The determination of the structure of Saturn’s F ring by nearby moonlets

Carl D. Murray (), Kevin Beurle, Nicholas J. Cooper, Michael W. Evans, Gareth A. Williams and Sébastien Charnoz
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Carl D. Murray: Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS, UK
Kevin Beurle: Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS, UK
Nicholas J. Cooper: Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS, UK
Michael W. Evans: Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS, UK
Gareth A. Williams: Astronomy Unit, Queen Mary, University of London, Mile End Road, London E1 4NS, UK
Sébastien Charnoz: C. E. de Saclay, Université Paris 7, L’Orme de Merisiers, 91191 Gif-sur-Yvette Cedex, France

Nature, 2008, vol. 453, issue 7196, 739-744

Abstract: Abstract Saturn’s narrow F ring exhibits several unusual features that vary on timescales of hours to years. These include transient clumps, a central core surrounded by a multistranded structure and a regular series of longitudinal channels associated with Prometheus, one of the ring’s two ‘shepherding’ satellites. Several smaller moonlets and clumps have been detected in the ring’s immediate vicinity, and a population of embedded objects has been inferred. Here we report direct evidence of moonlets embedded in the ring’s bright core, and show that most of the F ring’s morphology results from the continual gravitational and collisional effects of small satellites, often combined with the perturbing effect of Prometheus. The F-ring region is perhaps the only location in the Solar System where large-scale collisional processes are occurring on an almost daily basis.

Date: 2008
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DOI: 10.1038/nature06999

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