``Fingerprints'' of the size-distribution in planetary rings

Details ``Fingerprints'' of the size-distribution in planetary rings ``Fingerprints'' of the size-distribution in planetary rings

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dps....32.4910s&link_type=abstract

American Astronomical Society, DPS Meeting #32, #49.10; Bulletin of the American Astronomical Society, Vol. 32, p.1090

Astronomy and Astrophysics

Astronomy

Scientific paper

We extend the Markov-model of gravitational scattering by moonlets in planetary rings to viscous diffusion. The latter process counteracts the generation of structures due to the larger ring-boulder. As a result two types of steady state patterns evolve: i) a ``propeller'' shaped structure for moonlets D < 1km in size ii) a circumferential gap (+ringlet) for larger moonlets. The radial and the azimuthal extent scale with the Diameter D of the moonlet [radial: D (for D < 3 km in diameter) or D2 (for D> 3 km); azimuthal: (D3)/(ν ), with ν - kinematic viscosity]. In this way the size distribution and also the viscous properties of the ring matter could be probed by the high resolution images of the Cassini spacecraft in the near future.

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