Tracking the evolution of hot coronal plasma through `overlappograms' in response to magnetic flux emergence building up to an M2 flare

The evolution of hot plasma through the solar atmosphere during the early stages of a solar flare remains a question of interest in flare physics. Here we study a C-class and M-class flare which occurred within 6 hours of each other on 10-March-2015 to examine the interaction between the hot plasma and the reconnecting magnetic field. The Extreme ultraviolet Imaging Spectrometer (EIS) onboard \emph{Hinode} was observing using the wide slot for the He II emission line. It was possible to extract spectral information on the variation of Fe XXIV emission during the early phases of the flares, which were compared with those derived from hard X-rays. The plasma seen by RHESSI is directly related to the energy release process, whereas the one observed by EIS is consistent with evaporation of cooler plasma following the transfer of energy to the lower atmosphere. The onset of the flares was found to be the result of magnetic flux emergence, rotation, shearing and motion all of which combined to provide sufficient free energy to be released. The hot plasma from the flare were located in a small section of the active region to the north-west of the main sunspot. Within that region, there were three magnetic fragments involved, one of which did not have flux emergence, but did have a change in shear, and motion. We analysed the behavior of these fragments to relate them to the flaring.