. In the current study, we have utilized the approach of where the emission due to the hot line can be obtained as:

$$I(Fe~XVIII) \approx I(94~{\AA}) - I(211~{\AA})/120 - I(171~{\AA})/450$$

where I(94 [Å]{}), I(211 [Å]{}), and I(171 [Å]{}) are intensities from AIA 94 [Å]{}, 211 [Å]{}, and 171 [Å]{} passbands respectively.

After the first appearance of ARTBs, a loop structure was observed at different times in different filters with the footpoints located at the two ARTBs namely A and B. Figure \[fig:hot\_loop\] displays the hot loops seen in three AIA channels namely AIA 335 [Å]{}, corrected 94 [Å]{} (), and AIA 131 [Å]{} and in XRT Al\_med filter. The full extent of the hot loop was observed in AIA 131, corrected 94, and 335 [Å]{} filters at times 13:05:08, 13:05:25, and 13:10:14 UT respectively, whereas the peak phase of ARTB appeared at time 13:03:44 UT as observed from AIA 131 [Å]{} passband. We have identified and traced the complete hot loop in the corrected AIA 94 [Å]{} (top right panel in Figure \[fig:hot\_loop\]) passband from foot-points A to B  for further analysis. The traced loop is over-plotted in the top right panel of Figure \[fig:hot\_loop\]. The width of the traced 