A numerical model of the Uranian dust rings

Details A numerical model of the Uranian dust rings A numerical model of the Uranian dust rings

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990icar...86..530c&link_type=abstract

Icarus (ISSN 0019-1035), vol. 86, Aug. 1990, p. 530-560.

Astronomy and Astrophysics

Astronomy

40

Astronomical Models, Markov Chains, Micrometeoroids, Regolith, Uranus Rings, Voyager Project, Mathematical Models, Planetary Atmospheres, Planetary Structure

Scientific paper

The present numerical simulations of the Uranian rings discovered by Voyager 2 indicate that they may be the visible component of low optical depth moonlet belts made up of 10 to 100,000 cm objects; these objects would serve as the sources of dust, via both micrometeoroid bombardment and the collisional release of ejecta. It is proposed that the dust bands are generated by continuous ejection and reabsorption of micron-scale regolith material within the hypothesized moolet belts, and it is noted that numerical simulations of such a system in a Markov-chain formalism can reproduce Uranian dust ring characteristics.

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