Keiichiro FUKAZAWA in Kyoto Univ.
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We develop the massively parallel numerical simulation codes of Terrestrial, Jovian and Kronian magnetospheres. If you have questions, please ask me.
|Equatorial radius [km]||6,378||71,492||60,268|
|Dipole magnetic field [nT]||31,000||420,000||21,000|
|Rotation period [days]||0.997||0.414||0.444|
Figure 1. Jovian magnetosphere [Bagenal et al., 2004]
We use a three-dimensional MHD code, which has been used for studies on global structures and dynamics of planetary magnetospheres [Ogino et al., 1992, Fukazawa et al., 2012]. The MHD code uses the “Modified Leapfrog” method (MLF), in which partial difference equations are solved by the two-step Lax-Wendroff method for one time step and then by the Leapfrog scheme for (l-1) time steps and the procedure is repeated. Detailed explanation of MLF is in our previous paper [Fukazawa et al., 2014].
Figure 2. Simulation result of Terrestrial magnetosphere
Figure 3. Direction of plasma flow in the equatorial plane [Woch et al., 2002]
Figure 4. Evolution of magnetic plasmoid in the meridian plane [Fukazawa et al., 2005]
Figure 5. Periodic plasmoid ejection in the equaotrial plane [Fukazawa et al., 2005]
Figure 6. The temperature and flow vectors in the equatorial plane for the simulation with no IMF (a), southward (b) and northward IMF (c) [Fukazawa et al., 2005]
Figure 7. The magnetic field connection from the polar region to the magnetosphere [Fukazawa et al., 2012]
Figure 7. Domain decomposition [Fukazawa et al., 2010]
Figure 8. Effective performance of SR16000/L2 [Fukazawa et al., 2010]
ACE project（CREST, PI: Dr. Nanri@Kyushu Univ.）
PomPP project (CREST, PI: Dr. Kondo@Univ. of Tokyo）
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