HR: 1340h
AN: SM13B-0345    [Abstracts]
TI: An MHD Simulation Study of the Effects of IMF By and Dipole Tilt on the Configuration and Dynamics of Jupiter's Magnetosphere
AU: * Fukazawa, K
EM: fukazawa@stelab.nagoya-u.ac.jp
AF: Solar-Terrestrial Environment Laboratory, Nagoya University, Honohara 3-13, Toyokawa, 4428507 Japan
AU: Ogino, T
EM: ogino@stelab.nagoya-u.ac.jp
AF: Solar-Terrestrial Environment Laboratory, Nagoya University, Honohara 3-13, Toyokawa, 4428507 Japan
AU: Walker, R J
EM: rwalker@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, University of California, Los Angeles, 6843 Slichter Hall, Los Angeles, CA 90095-1567 United States
AB: Jupiter_fs rapidly rotating magnetosphere differs greatly from the Earth's magnetosphere. At the Earth magnetospheric dynamics primarily are driven by the solar wind. At Jupiter the magnetosphere is determined by a complex interaction between atmospherically driven corotation, the plasma source in the Io torus, and the solar wind. These processes are still not fully understood. In previous studies we used a three-dimensional global magnetohydrodynamic simulation to investigate the response of Jupiter_fs magnetosphere to changes in solar wind dynamic pressure and the north-south component of the interplanetary magnetic field (IMF). In this study we will expand on those results by including the effects of IMF By and dipole tilt. For northward IMF we found that the Jovian magnetotail was highly unstable. In particular plasmoids (magnetic O-type neutral lines) were periodically ejected down the tail at intervals similar to those of the periodic flow bursts observed by the Galileo Energetic Particle Detector (EPD). However, when we included a By component along with the northward IMF in the simulation the configuration changed dramatically. The periodic tailward injections were replaced by a complex spatially dependent neutral line which stayed fixed in space. Instead of large scale plasmoids that encompassed a large part of the tail a series of smaller localized plasmoid like structures formed across the tail. In this talk we will discuss the effects of IMF By and present the first results including dipole tilt in the simulation. In addition to comparing the results in the magnetotail for the various simulations we also will examine the energy flux to the ionosphere.
DE: 2756 Planetary magnetospheres (5443, 5737, 6033)
DE: 2784 Solar wind/magnetosphere interactions
DE: 4255 Numerical modeling (0545, 0560)
DE: 6220 Jupiter
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005