HR: 1340h
AN: SM13B-1220    [Abstracts]
TI: Particle entry through "Sash" groove simulated by Global 3D Electromagnetic Particle code with duskward IMF By
AU: * Yan, X
EM: yxy@aoi3.is.tsukuba.ac.jp
AF: Inst. Infor. Sci., University of Tsukuba, 1-1-1 Ten-nou-dai, Tsukuba, 305-8573 Japan
AU: Cai, D
EM: cai@cs.tsukuba.ac.jp
AF: Inst. Infor. Sci., University of Tsukuba, 1-1-1 Ten-nou-dai, Tsukuba, 305-8573 Japan
AU: Nishikawa, K
EM: Ken-Ichi.Nishikawa@nsstc.nasa.gov
AF: National Space Science and Technology Center, 320 Sparkman Drive, SD 50,, 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: We made our efforts to parallelize the global 3D HPF Electromagnetic particle model (EMPM) for several years and have also reported our meaningful simulation results that revealed the essential physics involved in interaction of the solar wind with the Earth's magnetosphere using this EMPM (Nishikawa et al., 1995; Nishikawa, 1997, 1998a, b, 2001, 2002) in our PC cluster and supercomputer(D.S. Cai et al., 2001, 2003). Sash patterns and related phenomena have been observed and reported in some satellite observations (Fujumoto et al. 1997; Maynard, 2001), and have motivated 3D MHD simulations (White and al., 1998). We also investigated it with our global 3D parallelized HPF EMPM with dawnward IMF By (K.-I. Nishikawa, 1998) and recently new simulation with dusk-ward IMF By was accomplished in the new VPP5000 supercomputer. In the new simulations performed on the new VPP5000 supercomputer of Tsukuba University, we used larger domain size, $305\times205\times205$, smaller grid size ($\Delta$), $0.5R_{\rm E}$(the radium of the Earth), more total particle number, 220,000,000 (about 8 pairs per cell). At first, we run this code until we get the so-called quasi-stationary status; After the quasi-stationary status was established, we applied a northward IMF ($B_{\rm z}=0.2$), and then wait until the IMF arrives around the magnetopuase. After the arrival of IMF, we begin to change the IMF from northward to duskward (IMF $B_{\rm y}=-0.2$). The results revealed that the groove structure at the day-side magnetopause, that causes particle entry into inner magnetosphere and the cross structure or S-structure at near magneto-tail are formed. Moreover, in contrast with MHD simulations, kinetic characteristic of this event is also analyzed self-consistently with this simulation. The new simulation provides new and more detailed insights for the observed sash event.
UR: http://www.coins.tsukuba.ac.jp/~cai/Sash.mov
DE: 2716 Energetic particles, precipitating
DE: 2753 Numerical modeling
DE: 2784 Solar wind/magnetosphere interactions
DE: 2788 Storms and substorms
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting