Topic/Type: 1.1 Space & astrophysical plasmas, Poster
N. Terada1, Y. Matsumoto2, T. Miyoshi3, K. Fukazawa4, T. Umeda2
1 Tohoku University, Sendai, Japan
2 Nagoya University, Nagoya, Japan
3 Hiroshima University, Higashi-hiroshima, Japan
4 Kyushu University, Fukuoka, Japan
High-resolution magnetohydrodynamic (MHD) and multi-fluid simulation codes have been developed based on a semi-discrete central scheme and high-order weighted essentially non-oscillatory (WENO) data reconstruction. The central scheme adopted in these codes is advantageous to solving solar-terrestrial and planetary (STP) problems, because they often include non-MHD effects such as Hall effect, ion FLR effect, and multi-fluid effect, where eigenvalues and eigenvectors of the governing equation system are difficult (or sometimes impossible) to obtain. The central scheme is a Riemann-solver-free approach, and has ability to accurately solve many of the non-MHD problems in the STP problems.
The purposes of this study are twofold: (1) to verify the performance of our newly developed code by comparing the MHD simulation of a planetary magnetosphere with that by high-resolution upwind scheme; and (2) to extend it to an electromagnetic multi-fluid equation system. The multi-fluid simulation is shown to be a powerful method to study non-MHD magnetospheric/ionospheric coupling processes in a planetary magnetosphere.