The Phoebe dust ring as seen as by the Cassini dust detector CDA

Details The Phoebe dust ring as seen as by the Cassini dust detector CDA The Phoebe dust ring as seen as by the Cassini dust detector CDA

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p13b1673k&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P13B-1673

Physics

[5420] Planetary Sciences: Solid Surface Planets / Impact Phenomena, Cratering, [5465] Planetary Sciences: Solid Surface Planets / Rings And Dust, [6280] Planetary Sciences: Solar System Objects / Saturnian Satellites

Scientific paper

Saturn's outermost moon Phoebe has been suggested to be the source of a gigantic diffuse dust extending from Phoebe's to Iapetus' orbital distance. Ejecta particles produced by hypervelocity impacts of interplanetary meteoroids with Phoebe are proposed to slowly migrate inward and eventually strike Iapetus' surface. Because of the similarities between the dark surfaces of Phoebe and Iapetus,, the putative Phoebe ring would naturally explain the pronounced colour dichotomy of Iapetus. About 20 days before Cassini's entry into its orbit around Saturn in 2004, the spacecraft performed a close Phoebe flyby, which has been optimised for detecting ejecta particles released from the moon's surface. The CDA measurements provide an upper constraint for the rate at which Phoebe can resupply a ring with fresh dust. After the flyby Cassini moved within the ring's symmetry plane. Dust data acquired during this early mission phase provide information about the size distribution and number density of Phoebe ring particles. To this aim we reanalysed the dust data obtained during the second half of 2004. Our analysis suggests that the ring must be populated by grains in excess of 40 micron in radius, if the ring is composed of Phoebe ejecta moving in retrograde orbits.

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