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Saturn's rings, reminiscent of an early Solar System present a uniqueopportunity to investigate experimentally some mechanisms thought to beresponsible for planet and planetesimal formation in protoplanetary discs. Herewe extended the comparison of our numerical models of Prometheus encounteringthe F ring employing non-interacting and interacting particles. Higherresolution analysis revealed that the density increases known to exist atchannel edges is more complex and localised than previously thought. Asymmetrybetween density increases on channel edges revealed that the channel edgefacing way from Prometheus to be the most stable but with lowest maximumincreases. However, on the channel edge facing Prometheus the interacting modelshowed large chaotic fluctuations in the maximum density of some clumps, muchlarger than those of the other channel. The likely cause of this asymmetry is avariance in localised turbulence introduced into the F ring by Prometheus. Highresolution velocity dispersion maps showed that there was a spatial linkbetween the highest densities and the highest velocity dispersions in theinteracting model. Thus suggesting that the high velocity dispersion we see isthe reason for the observed inhomogeneous distribution of fans (evidence ofembedded moonlets) on some of the channel edges facing Prometheus.

A Detailed Numerical Analysis of Asymmetrical Density Distribution in Saturn's F ring During an Encounter with Prometheus