  We present a radiative magneto-hydrodynamic simulation set-up using the
PENCIL CODE to study the generation, propagation and dissipation of Alfv\'en
waves in the solar atmosphere which includes a convective layer, photosphere
below and chromosphere, transition region and the corona above. We prepare a
setup of steady-state solar convection where the imposed external magnetic
field also has reached the final value gradually starting from a very small
value. From that state, we start several simulations by varying the magnetic
Prandtl number and the forcing strengths. We find the propagation
characteristics of waves excited in this simulation run depend strongly on the
magnetic Prandtl number and the wave number of the forcing. For magnetic
Prandtl number of unity, we obtain localized heating in the corona due to shock
dissipation.
