Evidence of Enceladus and Tethys microsignatures

Details Evidence of Enceladus and Tethys microsignatures Evidence of Enceladus and Tethys microsignatures

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005georl..3220101p&link_type=abstract

Geophysical Research Letters, Volume 32, Issue 20, CiteID L20101

Physics

10

Planetary Sciences: Solar System Objects: Saturnian Satellites, Planetary Sciences: Solar System Objects: Saturn, Magnetospheric Physics: Planetary Magnetospheres (5443, 5737, 6033), Planetary Sciences: Solid Surface Planets: Interactions With Particles And Fields, Magnetospheric Physics: Energetic Particles: Precipitating

Scientific paper

We present evidence of two icy satellite microsignatures in the Cassini LEMMS data. Just upstream of Enceladus, a deep and narrow decrease in the flux of several MeV electrons is consistent with a recent absorption by that moon. This microsignature is collocated with a deep depletion in the MeV proton flux. The proton feature is much wider than the satellite diameter, suggesting multiple interactions and/or losses to the E Ring and neutral gas. An observed increase in proton flux toward the planet suggests a possible inner magnetospheric source. A decrease in the low energy electron intensity downstream of Tethys is also consistent with a microsignature approximately the size of the satellite that has drifted slightly toward the planet near midnight. Modeling suggests that microsignatures near Tethys' orbit would persist for more than a complete rotation of Saturn and the radial diffusion coefficient is about 10-9 RS2/s.

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