HR: 0830h
AN: SM51C-0536    [PDF]
TI: Effects of asymmetric plasmasphere on MHD waves in a three-dimensional dipolar magnetosphere
AU: * Roh, S
EM: myamanda@hanmail.net
AF: Department of Astronomy and Space science, Kyung Hee University, Yongin, Kyunggi, 449-701 Korea, Republic of
AU: Lee, D
EM: dhlee@khu.ac.kr
AF: Department of Astronomy and Space science, Kyung Hee University, Yongin, Kyunggi, 449-701 Korea, Republic of
AU: Denton, R E
EM: Richard.Denton@dartmouth.edu
AF: Physics and Astronomy Department, Dartmouth College, 6127 Wilder Laboratory, Harnover, NH 03755 United States
AU: Takahashi, K
EM: Kazue.Takahashi@jhuapl.edu
AF: Applied Physics Laboratory, Johns Hopkins University, 11100 Johns Hopkins Road, Laurel, Maryland, 20723-6099 United States
AU: Goldstein, J
EM: jerru@hydra.rice.edu
AF: Depratment of Physics and Astronomy, Ms-108, Rice University, 6100 Main Street, Huston TX, 77005-1892 United States
AU: Keiling, A
EM: akeiling@ham.space.umn.edu
AF: Schools of Physics and Astronomy, University of Minnesota, 116 Church Street, S, Minneapolis, MN 55455 United States
AU: King, R A
EM: bob@arizona.edu
AF: Lunar and Planetary Laboratory-West, The University of Arizona, 1040 East Fourth Street Room 901, Tucson, AZ 85721 United States
AU: Yumoto, K
EM: yumoto@geo.kyushu-u.ac.jp
AF: Department of Earth and Planetary Sciences, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka, 812-8581 Japan
AB: The plasmaspheric region shows relatively strong longitudinal asymmetry in the sense that the location of the plasmapause and the density distribution significantly vary with respect to local time, and this asymmetry effect has been neglected in previous magnetospheric ULF wave studies. In this study, we numerically examine the MHD wave properties of field line resonances (FLRs) and Pi2 pulsations when the inner magnetosphere is assumed to be asymmetric. We use the dipole magnetic field model, but our density model is based on observational data from the IMAGE satellite. We assume an impulsive input in the magnetotail, which can be associated with a substorm onset. Our results suggest that local FLRs appear in both the radial and azimuthal oscillations owing to the asymmetry. Plasmaspheric Pi2 signals appear in the compressional component, but they are more strongly affected by ambient plasmaspheric structure than the FLRs. We compare our results with the observational data of Pi2 events.
DE: 2730 Magnetosphere--inner
SC: SPA - Magnetospheric Physics [SM]
MN: 2003 Fall Meeting