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tokens: of the projection effect of looking from the side, this corresponds to x = 11 when viewed from directly above. The line profile over the EB, shown in the left panel , is located at [ x , y ] = [17, 11] Mm and is evident in the line wings. The line core, shown in the right panel of Fig. 4 , shows extensive fibrils, some have about the length of the computational box, 20 Mm, but no evidence of brightening directly above the site of the EB. The two loop systems that meet and are the source of the EB are visible in the center of the right panel of Fig. 4 . They stretch toward greater and lower y -values from their meeting point close to y = 11 Mm? When viewed from directly above, the EB region is bright in H α in the line core as well, but this is due to emission that is formed much higher in the atmosphere, at least 5 Mm above the photosphere: The cool canopy above the current sheet is heated by Ly α and Ly-continuum radiation from the hot plasma of the current sheet below, raising the temperature of the canopy plasma significantly, as is visible in the lower middle panel of Fig. 1 and in the left panel of Fig. 3 . This relatively high-temperature gas excites some H α emission in the region that is heated above the current sheet. This heating at large heights directly above the reconnection region is probably a result of the method we chose for the coronal back-radiation and raises the temperature more than what would occur on the real Sun. The heating does not affect the evolution or diagnostics of the EB or UV burst. Swedish 1-meter Solar Telescope observations (Ortiz et al., in prep.) show that the wing of the Ca II 854.2 nm line can be a very good proxy for the existence of EBs, with enhanced emission that is colocated and roughly cotemporal with bright H α wing enhancement. These observations in the blue wings of both the Ca II 854.2 nm and H α lines also show dark, presumably cool, surges that occasionally emanate from the site of EB emission. We find that the EB in this location shows brightening, starting at time t = 7500 s and lasting for at least 1200 s thereafter. This enhanced emission, 0.0735 nm in the blue wing of the Ca II 854.2 nm triplet line, is shown in Fig. 5 , which also shows emission in the line core and in the shape of the line profile. Similar as for H α , the cores of the Ca II H Kand the Ca II 854.2 nm triplet lines show the loops that emanate from the vicinity of the current sheet as narrow thin fibrils that stretch toward higher and lower y -values, approximately in the y -direction. The EB is visible as a narrow band of emission in the line wing, and it is also visible at the time of this image ( t = 8220 s) in the line core, although this emission is partially covered by overlying longer fibrils. Apparently rising from the EB location, about parallel with the positive y -axis, a small cool surge is seen to be accelerated along the field lines, or loops, that form the cool portion of the canopy. Signs of the