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tokens: the nonrotating case. Reconnection proceeds whenever the orientation of the BR is close to optimal and the continued disruption of the same section of overlying field eventually triggers a flare. The peak KE is higher for the corotating case because the flares are triggered at the same time unlike the counter-rotating case. The peak KE released for the simulations with two colliding rotating BRs is almost negligible. Looking at the simulation results more closely reveals that no flares are triggered in either simulation. This is likely because no section of the overlying field is disrupted for long enough to trigger a flare. Each rotating BR is in the optimal orientation only for a short time during rotation and never twice for the same section of overlying field. 4. Discussion The results from these simulations indicate that the motion of the emerging small-scale BRs that trigger flares can have a significant effect on the strength of those flares. In the most extreme cases the effect of motion alone caused over a threefold increase in the peak KE released by the flare. The proper motion of magnetic features such as these has been observed on the solar surface, for example, sunspots have been seen to drift at speeds of 0.14 km s −1 (Herdiwijaya et al. 1997 ) and moving magnetic features within sunspots move at ∼0.5 km s −1 (Zhang et al. 2007 ). Rotational motion of magnetic features has also been observed, the rotational velocity of sunspots has been measured at values of up to hr −1 during their emergence from the photosphere (Zhu et al. 2012 ). Photospheric motions are known to twist the coronal magnetic field into nonpotential configurations as discussed in Sundara Raman et al. ( 1998 ), Gerrard et al. ( 2002 ), Wang et al. ( 2018 ), and Yan Qu ( 2007 ). These magnetic fields can then be triggered resulting in a flare. In these simulations, however, which include a preexisting nonpotential field, we are only interested in how these motions effect the strength of the flare through the triggering process. In our first set of simulations we specifically considered linear oscillation of the emerging BR rather than simply drift; though, the results indicate that there may be little distinction. Interestingly the frequency at which the emerged BR oscillates does not seem to effect the strength of the flare. It is thought that this is because the frequency of the oscillation ultimately has no effect on how much of the overlying field is exposed to the disruptive trigger of the emerging small-scale BRs. The orientation of the oscillation on the other hand has been shown to be very important. Motion along the PIL generally increases the strength of the flare while motion across the PIL generally detracts from the strength of the flare. This is likely because the position of the emerging field on the PIL is the most disruptive to the overlying field and more of this field is disrupted if there is motion of the BR along the PIL. The most explosive