The Role of MHD Waves in Coronal Heating

We will examine the effect of chromospheric evaporation occurring at the footpoints of a coronal loop. This will be achieved with a 2.5-D simulation using the Lare2d code to solve the set of MHD equations. The coronal loop is modelled as a 'straight loop', initially in a magnetohydrostatic equilibrium. This 'straight loop' model is justified by the small aspect ratio of observed coronal loops. The coronal loop is modelled as an area of enhanced density compared to the surrounding coronal plasma. The chromosphere is modelled as an area of enhanced density when compared with the coronal region. We will then examine the propagation and dissipation of Alfvén waves in this basic model. We will consider a range of different periods for the driver as well as different amplitudes and location of the wave excitation.

I am following the University of St Andrews' induction plan for new PGR students. Alongside this I will be following a course of directed reading and computational skills/projects organised by the School of Mathematics and Statistics.