MHD mesoscale interactions at the magnetopause and driven reconnection

A brief review of the theoretical development of the planetary dynamo problem and theoretical models of the solar wind-magnetosphere interaction, such as the reconnection, viscous interaction and impulsive penetration models, is given. MHD mesoscale physics in the non-uniform plasma interaction region should be applied in order to understand how the energy of motion of the magnetofluids is transferred into electromagnetic (E-M) energy. A macro-particle description involving compressional and shear Alfvenons has been introduced to give the particle-like behavior of the corresponding MHD waves [Song and Lysak, 1994]. The driven nature of the solar windmagnetosphere interaction and driven reconnection are discussed in terms of the interactions between Alfvenons and between Alfvenons and the ambient magnetic field. A unified model of the solar wind-magnetosphere interaction may be established on the basis of Alfvenon dynamics.