  We investigate the thermal, kinematic and magnetic structure of small-scale
heating events in an emerging flux region (EFR). We use high-resolution
multi-line observations (including Ca II 8542~\AA, Ca II K, and Fe I 6301~\AA
line pair) of an EFR located close to the disk center from the CRISP and
CHROMIS instruments at the Swedish 1-m Solar Telescope. We perform non-LTE
inversions of multiple spectral lines to infer the temperature, velocity, and
magnetic field structure of the heating events. Additionally, we use the
data-driven Coronal Global Evolutionary Model to simulate the evolution of the
3D magnetic field configuration above the events and understand their dynamics.
Furthermore, we analyze the differential emission measure to gain insights into
the heating of the coronal plasma in the EFR. Our analysis reveals the presence
of numerous small-scale heating events in the EFR, primarily located at
polarity inversion lines of bipolar structures. These events not only heat the
lower atmosphere but also significantly heat the corona. The data-driven
simulations, along with the observed enhancement of currents and Poynting flux,
suggest that magnetic reconnection in the lower atmosphere is likely
responsible for the observed heating at these sites.
