Oscillatory and radiative properties of solar magnetic flux concentrations

Photospheric magnetic field structures, such as sunspots, are important visible markers of the Suns activity. Computational modelling of wave motions is used to investigate the structure of these magnetic fields. To directly compare our simulation results to satellite measurements we calculate the radiation spectrum that would be observed. We apply these techniques to two topics. Firstly, we identify the observational signatures of fast-to-slow mode conversion of sound waves in a sunspot and analyse the implications for helioseismology. Secondly, we study the observational manifestation of Alfvén waves in intergranular flux concentrations and investigate their potential to heat the solar chromosphere.