Magnetic Effects in the Sun's Corona and Interior

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The solar magnetic field is cyclical in time and intermittent in space. The field plays a basic role in the formation of the Sun's hot outer corona and in the twenty two year activity cycle. This study will investigate magnetic phenomena on the Sun which range from probing the interior field using helioseismology to studying the evolution of the field in the corona, including the generation of waves and the acceleration of particles in solar flares. The helioseismology studies will help to elucidate the structure and temporal behavior of the magnetic field in the solar interior. The investigation of coronal magnetic field evolution will focus on the formulation of singularities and the loss of equilibrium, which are important for understanding both steady state coronal heating and eruptive phenomena such as flares and mass ejections. The particle acceleration studies will focus on the generation of hydromagnetic disturbances during the flare process and on simulations of particle interaction with these waves. The latter should have application to acceleration in a wide range of environments in addition to solar flares. Both analytical and numerical techniques based on prior studies will be employed.