Programme by Session

Coupling of fast and Alfven MHD waves occurs naturally in nonuniform media such planetary magnetospheres and the solar corona. Until recently, theory and simulations of the resonant coupling process was confined to 2D. The real word is 3D in nature, and recently 3D simulations have shown that there unexpected features present in 3D that are totally absent in 2D. It is too early to say what the effect of a 3D perspective will have on understanding of coronal and magnetospheric waves, although the theory has already been used to explain the dawn-dusk asymmetry of Field Line Resonances in the Earth's magnetosphere. We shall briefly outline the 3D scenario and its novel features.