location of heating does not matter much to reproduce qualitative aspects of the observed upflow in the loop.

In order to be consistent with observations, the loop length is taken to be $24$ Mm, with $20$ Mm inside the corona. The loop-top of the simulated loop is situated at the center of the coordinate system, whereas each end of the loop is assumed to be embedded $2$ Mm into the transition region and the chromosphere to serve as a plasma reservoir. The radius of the loop is assumed to be $1$ Mm. Gravity is made to change with height. The gravitational potential has the usual $1/r$ fall off with respect to the center of the Sun. The numerical details of the loop are described in @2009ApJ...699.1480S.

The initial temperature of the coronal part of the loop is taken to be $4$ MK. Density profile maintains an exponential profile with the least density ($1.46 \times 10^9$ cm$^{-3}$) at the loop-top and the highest density ($2.45 \times 10^{11}$ cm$^{-3}$) towards the footpoints. We allow the loop to cool down through radiation until $100$ s, when the loop is hit by two similar heating events at the two ends of the footpoints within 