CICLOPS: Cassini Imaging Central Laboratory for OPerationS

New Ring Phenomena
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New Ring Phenomena
PIA 06195

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  A collection of new ring phenomena, first observed in the sequence of images taken of the dark side of Saturn's rings immediately after Cassini entered orbit, may be evidence of the clumping and aggregation of ring particles caused by the combined gravitational effects of Saturn, orbiting moons, and other ring particles.

Image A displays an unusual mottled-looking narrow region, with a radial width varying with longitude from 5 to 10 kilometers (3 to 6 miles), seen for the first time about 60 kilometers (37 miles) inside the outer edge of the A ring. The resolution of this dayside image is about 1 kilometer (0.6 miles) per pixel. Image B is a close-up of the region, mapped into a longitude-radius system and contrast enhanced. The region is characterized by blotchy light and dark areas about 30 to 40 kilometers (19 to 25 miles) in longitudinal extent. The observed longitudinal extent of this region is about 3.5 degrees.

The mottled regions also are probably caused by particle clumping brought about by gravitational disturbances. The outer A ring edge is sculpted into a seven-lobed pattern by a 7:6 Lindblad resonance (a type of dynamical resonance that occurs in rings systems) with the satellites Janus and Epimetheus. The resonant perturbations in this region are complicated by the presence of these two moons whose orbits are within 50 kilometers (31 miles) of each other. It is possible that the mottled region may be related to the co-orbitals' non-axisymmetric perturbations in this region.

Image C is a dark-side image of the outer edge of the Encke gap, with a resolution of about 270 meters (886 feet) pixel, taken 18 degrees upstream from the moon, Pan, which inhabits the gap. The regularly spaced, narrow dark lanes observed here are the wakes caused by Pan. Rope-like features can be seen between the first two wakes nearest the gap edge. These features are unique in all Cassini images taken so far. They are generally between 10 and 20 kilometers (6 and 12 miles) long and have a cant angle of 5 degrees relative to the orbital direction (in the trailing sense) in the band closest to the gap, and about 9 degrees in the next band out.

In their orbits around Saturn, the particles comprising the rings in this region pass through the Pan wakes. When they do so, they are forced closer together than usual. These ropy features appear to be a product of the enhanced gravitational disturbances that occur when the particles pass through the wakes caused by Pan and consequently are squeezed close together. These disturbances obviously persist even outside the wakes, as is evident here in the presence of the ropy structures in the bands in between the wakes.

The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini-Huygens mission for NASA's Science Mission Directorate, Washington, D.C. The imaging team consists of scientists from the US, England, France, and Germany. The imaging operations center and team lead (Dr. C. Porco) are based at the Space Science Institute in Boulder, Colo.

For more information about the Cassini-Huygens mission, visit http://saturn.jpl.nasa.gov and the Cassini imaging team home page, http://ciclops.org.

Credit: NASA/JPL/Space Science Institute
Released: February 24, 2005 (PIA 06195)
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