Analysis of Saturn's Huygens Ringlet using Cassini ISS images

Details Analysis of Saturn's Huygens Ringlet using Cassini ISS images Analysis of Saturn's Huygens Ringlet using Cassini ISS images

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1417s&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1417

Computer Science

Scientific paper

The relation between Keplerian modes of the inner and outer edges of the ringlet is complicated, with two distinct behaviors apparent: the earliest data set, taken in 2005, shows a steep eccentricity gradient, a mean width of ~50 km, and an apsidal offset (outer minus inner) of ~45 deg; later data sets show a nearly flat eccentricity gradient, mean widths decreasing with time to ~20 km, and near apsidal alignment. Differential precession would produce a negative apsidal offset (at least initially), not the positive offset seen in the earliest observation. In order to reach the observed configuration, the ring would have to be either oscillating about an apsealigned state with an amplitude of at least 45 deg, or the inner edge would need to have overtaken the outer edge shortly before the 2005 observations. In order for the inner apoapse to shear past the outer periapse, the ring elements would need to adjust to avoid streamline crossing. The large mean width and eccentricity gradient seen in the earliest data set may be consistent with such an adjustment. The decreasing width seen in the subsequent observations suggests an active confinement mechanism that has yet to be explained.

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