Alternating light and dark bands, extending a great distance across Saturnís D and C rings, are shown here in these Cassini images taken one month before the planetís August 2009 equinox.
The C ring stretches across the upper left and middle of the image. The D ring is barely visible amid the noise in the lower right of the image.
The periodic brightness variations in the rings have a subtler, narrow appearance in this mosaic of three Cassini images than other larger features of the rings, such as the Columbo Gap which appears as a black arc on the left of the center frame of the mosaic. These brightness variations are almost certainly caused by the changing slopes in the rippled ring plane, much like the corrugations of a tin roof. Although previous Cassini observations (see PIA08325) had revealed corrugations in the D ring extending over 500 miles (800 kilometers), this image shows these features extending for 6,200 miles (10,000 kilometers) into the C ring.
Later equinox images revealed the true dimension of this corrugation, extending completely across the C ring, right up to the inner B ring edge for a total breath of about 17,000 kilometers (11,000 miles) -- see PIA11670 and PIA11671.
This and other new imagery supports earlier evidence that something dramatic happened in the early 1980s to initiate this feature.
In 2006, imaging scientists speculated that a collision with a comet or asteroid may have disturbed the D ring. That explanation seems less likely now that this and other new images show the effect spread over a much broader radial range, extending right up to the inner B ring. Scientists continue to investigate the cause of this disturbance.
Whatever caused the corrugation apparently tilted a vast region of the inner rings relative to Saturnís gravitational field in a relatively short period of time during the early 1980s. In the intervening years, the natural tendency for inclined orbits to systematically and slowly wobble at different rates, depending on their distance from Saturn, has created a tightly wound spiral corrugation in the ring plane.
These images and others like them are only possible around the time of Saturnís equinox which occurs every half-Saturn-year (equivalent to about 15 Earth years). The illumination geometry that accompanies equinox lowers the sunís angle to the ring plane, significantly darkens the rings, and causes out-of-plane structures to cast long shadows across the rings. Cassiniís cameras have spotted not only the predictable shadows of some of Saturnís moons (see PIA11657), but also the shadows of newly revealed vertical structures in the rings themselves (see PIA11665).
This view looks toward the unilluminated side of the rings from about 24 degrees above the ring plane. The D ring has been brightened relative to C ring to enhance visibility.
The images were taken in visible light with the Cassini spacecraft narrow-angle camera on July 11, 2009. The view was acquired at a distance of approximately 470,000 kilometers (292,000 miles) from Saturn and at a Sun-Saturn-spacecraft, or phase, angle of 25 degrees. Image scale is 2 kilometers (2 miles) per pixel.
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 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 operations center is based at the Space Science Institute in Boulder, Colo.
For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/. The Cassini imaging team homepage is at http://ciclops.org.