Modeling the Evolution of Solar Magnetic Fields

Abstract

The solar atmosphere is a laboratory for studying complicated physical processes. The Magneto-Hydro-Dynamic (MHD) equations is the simplest theoretical approach that captures the complicated dynamical interaction between plasma and magnetic fields. These equations are therefore widely used for investigating the dynamical processes that takes place in the solar atmosphere. The MHD equations can also be used to provide information about the field line structure of the coronal magnetic field. Knowledge of the magnetic field topology is required before we can understand where the magnetic field tends to liberate it’s free energy. To fully understand the energy release process, magnetic reconnection and wave dissipation processes have to be understood in detail. The MHD equations can also provide information about temperature profile along loops that are heated by, both static and time depend, heating profiles. This paper gives a review of magnetic reconnection, the basic idea behind magnetic field extrapolation, and the problems related to using temperature profiles for determining the underlying heating profile. A full understanding and utilisation of all of these disciplines within solar physics MHD is required to significantly advance our knowledge of the dynamical solar corona.