Simulating the Keeler Gap in Saturn's Rings: Wake and Edge Dynamics

Details Simulating the Keeler Gap in Saturn's Rings: Wake and Edge Dynamics Simulating the Keeler Gap in Saturn's Rings: Wake and Edge Dynamics

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.4205l&link_type=abstract

American Astronomical Society, DPS meeting #38, #42.05; Bulletin of the American Astronomical Society, Vol. 38, p.560

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Large scale simulations (15-30 million particles) of the Keeler gap region are presented that explore the dynamics within a few tens of kilometers of the gap edge radially and one degree downstream from Daphnis. The simulations are able to reproduce most of the features seen in Cassini observations of the region and help to explain their origins by allowing us to compare different system configurations. Simulations are presented with Daphnis on a circular orbit as well as on an eccentric orbit and with varying masses. Three styles of simulations are presented to show the impact of collisions and particle self-gravity on the dynamics. The significant differences between the Encke gap and the Keeler gap can be explained by the early wake formation at the Keeler gap and the intersection of streamlines in the first few orbital periods. The strong radial eccentricity gradient caused by the close proximity to the moon is also significant. Particle self-gravity effects become more significant further downstream from Daphnis after collisions have significantly damped the forced eccentricity. This work was supported by a NASA PG&G grant.

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