hypothesis that the phase reddening of the rings is less due to collective properties of the ring particles than to the individual properties of the ring particles. We use a modified Drossart model, the Hapke model, and the Shkuratov model to model reddening by either intraparticle shadow-hiding on fractal and normal surfaces, multiple scattering, or some combination. The modified Drossart model (including only shadowing) failed to reproduce the data. The Hapke model gives fair fits, except for the color ratios. A detailed study of the opposition effect suggests that coherent backscattering is the principal cause of the opposition surge at very small phase angles. The shape of the phase curve and color ratios of each main ring regions are accurately represented by the Shkuratov model, which includes both a shadow-hiding effect and coherent backscatter enhancement. Our analysis demonstrates that in terms of particle roughness, the C ring particles are comparable to the Moon, but the Cassini division and especially the A and B ring particles are significantly rougher, suggesting lumpy particles such as often seen in models. Another conspicuous difference between ring regions is in the effective size d of regolith grains (d∼λ for the C ring particles, d∼1-10 μm for the other rings). |
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| Keywords: | planetary rings |
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