Abstract

The seminar will describe recent attempts to model magnetic fields in the solar corona using the non-linear force-free approximation. To begin with a new global model which is based on observational data will be described. The model is designed to simulate the large-scale evolution of photospheric and coronal magnetic fields on the Sun over long periods of time (weeks-months).Once the construction of the model is discussed two tests of the model are carried out. First it is tested with observations of the hemispheric pattern of solar filaments and secondly with IMF measurements of the Sun’s Open Flux. Following on from this non-linear force-free simulations are carried out of the dispersal of an active region. Results show that small scale convective motions may provide sufficient energy to explain the radiative losses in the corona. Finally future applications of the model will be discussed.