HR: 1340h
AN: SM43A-1218    [Abstracts]
TI: Bifurcation of 3D Vector Field Topology in Magnetospheric Dynamics
AU: * Cai, D
EM: cai@is.tsukuba.ac.jp
AF: University of Tsukuba, CS, Tsukuba, 305-8573 Japan
AU: Li, W
EM: liwei@aoi3.cs.tsukuba.ac.jp
AF: University of Tsukuba, CS, Tsukuba, 305-8573 Japan
AU: Nishikawa, K
EM: ken-Ichi.Nishikawa@nsstc.nasa.gov
AF: National Space Science and Technology Center, 320 Sparkman Drive, Huntsville, AL 35805 United States
AU: Lembege, B
EM: lembege@cetp.ipsl.fr
AF: CETP/UVSQ/IPSL, 10-12 Avenue de l'Europe, Velizy, FR-78140 France
AB: The 3D magnetospheric plasma flows and magnetic fields produced by global PIC simulations are often very complex and difficult to understand. In order to make sense of the vast amount of information that a vector field can carry, we present some important topological features and concepts that can be used to get a glimpse of _gwhat a vector field is doing_h. Field topology visualization is an important technique to represent the important aspects of the vector field topology. This technique has enabled space physicists to visualize the complex nature of magnetospheric dynamics globally. If we consider magnetic vector field depends on an additional parameter, the structure of the phase portrait (field topology) may transform as the value of this parameter evolves. This change is called bifurcation and brings the topology from stable state to another. We discuss how bifurcation occurs increasing IMF. We also discuss the structural stability of the magnetospheric dynamics.
UR: http://www.coins.tsukuba.ac.jp/_`cai/ICNSP_2005-topology_18_07_10.ppt
DE: 2723 Magnetic reconnection (7526, 7835)
DE: 2753 Numerical modeling
DE: 2784 Solar wind/magnetosphere interactions
DE: 2790 Substorms
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005