  Coupled flux transport and magneto-frictional simulations are extended to
simulate the continuous magnetic field evolution in the global solar corona for
over 15 years, from the start of Solar Cycle 23 in 1996. By simplifying the
dynamics, our model follows the build-up and transport of electric currents and
free magnetic energy in the corona, offering an insight into the magnetic
structure and topology that extrapolation-based models can not. To enable these
extended simulations, we have implemented a more efficient numerical grid, and
have carefully calibrated the surface flux transport model to reproduce the
observed large-scale photospheric radial magnetic field, using emerging active
regions determined from observed line-of-sight magnetograms. This calibration
is described in some detail. In agreement with previous authors, we find that
the standard flux transport model is insufficient to simultaneously reproduce
the observed polar fields and butterfly diagram during Cycle 23, and that
additional effects must be added. For the best-fit model, we use automated
techniques to detect the latitude-time profile of flux ropes and their
ejections over the full solar cycle. Overall, flux ropes are more prevalent
outside of active latitudes but those at active latitudes are more frequently
ejected. Future possibilities for space-weather prediction with this approach
are briefly assessed.
