Abstract:
We present a radiative magneto-hydrodynamic simulation set-up
using the pencil code to study the generation, propagation and dis-
sipation of Alfvén waves in the solar atmosphere which includes a
convective layer, photosphere below and chromosphere, transition
region and the corona above. We prepare a set-up 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 propaga-
tion 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
localised heating in the corona due to shock dissipation.
