Vertical magnetic field B_z in the photosphere at three separate times during the simulation (upper panels). The white dotted lines at y = 10.78 Mm in the upper three panels show the location of the vertical cut in the xz-plane of the chromospheric and coronal temperature structure displayed in the panels below. These six panels show the evolution of the outer atmosphere as the magnetic bubble pierces the photosphere and expands through the chromosphere, pushing the corona upward, carrying cool material to large heights and heating the corona as the emergent and ambient field interact at large angle. The EB and UV burst described in the paper both occur in a period centered on t = 8200 s. The UV burst visible in the lower middle panel lasts some 200 s. The temperature rise of the EB is not easily visible in these panels because the temperature of EBs is far lower than that of the UV burst (but see Fig. 6). The EB occurs on the white dotted line around x = 11.5 Mm near the center of the meeting opposite polarities that are visible in the upper right panel, and it lasts significantly longer than the UV burst. It starts at t = 7600 and lasts at least 1200 s thereafter.