  The large field-of-view of the Sun Watcher using Active Pixel System detector
and Image Processing (SWAP) instrument on board the PRoject for Onboard
Autonomy 2 (PROBA2) spacecraft provides a unique opportunity to study extended
coronal structures observed in EUV in conjunction with global coronal magnetic
field simulations. A global non-potential magnetic field model is used to
simulate the evolution of the global corona from 1 September 2014 to 31 March
2015, driven by newly emerging bipolar active regions determined from
Helioseismic and Magnetic Imager (HMI) magnetograms. We compare the large-scale
structure of the simulated magnetic field with structures seen off-limb in SWAP
EUV observations. In particular, we investigate how successful the model is in
reproducing regions of closed and open structures; the scale of structures; and
compare the evolution of a coronal fan observed over several rotations. The
model is found to accurately reproduce observed large-scale off-limb
structures. When discrepancies do arise they mainly occur off the east solar
limb due to active regions emerging on the far side of the Sun, which cannot be
incorporated into the model until they are observed on the Earth-facing side.
When such ``late'' active region emergences are incorporated into the model, we
find that the simulated corona self-corrects within a few days, so that
simulated structures off the west limb more closely match what is observed.
Where the model is less successful, we consider how this may be addressed,
through model developments or additional observational products.
