The eccentric Saturnian ringlets at 1.29 R(s) and 1.45 R(s)

Details The eccentric Saturnian ringlets at 1.29 R(s) and 1.45 R(s) The eccentric Saturnian ringlets at 1.29 R(s) and 1.45 R(s)

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...60....1p&link_type=abstract

Icarus (ISSN 0019-1035), vol. 60, Oct. 1984, p. 1-16.

Physics

39

Planetology, Saturn Rings, Voyager Project, Eccentricity, Kinematics, Mass, Optical Thickness, Shapes, Stellar Occultation, Saturn, Rings, Ringlets, Eccentricity, Shape, Kinematics, C Ring, Iss Instrument, Physical Properties, Characteristics, Voyager Missions, Rss Instrument, Particles, Imaging Science Experiment, Optical Properties, Radio Science Experiment, Uvs Instrument, Pps Instrument, Density, Width, Ultraviolet Spectrometer, Photopolarimeter Instrument, Precession, Depth, Gaps, Radius, Gravity Effec

Scientific paper

The shapes and kinematics of the Titan and Maxwell ringlets of Saturn's C ring are studied. The ringlets are narrow and eccentric, with mean widths of about 25 km for Titan and abut 64 km for Maxwell, and with eccentricities of order 10 to the -4th. They have sharp edges on a scale of about 1 km, normal optical depths of roughly 0.5-2.0, normal optical depth of the surrounding region, and positive linear width-radius relations. The Titan ringlet is the only feature whose dynamics appears to be completely determined by an external satellite; the kinematics of the Maxwell ringlet are determined solely by Saturn's nonspherical gravity field. The comparatively large measured optical depths and large inferred mass extinction coefficients for the ringlets suggest an environment and particle size distribution different from the remainder of the C ring and presumably caused by the mechanism responsible for ring confinement.

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