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Seven different models are applied to the same problem of simulating theSun's coronal magnetic field during the solar eclipse on 2015 March 20. All ofthe models are non-potential, allowing for free magnetic energy, but theassociated electric currents are developed in significantly different ways.This is not a direct comparison of the coronal modelling techniques, in thatthe different models also use different photospheric boundary conditions,reflecting the range of approaches currently used in the community. Despite thesignificant differences, the results show broad agreement in the overallmagnetic topology. Among those models with significant volume currents in muchof the corona, there is general agreement that the ratio of total to potentialmagnetic energy should be approximately 1.4. However, there are significantdifferences in the electric current distributions; while static extrapolationsare best able to reproduce active regions, they are unable to recover shearedmagnetic fields in filament channels using currently available vectormagnetogram data. By contrast, time-evolving simulations can recover thefilament channel fields at the expense of not matching the observed vectormagnetic fields within active regions. We suggest that, at present, the bestapproach may be a hybrid model using static extrapolations but with additionalenergization informed by simplified evolution models. This is demonstrated byone of the models.

Global Non-Potential Magnetic Models of the Solar Corona During the March 2015 Eclipse