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. The cosmic rays colliding to the Sun are absorbed and the others passing near the Sun bend their orbits due to the solar magnetic field. However, when we detect air showers induced by these protons in the atmosphere, the Sun's shadow, i.e., the deficit on the arrival direction map of air showers, should be observed with a shift of 0.25 degrees. We also found the Sun's shadow moves year by year.