  During solar minimum, the Sun is relatively inactive with few sunspots
observed on the solar surface. Consequently, we observe a smaller number of
highly energetic events such as solar flares or coronal mass ejections (CMEs),
which are often associated with active regions on the photosphere. Nonetheless,
our magnetofrictional simulations during the minimum period suggest that the
solar corona is still dynamically evolving in response to the large-scale
shearing velocities on the solar surface. The non-potential evolution of the
corona leads to the accumulation of magnetic free energy and helicity, which is
periodically shed in eruptive events. We find that these events fall into two
distinct classes: One set of events are caused by eruption and ejection of
low-lying coronal flux ropes, and they could explain the origin of occasional
CMEs during solar minimum. The other set of events are not driven by
destabilisation of low-lying structures but rather by eruption of overlying
sheared arcades. These could be associated with streamer blowouts or stealth
CMEs. The two classes differ significantly in the amount of magnetic flux and
helicity shed through the outer coronal boundary. We additionally explore how
other measurables such as current, open magnetic flux, free energy, coronal
holes, and the horizontal component of the magnetic field on the outer model
boundary vary during the two classes of event. This study emphasises the
importance and necessity of understanding the dynamics of the coronal magnetic
field during solar minimum.
