Observation of the Spectrum and Angular Distribution of Trapped Protons in Saturn's Inner Magnetosphere: Implications for Sources, Transport, and Loss

Details Observation of the Spectrum and Angular Distribution of Trapped Protons in Saturn's Inner Magnetosphere: Implications for Sources, Transport, and Loss Observation of the Spectrum and Angular Distribution of Trapped Protons in Saturn's Inner Magnetosphere: Implications for Sources, Transport, and Loss

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p43a0951a&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #P43A-0951

Physics

2756 Planetary Magnetospheres (5443, 5737, 6033), 5737 Magnetospheres (2756), 6280 Saturnian Satellites

Scientific paper

The Cassini MIMI investigation carried a set of solid state detectors designed in part to resolve the shape and magnitude a local minimum in the flux of energetic protons at about 10 MeV reported from the Voyager 2 flyby in 1981. Preliminary results from Cassini Saturn Orbit Injection (SOI) show that this reported feature of the proton spectrum has persisted throughout the region within Dione's orbit . We will report the fluxes, pitch angle distributions, and phase space densities along with our estimates of source and loss processes of Saturnian trapped protons. Further, we will attempt to reconcile our results with those from Voyagers 1 and 2 and Pioneer 11, especially regarding the inner "CRAND" source.

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