A new multi-fluid code for solar coronal plasma simulations

Physics – Fluid Dynamics

Scientific paper

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7526 Magnetic Reconnection (2723, 7835), 7827 Kinetic And Mhd Theory, 7829 Kinetic Waves And Instabilities, 7833 Mathematical And Numerical Techniques (0500, 3200), 7859 Transport Processes

Scientific paper

Multi-fluid dynamics of plasma is more complex than MHD because the ion and electron motions need not be identical. The multi-fluid model takes into account electron inertia, charge separation and the full electromagnetic field equations and allows for separate electron and ion motion. Temperature anisotropy effects are taken into account by self consistently evolving the anisotropic pressure tensor. We adopt central semi-discrete finite volume scheme to evolute dynamics of each plasma species. This algorithm allows to incorporate source terms (e.g. Lorentz force) without operator splitting method. Extended stencil discretization have been used for the Maxwell equations. This method results in isotropic al representation of electromagnetic waves and keeps divergence of magnetic field constant. Presented multi-fluid-Maxwell code is applied to study of driven magnetic reconnection. Magnetic reconnection driven by plasma flow is observed in various plasma systems such as solar flares, earth's magnetosphere and laboratory plasma. We have studied the the process collisionless reconnection resulting from charge separation effects. The comparison of the results of full multi-fluid reconnection with Hall-MHD simulation have shown that velocity difference of ions and electrons from the multi-fluid simulation is large than that from Hall-MHD. This is because in Hall MHD electrons move with ions along the direction of local magnetic, but for perpendicular direction electron can move separately and generate the so called Hall current. So multi-fluid simulation demonstrates more precise physics than Hall MHD.

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