  Small scale transients occur in the Solar corona at much higher frequencies
than flares and play a significant role in coronal dynamics. Here we study
three well-identified transients discovered by Hi-C and also detected by the
EUV channels of Atmospheric Imaging Assembly (AIA) on board Solar Dynamics
Observatory (SDO). We use 0-D enthalpy-based hydrodynamical simulations and
produce synthetic light curves to compare with AIA observations. We have
modeled these transients as loops of ~ 1.0~Mm length depositing energies ~
10^23 ergs in ~ 50 seconds. The simulated synthetic light curves show
reasonable agreement with the observed light curves. During the initial phase,
conduction flux from the corona dominates over the radiation, like impulsive
flaring events. Our results further show that the time-integrated net enthalpy
flux is positive, hence into the corona. The fact that we can model the
observed light curves of these transients reasonably well by using the same
physics as those for nanoflares, microflares, and large flares, suggests that
these transients may have a common origin.
