SOLARNET Conference: The Many Scales of the Magnetic Sun

Quasi-static modelling of the Sun’s corona using the magneto-frictional approximation makes predictions of how its large-scale magnetic structure might vary over the solar cycle. Unlike the traditional potential field source surface model, this approach is able to probe the effects of low coronal electric currents and the corresponding free magnetic energy. In particular, ongoing footpoint shearing and flux cancellation lead to the concentration of free energy within closed-field regions, naturally forming sheared arcades and magnetic flux ropes. I will show model results for Cycle 24 driven by magnetogram data from SDO/HMI, with the aim of comparing to earlier results from a decade ago for Cycle 23. In particular, we will consider how solar flux ropes and their eruptions vary over the solar cycle, at least according to this model.