Saturn's Magnetosphere During Cassini's Approach and Initial Orbit

HR: 14:35h
AN: P53B-04 [Abstracts]
TI: Saturn's Magnetosphere During Cassini's Approach and Initial Orbit
AU: * Hansen, K C
EM: kenhan@umich.edu
AF: University of Michigan, 1411D Space Research Bldg., Ann Arbor, MI 48109-2143
AU: Clarke, J T
AF: Boston University, Center for Space Physics Boston University 725 Commonwealth Ave, Boston, MA 02215
AU: Crary, F J
AF: Southwest Research Institute, 6220 Culebra Road P.O. Box 28510, San Antonio, TX 78228-0510
AU: De Zeeuw, D L
AF: University of Michigan, 1411D Space Research Bldg., Ann Arbor, MI 48109-2143
AU: Dougherty, M
AF: Imperial College, H/707 Huxley Building South Kensington campus, London, SW7 2AZ
AU: Gurnett, D A
AF: University of Iowa, 203ÿVanÿAllenÿHall, Iowa City, IA 52242-1479
AU: Gombosi, T I
AF: University of Michigan, 1411D Space Research Bldg., Ann Arbor, MI 48109-2143
AU: Hospodarsky, G
AF: University of Iowa, 203ÿVanÿAllenÿHall, Iowa City, IA 52242-1479
AU: Kurth, W S
AF: University of Iowa, 203ÿVanÿAllenÿHall, Iowa City, IA 52242-1479
AU: Ridley, A J
AF: University of Michigan, 1411D Space Research Bldg., Ann Arbor, MI 48109-2143
AU: Young, D T
AF: Southwest Research Institute, 6220 Culebra Road P.O. Box 28510, San Antonio, TX 78228-0510
AB: We present results of a 3D global magnetohydrodynamic (MHD) model of the Saturnian system during Cassini's approach to Saturn and its initial orbit. During approach Cassini made measurements of the solar wind conditions upstream of Saturn while at the same time HST measurements were made of the Saturnian aurora and remote sensing measurements of the Saturn Kilometric Radiation (SKR) were made. Using both Cassini data and data propagated from Earth as input to our MHD model, we examine the state of the magnetosphere-ionosphere system for this period. In addition we examine the correlations between remote sensing measurements and the simulations. During orbital insertion and its initial orbit, Cassini measured several crossings of the bow shock and magnetopause of Saturn. Several of these crossing would not have been predicted by Voyager era measurements. Using our MHD model we examine the structure and location of these boundaries and compare them with locations measured by Voyager. Our MHD model includes all the major factors that influence the Kronian magnetosphere: solar wind IMF, planetary rotation, ionospheric conductivities, plasma mass loading and the magnetospheric interaction with Titan.
DE: 5737 Magnetospheres (2756)
DE: 6275 Saturn
DE: 2753 Numerical modeling
DE: 2756 Planetary magnetospheres (5443, 5737, 6030)
DE: 2784 Solar wind/magnetosphere interactions
SC: Planetary Sciences [P]
MN: 2004 AGU Fall Meeting