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We investigate the thermal, kinematic and magnetic structure of small-scaleheating events in an emerging flux region (EFR). We use high-resolutionmulti-line observations (including Ca II 8542~\AA, Ca II K, and Fe I 6301~\AAline pair) of an EFR located close to the disk center from the CRISP andCHROMIS instruments at the Swedish 1-m Solar Telescope. We perform non-LTEinversions of multiple spectral lines to infer the temperature, velocity, andmagnetic field structure of the heating events. Additionally, we use thedata-driven Coronal Global Evolutionary Model to simulate the evolution of the3D magnetic field configuration above the events and understand their dynamics.Furthermore, we analyze the differential emission measure to gain insights intothe heating of the coronal plasma in the EFR. Our analysis reveals the presenceof numerous small-scale heating events in the EFR, primarily located atpolarity inversion lines of bipolar structures. These events not only heat thelower atmosphere but also significantly heat the corona. The data-drivensimulations, along with the observed enhancement of currents and Poynting flux,suggest that magnetic reconnection in the lower atmosphere is likelyresponsible for the observed heating at these sites.

Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region