Abstract

The magnetohydrodynamic (MHD) relaxation process in the solar coronal magnetic field is investigated by using a three-dimensional MHD numerical simulation. Our main objective is to explain the physical mechanisms of solar flares based on bifurcation theory, arguing that the solar flare is a transition process between two different solutions (the coupled solution (CS) and the mixed solution (MS)) of the linear force free field (LFFF) (Kusano et al., 1995). To achieve this, the dynamics of a system of model magnetic loops, periodically aligned on the photosphere, is numerically considered. Magnetic helicity and magnetic energy are assumed to be injected into the coronal region by the rotational motion of the photosphere

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