  The solar corona consists of a million-degree Kelvin plasma. A complete
understanding of this phenomenon demands the study of Quiet Sun (QS) regions.
In this work, we study QS regions in the 171 {\AA}, 193 {\AA} and 211 {\AA}
passbands of the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics
Observatory (SDO), by combining the empirical impulsive heating forward model
of Pauluhn & Solanki (2007) with a machine-learning inversion model that allows
uncertainty quantification. We find that there are {\approx} 2--3 impulsive
events per min, with a lifetime of about 10--20 min. Moreover, for all the
three passbands, the distribution of power law slope {\alpha} peaks above 2.
Our exploration of correlations among the frequency of impulsive events and
their timescales and peak energy suggests that conduction losses dominate over
radiative cooling losses. All these finding suggest that impulsive heating is a
viable heating mechanism in QS corona.
