Saturn's Ring System
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Saturn's Ring System

The rings of Saturn have puzzled astronomers ever since they were discovered by Galileo in 1610, during the first telescopic observations of the night sky. The puzzles have only increased since Voyagers 1 and 2 imaged the ring system extensively in 1980 and 1981. In addition to the images, several Voyager instruments observed occultations of the ring system with radial resolution as fine as 100 meters. The rings have been given letter names in the order of their discovery. The main rings are, working outward from the planet, known as C, B, and A. The Cassini Division is the largest gap in the rings and separates Rings B and A. In addition a number of fainter rings have been discovered more recently. The D Ring is exceedingly faint and closest to the planet. The F Ring is a narrow feature just outside the A Ring. Beyond that are two far fainter rings named G and E. The particles in Saturn's rings are composed primarily of water ice and range from microns to meters in size. The rings show a tremendous amount of structure on all scales; some of this structure is related to gravitational perturbations by Saturn's many moons, but much of it remains unexplained.

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Animations

  • The Voyager 2 flyby of Saturn (Quicktime format, 822 Kbytes)

    This animation illustrates the geometry of Voyager 2's passage through the Saturn system. This was a NASA full motion video clip, converted to QuickTime format.

  • A "spoke" movie (Quicktime format, 1.02 Mbytes)

    A sequence of Voyager images was used to generate this movie showing the motion of the mysterious "spokes" in Saturn's B Ring.

  • A stellar occulation by Saturn's rings (Quicktime format, 1.02 Mbytes)

    The Voyager 2 photopolarimeter (PPS) and ultraviolet spectrometer (UVS) instruments observed the occultation of the star delta Sco by Saturn's rings. These experiments resolved the rings down to a scale of 100 meters. This animation shows the viewing geometry during the experiment.

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Images

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References

30-day reports from the Voyager 1 and Voyager 2 instrument teams. (Excerpts from Science, April 10, 1981 and January 29, 1982.)

For further reading, consult the following:

  • Cuzzi, J. N., J. J. Lissauer, L. W. Esposito, J. B. Holberg, E. A. Marouf, G. L. Tyler, and A. Bouschot 1984. Saturn's rings: Properties and processes. In Planetary Rings, (R. Greenberg and A. Brahic, Eds.), University of Arizona Press, Tucson, pp. 73-199.
  • Esposito, L. W., J. N. Cuzzi, J. B. Holberg, E. A. Marouf, G. L. Tyler, and C. C. Porco 1984. Saturn's rings: Structure, dynamics, and Particle properties. In Saturn, (T. Gehrels and M. S. Matthews, Eds.), University of Arizona Press, Tucson, pp. 463-545.
  • Nicholson, P. D., M. R. Showalter, L. Dones, R. G. French, S. M. Larson, J. J. Lissauer, C. A. McGhee, P. Seitzer, B. Sicardy, and G. E. Danielson 1996. Observations of Saturn's ring-plane crossings in August and November 1995. Science 272, 509-515.
  • Bosh, A. S., and A. S. Rivkin 1996. Observations of Saturn's inner satellites during the May 1995 ring-plane crossing. Science 272, 518-521.

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Related Web Sites

These sites contain more information about Saturn and its ring system.

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