The top two panels show the combined JADE and JEDI energy fluxes for upward (a) and downward (b) electrons during the main auroral oval crossing in the south from perijove 6 (same time interval as Fig. 1). The black curves are the characteristic energy. Panel (c) shows the total energy flux within the loss cone of upward and downward electrons, as well as the UV brightness shifted by 21 seconds (same as in Figure 1(c)). The bottom two panels show the fraction of the energy flux in the energy bands listed on the right with respect to the total energy flux for upward (d) and downward (e) electrons within the loss cone. The 100-780 keV electrons provide the largest contribution to the total energy flux for most of the interval, except for a region just equatorward of the main oval crossing where the 3-30 keV electrons dominate for a short duration (< 1 minute). The gray vertical lines delimit the “peak” of the 3-30 keV electrons fraction contribution (see also Table 1). The M-shell values are derived from JRM09+CAN1981.
