A self-consistent solar coronal heating model by Alfvenic waves

The relative importance of AC versus DC heating depends on the details of the photospheric driver and on the configuration of the magnetic field.

Moreover, even if AC heating prevails, several wave dissipation mechanisms have been proposed, and which of them dominates remains unclear, as its efficiency depends on plasma compressibility and density inhomogeneity. We address these issues by performing three-dimensional radiative magnetohydrodynamic (MHD) simulations of a coronal loop spanning from the upper convection zone to the corona, which self-consistently capture many relevant physical processes.