The Saturn ring plane crossings in 1995--96 allowed observers using the Hubble Space Telescope and the W. M. Keck telescope to image the planet's diffuse rings from 0.3 ��m-- 2.2 ��m at a scattering angle ` � � 175 ffi. We calculate the G ring reflectance for size distributions of dust to km-sized bodies derived from a physical, evolutionary model. The model tracks the evolution of the G ring from its initial formation following the disruption of a progenitor satellite (Canup & Esposito 1997), until a steady state distribution is reached. We calculate the total particle scattering from contributions due to Mie scattering, isotropic scattering, and Lambert scattering, and compare the spectra, phase curves, and RMS particle mass from our physical model to that observed by HST, Keck, and Voyager. A range of particle size distributions from the models are consistent with the observations. These distributions have a dust component that can be described by the differential power law exponent q dust, in the range 1.5--3.5. A quasi-Gaussian size distribution centered at 15 ��m also matches the observations, although is not predicted by the evolutionary model. Distributions with q dust � � 4, such as that
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