By channeling the energy flux from the energy-containing motion below the photosphere to the solar atmosphere, magnetic fields play an important role in the energetics of the chromosphere and of the corona. The mechanical energy which must be supplied at the higher altitudes may have its origin in quasi- steady magnetic fields relaxing themselves via microflares, and/or in waves propogating in the magnetized plasma. Most of the magnetic flux emerges from the sun in high intensity flux tubes. Near the surface of the sun, the flux tubes expand as they reach the solar atmosphere. Previous studies have shown that this expansion strongly affects the equilibrium structure and the observed emission measure. The propagation of magnetohydrodynamic (MHD) waves is also affected by the expansion. A numerical study of these processes in multidimensional geometry will bring a better understanding of the coupling between the photosphere and solar atmosphere, such as e.g., estimates of wave energy output. It is planned to use a previously developed magnetohydrodynamic numerical code with curvilinear coordinates adaptable to the geometrical complexity of the magnetic field and to the strong density stratification. The focus of this study is on the effects of magnetic structures on MHD wave excitation and transfer in the solar atmosphere. These multidimensional results will be compared with the previous one-dimensional estimates as well as with the mechanical energy requirements given by transport models.
