Data-Driven Simulations of Coronal Magnetic Fields: A First Attempt with SDO Data

We present results from numerical simulations of coronal field evolution in response to photospheric driving. In the simulations, the coronal field evolves according to magnetofriction, which ensures that the model field evolves toward a non-linear force-free state. Unlike static field extrapolation methods, this approach takes into account the history of the photospheric field evolution. This allows for the formation of flux ropes as well as current sheets between magnetic domains of connectivity. Using time sequences of HMI magnetograms as the bottom boundary condition, we apply this method to model the emergence and evolution of recent active regions. For the case of AR 11066, flux cancellation between opposite polarities within the AR leads to the formation of a flux rope, which subsequently lifts off. Comparisons of the models with AIA observations will be presented.