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M. Horányi (LASP), A. Juhász (LASP, KFKI)
We investigated the dynamics of small (0.1~ \mum< rg < 10~ \mum) dust particles in the fields and particles environment of Saturn extending earlier models (Horányi et al., Icarus, 97, 248, 1992; Hamilton and Burns, Science, 264, 550, 1994; and Dikarev, Astron. Astrophys, 346, 2579, 1999). Perturbations due to time-dependent electric charge, solar radiation pressure, planetary oblateness, plasma- and neutral drags were taken into account. The sizes of the dust grains were followed as as they decrease in time due to sputtering. We considered the moons Mimas, Enceladus, Tethys and Dione as sources and sinks of dust grains. Using a Monte Carlo simulation we calculated the spatial density distribution of different sized dust particles. Combining the spatial density distribution with a Mie light scattering calculation, we model the optical depth and brightness distributions of Saturn's E ring. The relative contribution from the various moons can be estimated to achieve an excellent fit to several ground-based and the Voyager observations. The model can be used to predict impact rates for the Cosmic Dust Analyzer on-board Cassini as it will cross this region many times during its mission around Saturn