Modified Magnetohydrodynamic Model of Magnetic Reconnection

This paper presents the modified magnetohydrodynamic (MHD) model and simulations of solar wind-magnetosphere interactions. We use the two-dimensional and three-component, compressible, resistive, ion gyroviscous and Hall MHD model, i.e., including the ion finite Larmor radius (FLR) and Hall MHD effects, but neglecting the electron inertia and electron FLR effects. The composed dynamic pressure pulses (shear variations in the flow velocity) in the solar wind form gusts that continually buffet the magnetosphere and cause the time-dependent magnetic reconnection a t the magnetopause. The results show that the magnetic field and the flow velocity components perpendicular to the reconnection plane can be generated in magnetopause current layer. The vortical flow structures can also occur in the magnetospheric side region. These results are responsible for non-ideal MHD properties of the plasma fluid, i.e., ion FLR and Hall MHD effects.