Fredagskollokvium: Analysis of radiation-MHD simulations of the solar atmosphere

The solar atmosphere is very complex and consists of a number of different physical regimes. Highly efficient massively parallel numerical codes are needed to solve the associated equations. We use the Bifrost stellar atmosphere code to perform 3D radiation MHD simulations of the solar atmosphere above a quiet Sun region.The focus of this study is on flows between the chromosphere and corona. We will investigate the temporal evolution of magnetic field structures extending from the convection zone to the corona and their underlying dynamics. By adding tracer particles to the simulation, we are able to follow the magnetic field lines properly and to investigate the generation and propagation of waves travelling into the corona. By tracking the evolution of the observed perturbations in time, we can provide new insights on the physical processes driving them and on their role in the chromosphere-corona mass cycle.