We note here that these are just the lower limit of energy released during ARTBs, as was also pointed out by @2014Sci...346C.315P. Estimated energies are equivalent to the energies involved in a typical micro-flare events.

Comparison with Hydrodynamic Simulations {#sec:model}
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![image](fig16.eps){width="95.00000%"}

![image](fig17.eps){width="95.00000%"}

For a better understanding of the observations described in earlier sections, it is instructive to numerically simulate the scenario where a coronal loop may get brightened up following ARTBs. The observed downflows (shown in Section \[sec:spectroscopy\]) in cooler lines (such as and ) associated with ARTBs suggest a strong chromospheric condensation due to impulsive heating, similar to those observed in flaring loop [e.g., @2006ApJ...638L.117M; @2006SoPh..234...95D; @2006SoPh..239..173D] or predicted by @2014Sci...346B.315T. In this scenario, heat from the coronal part of the loop gets conducted to the chromosphere, that pushes down the chromospheric plasma further during its initial phase and eventually makes it evaporate into the corona. Based on this assumption, we perform two simulations of a monolithic loop. In one of the simulations, the loop is heated by two identical microflare-like heating events of energy $10^{27}$ erg, while in the second one heat is deposited close to the loop-top via a single microflare-like event. As we demonstrate below, 