Testing Alfvén wave propagation in a "realistic" set-up of the solar atmosphere
arXiv:1806.08166 · doi:10.1080/03091929.2019.1672676
Abstract
We present a radiative magneto-hydrodynamic simulation set-up using the PENCIL CODE to study the generation, propagation and dissipation 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 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.
19 pages, 8 figures, 1 table
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