Distribution of Ringshttp://photojournal.jpl.nasa.gov/catalog/PIA08389
This image of the B ring in 2010 shows spoke phenomena, appearing bright when viewed at a high phase angle. They appear dark in images taken at lower phase angles, telling us something about the nature of the particles making up the spokes. http://photojournal.jpl.nasa.gov/catalog/PIA12605
A colour image of the Cassini division from 2005, separating the main A and B rings, possibly consisting of more contaminated ices than the fresher material comprising the two rings. http://photojournal.jpl.nasa.gov/catalog/PIA07631
A large ring of dust was discovered in 2009 by the Spitzer Space Telescope in infrared light, possibly originating from impact events on Phoebe (a retrograde satellite with an inclined orbit). The full story can be found here.
Probing the Ring Properties
Just as for Saturn, astronomers use images of the rings in different wavelengths to deduce the composition, sizes and structure of the various ices. This comparison image from the Visual and Infrared Mapping Spectrometer (VIMS) in 2004 shows scattered light coming through the rings on the left (so thicker rings appear darker); then the strength of a signature of pure water ice that seems to grow strong in the A ring; and finally a signature of some unidentified 'dirty' material causing darkening of the rings. For more details see: http://photojournal.jpl.nasa.gov/catalog/PIA06350 (Credit: NASA/JPL/University of Arizona)
http://photojournal.jpl.nasa.gov/catalog/PIA03561 Credit: NASA/JPL/GSFC
Another example of vertical structures observed in May 2009 when tiny Daphnis, sat within the Keeler gap within Saturn's A ring, interacts with the surrounding material. The shadows indicate structures some 1.5 km tall, compared to the expected 10-m thickness of the main rings. The continuous interaction creates an edge wave which propagates around the circumference of the Keeler gap. http://photojournal.jpl.nasa.gov/catalog/PIA11653