Magnetohydrodynamics (MHD) describe the dynamics of conducting fluids by means of hydrodynamic and magnetic forces. The solar corona, the subject of research in this thesis, consists of plasma and is hence examined by MHD simulations based on measurements of the heliospheric and magnetic imager (HMI). These imagers obtain magnetic field data from the photosphere, the ßurface" of the Sun. There are multiple fields which exist in the context of MHD. This thesis will concentrate on the three main fields: the magnetic, plasma velocity and the current density fields. The thesis first describes the methods needed to parse and precompute the data, the assumptions behind the simulation, as well as the HDF data format. In the main part, several visualization approaches are presented, including a method to analyze the advection property of the magnetic field, an analysis of the fields' shapes, followed by the interrelations between them on global as well as local scale.