HR: 0800h
AN: P51A-1411    [Abstracts]
TI: SATURN'S GLOBAL ION DISTRIBUTION FROM CASSINI/INCA ENA AND IN-SITU MEASUREMENTS
AU: * Brandt, P C
EM: pontus.brandt@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Saur, J
EM: joachim.saur@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Mitchell, D G
EM: donald.mitchell@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Roelof, E C
EM: edmond.roelof@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Paranicas, C P
EM: christopher.paranicas@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Mauk, B H
EM: barry.mauk@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Krimigis, S M
EM: stamatios.krimigis@jhuapl.edu
AF: The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723 United States
AU: Krupp, N
EM: krupp@linmpi.mpg.de
AF: Max Planck Institut fur Sonnensystemforschung, Max Planck Strasse 2, Katlenburg-Lindau, D-37191 Germany
AB: The Saturn Orbit Insertion (SOI) of Cassini took place on 1 July 2004. The Ion and Neutral Camera (INCA) obtained global energetic neutral atom (ENA) images of the magnetosphere during 1-2 July, while the LEMMS detector obtained {\it in-situ} ion and electron intensities and pitch-angle distributions. Since Cassini made a cut through the morning (inbound) and post-midnight (outbound) sector, we have enough information to use the INCA images and LEMMS in situ intensities to constrain the global ion distribution using simulations with a parametrized model adapted from Roelof and Skinner [2000]. The model for the neutral gas distribution was adapted from Richardson [1998]. From the ENA images, the ion distribution appeared to peak on the nightside, while the LEMMS ion and electron intensities displayed two strong peaks between 3 to 8 RS on both the inbound and outbound passes, with the outbound pass displaying stronger intensities. The LEMMS pitch-angle distributions exhibited clear depletions around 90 deg within these regions, consistent with ion/gas interactions contributing to the minima between the intensity peaks. Additional resolved ENA images and in situ intensities will be obtained after the first close Titan flyby (Ta) on 26 October 2004.
UR: http://sd-www.jhuapl.edu/CASSINI/
DE: 2720 Energetic particles, trapped
DE: 2730 Magnetosphere--inner
DE: 2740 Magnetospheric configuration and dynamics
DE: 2756 Planetary magnetospheres (5443, 5737, 6030)
DE: 2778 Ring current
SC: Planetary Sciences [P]
MN: 2004 AGU Fall Meeting