Coupling Photosphere and Corona: Linear and Turbulent Regimes
Résumé
In numerical modeling, corona is often stuck directly on the photosphere where movements are prescribed, thus fully reflecting Alfven waves running along closed loops. In reality, reflection is not complete. We consider here for the first time the combined effects of finite reflection and turbulence which both control the coronal magnetic energy injected by the photospheric velocity shear. The loop model used is that of linear Alfven wave propagation along a 1D loop model, defined by a piece-wise constant Alfven speed (chromosphere and corona), and a turbulence shell model in the perpendicular direction.