Their relative acceleration and slowing down were found. MHD wave propagations due to footpoint motions in the photosphere. The profiles for density, magnetic field and driver are considered to be steep. The numerical simulation presents the evolution of MHD waves. The resonance layer is clearly observed at the slab edges.
Dissipation takes place around the resonance layer where the perturbation develops large gradients.
The width of the resonance layer is calculated. It is observed that the thickness of the Alfven resonance layer is more that that of the slow wave resonance layer. Effort is made to distinguish between slow and Alfven wave resonance layers. Fast waves develop kink instability. As plasma evolves the current sheets which provide the heating at the edges gets distorted and fragment into two current sheets at each edge which, in turn come closer when the twist is enhanced.