the corona ($\pm 9.7$ Mm). These heating events last for $120$ s, span over $200$ km (energy $\sim 10^{27}$ erg), and produce plasma dynamics in the loop. Panels (a) and (b) in Figure \[fig:simul\_param\] depict temperature and velocity evolutions along the loop. Simulation outputs are folded through AIA response functions of 131 [Å]{} and 94 [Å]{} filters to produce emission measure outputs. To compare these emission measures with real observations we degrade the spatiotemporal resolution to $1000$ km and $12$ s. The resulting emission measure is depicted in panels (c) and (d) of Figure \[fig:simul\_param\]. Following the deposition of the heating events, both emission measure plots show a continuous brightening of the coronal loop starting at the footpoints which propagates towards the loop-top. Just as in the real observations (compare Figure \[fig:bright\_front\]), we also mark these locations with white lines.

Soon after the occurrence of heating events at the both footpoints along coronal loop, local plasma of the loop gets heated up and pushes the transition region downward. This is evident in the temperature plot shown in panel (A) of Figure \[fig:simul\_loop\]. Heat energy from the event sites quickly flows down to the chromosphere through conduction and leads to the 