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Coupled flux transport and magneto-frictional simulations are extended tosimulate the continuous magnetic field evolution in the global solar corona forover 15 years, from the start of Solar Cycle 23 in 1996. By simplifying thedynamics, our model follows the build-up and transport of electric currents andfree magnetic energy in the corona, offering an insight into the magneticstructure and topology that extrapolation-based models can not. To enable theseextended simulations, we have implemented a more efficient numerical grid, andhave carefully calibrated the surface flux transport model to reproduce theobserved large-scale photospheric radial magnetic field, using emerging activeregions determined from observed line-of-sight magnetograms. This calibrationis described in some detail. In agreement with previous authors, we find thatthe standard flux transport model is insufficient to simultaneously reproducethe observed polar fields and butterfly diagram during Cycle 23, and thatadditional effects must be added. For the best-fit model, we use automatedtechniques to detect the latitude-time profile of flux ropes and theirejections over the full solar cycle. Overall, flux ropes are more prevalentoutside of active latitudes but those at active latitudes are more frequentlyejected. Future possibilities for space-weather prediction with this approachare briefly assessed.

Coronal Magnetic Field Evolution from 1996 to 2012: Continuous Non-Potential Simulations