be summarized as follows.

![image](fig1.eps){width="60.00000%"}

At the time of impulsive energy release in (micro-)flares, local chromospheric material gets heated up to very large temperatures $\approx 10$ MK. This leads to increase in local pressure that drives the local chromospheric material upward in to the corona along the (micro-)flare loops. Such process of filling of the loop with hot plasma is called chromospheric evaporation [@2009ApJ...699..968M; @2017ApJ...841L...9L and references therein]. The concept of chromospheric evaporation have been successfully used to explain the loop-top brightening in post-flare loops [see, e.g. @2016ApJ...823...47S] as well as coronal loops in general [@2006SoPh..234...41K]. Along with this, high pressure also pushes denser plasma downwards into the lower chromosphere, which is referred as chromospheric condensation [@2006ApJ...638L.117M and references therein]. In such models, emissions from hot materials from corona are expected to show blueshift (upflow) and that from cool material from upper chromosphere and transition region are expected to show redshift (downflow) as reported recently in a single observation by @2017ApJ...841L...9L. As underlying chromosphere is denser than the overlying corona, the expected speed of blueshift (upflow) should be much larger (approximately an order of magnitude) than that of redshift (downflow) [e.g., @1985ApJ...289..414F; @2009ApJ...699..968M]. The spectroscopic observations do show larger blueshifts 