Modelling Elementary Coronal Heating Events

点击翻译按钮获取中文摘要

The convective driving of the photosphere can generate a Poynting Flux into the solar atmosphere that is sufficient to power coronal heating. A driver that is slow in comparison to the local Alfvén speed will build stresses in the atmospheric magnetic field, which can be released during reconnection events. A faster driver on the other hand, will lead to wave motions. Using the numerical code Lare3D, we plan to develop coronal models that considers the effects of continuous driving on (sets of) magnetic flux-tubes. We will include thermal conduction to determine how heat is re-distributed and consider its effects on both the plasma and the magnetic field. Further we investigate the magnitude of radiative cooling on the heating timescale in order to help establish the efficacy of the proposed heating mechanism. Forward modelling will be used to derive observables for current and future instrumentation.Training -+ University wide induction for new PhD students+ University induction sessions for new tutors+ St Andrews Solar Group induction programme consisting of guided reading and 3 mini projects during the first 3 months+ Solar Group weekly seminar programme+ Course on MPI