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Cassini Finds Treasures Among The Rings And Small Satellites Of Saturn
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CASSINI IMAGING CENTRAL LABORATORY FOR OPERATIONS (CICLOPS)
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Preston Dyches (720) 974-5823
CICLOPS/Space Science Institute, Boulder, Colo.

For Immediate Release: February 24, 2005

CASSINI FINDS TREASURES AMONG THE RINGS AND SMALL SATELLITES OF SATURN

The high porosity of Saturn's innermost small moons, tenuous ringlets discovered in some of the gaps in its rings, the variation in ring particle composition across the rings, and new ring structures which indicate more clearly than ever the transient clumping and aggregation of particles as they orbit Saturn are among the discoveries being reported today in the journal Science by the Cassini Imaging Science team.

The Cassini imaging scientists have spent the last year analyzing images acquired by the Saturn orbiter's camera system beginning last February, when routine imaging of Saturn and its rings and moons began. This collection includes the most detailed images ever collected, taken immediately after the Saturn orbit insertion maneuver, when the spacecraft Cassini flew closer to the rings than any previous spacecraft. This treasure trove of data has yielded surprising results which will, with further study, improve scientists' understanding of how Saturn's rings actually work.

Ring features never before observed have been found in many of the images. Weak, linear density waves excited in the rings by the small moons, Atlas and Pan, have been examined and have yielded satellite masses more reliable than previous measures. These new masses imply that Atlas and Pan are very porous - perhaps constructed like rubble-piles - and similar in this regard to the other moons orbiting just outside Saturn's rings, such as the moons that shepherd the F ring, Prometheus and Pandora. These low densities suggest that all the close-in satellites have been gravitationally pulled together out of smaller bits and pieces.

The examination of these same linear density waves, which lie in the Cassini division in Saturn's rings, indicates that this rarefied region of the rings, like Saturn's C ring, is populated with particles which are on average smaller than particles in the A and B rings, two major rings lying on either side of the Cassini division. The Cassini division material seems also to be vertically thinner - only several meters (yards) - than the A or B rings. Other features, like 'rope-like', 10-kilometer (6-mile) scale structures found in the outer edge of the Encke gap, and splotchy, 30-kilometer (20-mile) scale structures seen near the edge of the A ring, are the newly-found evidence of transient particle clumping - a finding that is key to understanding in full the behavior of particles under the influence of Saturn, orbiting moons and other nearby particles.

Circumstantial evidence, in the form of spike-like features in the outer edge of the narrow Keeler gap in Saturn's A ring, is also presented today that a tiny moon is likely to be found eventually orbiting dead center in this gap. Imaging sequences have been planned to scour the gaps in Saturn's rings for new moons. Imaging scientists expect that eventually, they will find the moon hidden in the Keeler gap.

Several new faint rings have been sighted in Cassini images. One of these, reported earlier, populates the same orbit as the small moon Atlas; others lie in various gaps in the rings and may indicate the presence of tiny embedded moons coincident with them or acting as shepherds nearby. All of these saturnian diffuse rings are either comparable to the jovian ring or more robust. Several of them are spatially variable or kinked, likely evidence of the perturbations of nearby moons.

Saturn's rings are primarily composed of water ice. But recently analyzed multi-color images taken on approach to Saturn suggest more strongly than ever that the amounts of rocky or organic contaminants in the rings is often quite different in neighboring parts of the ring system.

Finally, the new findings include refinements in the orbits of several of Saturn's small satellites, some of them discovered by Cassini and reported earlier. One especially intriguing result is the eccentric and slightly inclined configuration of the orbit of the moon, Pan, which maintains the Encke gap in Saturn's A ring. Until Cassini reached Saturn, it wasn't clear if this moon's orbit would be circular or eccentric. The shape is significant as it indicates the type of interaction the moon has with the ring material surrounding it. If Pan's orbit can be kept eccentric by this interaction, then planets growing in a disk of material surrounding a star may also have eccentric orbits - a conclusion that may help explain the eccentric orbits of planets being discovered today orbiting other stars in our galaxy.

Another reported finding is the observation that the tiny, 5 kilometer (3 mile) -wide moon of Saturn, S/2004 S5 (recently named Polydeuces), discovered by the imaging team and reported late last year, is in fact a Trojan moon of Dione. Saturn is the only planet known to have moons with smaller companion 'Trojan' moons. Trojan moons are those found near stable 'Lagrange points', situated 60 degrees ahead or behind a larger moon in its orbit around a planet. Helene is a previously-known 32-kilometer (20-mile) sized Trojan which orbits ahead of Dione, usually within 15 degrees of the leading Lagrange point; newly-discovered Polydeuces can stray by as much as 32 degrees from Dione's trailing Lagrange point. Dione is not alone in possessing Trojan moons - Tethys, another of Saturn's moons also has a Trojan near each of its stable Lagrange points. However, the wandering exhibited by Polydeuces is the largest so far detected of any Trojan moon.

Images associated with this release, and information about the Cassini-Huygens mission, are available at http://ciclops.org, http://saturn.jpl.nasa.gov and http://www.nasa.gov/cassini.

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 Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo.

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