Evolution of Jupiter's Main Ring

Details Evolution of Jupiter's Main Ring Evolution of Jupiter's Main Ring

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....12925e&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #12925

Computer Science

Scientific paper

Voyager and Galileo observations constrain the size distribution of the Jovian main ring. Brooks etal 2003 matched the phase curves and spectra with a broken power law for the size distribution. This distribution can be explained as the result of erosion of an initially steeper size distribution, which was the outcome from disruption of a parent body. The smaller ring particles are more rapidly lost, giving an estimate for the time since the disruption of about 1000 years. The differences in brightness reported for the far arm compared to the near arm are not associated with magnetic longitude, viewing direction or phase angle. The asymmetries seen may be best explained by random collisions, as in the model of the Saturn F ring by Barbara and Esposito (2002). Radial transport of small particles in the ring is so rapid that little is swept up by the parent bodies after release, and these maternal bodies have likely very thin regoliths, if any. The radial distribution of ring material seen at high phase angle is not easily interpreted as dust knocked off of the parent bodies in steady state. More complicated models will be discussed.

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