Panels, from L-R, showing a) a Hinode/SOT magnetogram of an AR core seen on the 14th Nov. 2007 saturated at ± 300 G; b) a Hinode/EIS image of the Fe xv emission (at 1.5 MK) of the corona above this region and c) the co-spatial and co-temporal simulated parallel electric field strength and orientation within this region (where pink/purple represents positive/negative E_||, and the opacity represents the relative strength of E_||− fully opaque regions identify while transparent regions show , for a peak coronal electric field strength in the simulation domain). The right hand panel is generated by simulations described in Bourdin et al. (2013), which also describes field lines which cross the intensity maxima of several EUV-emissive coronal loops, which have been overlaid in each panel; “CL” indicates core loops, while “SL” indicates shorter loops. The circles indicate EUV-emissive loop footpoints in the model and the corresponding plasma motion (and observed Doppler shifts) at these locations; red represents draining (i.e. motion along the line-of-sight away from an observer) while blue represents upflows (motion towards an observer).