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

HR: 1340h
AN: P43A-0951 [Abstracts]
TI: Observation of the Spectrum and Angular Distribution of Trapped Protons in Saturn's Inner Magnetosphere: Implications for Sources, Transport, and Loss
AU: * Armstrong, T
EM: armstrong@ftecs.com
AF: Fundamental Technologies, LLC, 2411 Ponderosa Drive Suite A, Lawrence, Ks 66046 United States
AU: Manweiler, J
EM: manweiler@ftecs.com
AF: Fundamental Technologies, LLC, 2411 Ponderosa Drive Suite A, Lawrence, Ks 66046 United States
AU: Krupp, N
P43A-0951 AF: MPI f〉 Sonnensystemforschung, Katlenburg-Lindau, Katlenburg-Lindau, 37191 Germany
AU: Lagg, A
P43A-0951 AF: MPI f〉 Sonnensystemforschung, Katlenburg-Lindau, Katlenburg-Lindau, 37191 Germany
AU: Krimigis, S
P43A-0951 AF: The Johns Hopkins University Applied Physics Laboratory, Johns Hopkins Road, Laurel, Md 20723 United States
AU: Livi, S
P43A-0951 AF: The Johns Hopkins University Applied Physics Laboratory, Johns Hopkins Road, Laurel, Md 20723 United States
AU: Mitchell, D
P43A-0951 AF: The Johns Hopkins University Applied Physics Laboratory, Johns Hopkins Road, Laurel, Md 20723 United States
AU: Roelof, E
P43A-0951 AF: The Johns Hopkins University Applied Physics Laboratory, Johns Hopkins Road, Laurel, Md 20723 United States
AU: Paranicas, C
P43A-0951 AF: The Johns Hopkins University Applied Physics Laboratory, Johns Hopkins Road, Laurel, Md 20723 United States
AU: Hamilton, D
P43A-0951 AF: Department of Physics University of Maryland, University of Maryland, College Park, Md. 20742
AB: 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.
DE: 2756 Planetary magnetospheres (5443, 5737, 6033)
DE: 5737 Magnetospheres (2756)
DE: 6280 Saturnian satellites
SC: Planetary Sciences [P]
MN: Fall Meeting 2005