the time range of interest. If a RHESSI flare is detected, the fraction of the rise time (GOES start $\rightarrow$ GOES peak) that the RHESSI flare flag was active was also calculated. While RHESSI is a full-disk instrument, its orbit implies that it may have captured anywhere from a few seconds of a given flare up to around an hour (note that some long-duration flares are detectable over several RHESSI orbits).

From the lightcurves presented in the lower-left panel of Figure \[sff\_plot\] it can be seen that RHESSI captured the peak of the M1.5 flare up to an energy of 50–100keV. The contours of the RHESSI quicklook image (6–25keV; black contours overlaid on the EUV image) agree with the flare location computed from the AIA 131Å data (white circle).

The *EUV Variability Experiment* {#ss:sdo_eve}
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The SDO spacecraft is in a geosynchronous orbit allowing it to observe the full disk of the Sun continuously without interruption (except for the occasional lunar and terrestrial eclipses). For simplicity, it was assumed that both AIA and the *Helioseismic and Magnetic Imager* (HMI: @sche12) were observing continuously throughout each event. The EVE instrument, however, is less straightforward. While MEGS-A, which provides spatially integrated Sun-as-a-star 