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The small-scale moving intensity enhancements remotely observed in theextreme ultraviolet images of the solar active regions, which we refer to asactive region moving campfires (ARMCs), are related to local plasma temperatureand/or density enhancements. Their dynamics is driven by the physical processesin the entire coronal plasma. Our previous study of ARMCs indicates that theyhave characteristic velocities at around the background sound speed. The maingoal of our work is to carry out a simultaneous analysis of EUV images from twoobservational missions, SDO/AIA and Hi-C 2.1. The aims of the performedcross-validating analysis of both SDO/AIA and Hi-C 2.1 data were to reveal howthe observed moving features are distributed over the studied active region,AR12712, test the existence of different groups of ARMCs with distinct physicalcharacteristics. We use the statistical model of intensity centroid convergenceand tracking that was developed in our previous paper. Furthermore, a Gaussianmixture model fit of the observed complex of moving ARMCs is elaborated toreveal the existence of distinct ARMC groups and to study the physicalcharacteristics of these different groups. In data from the 171\AA, 193\AA\ and211\AA\ channels of SDO/AIA, we identified several groups of ARMCs with respectto both blob intensity and velocity profiles. The existence of such groups isconfirmed by the cross-validation of the 172\AA\ data sets from Hi-C 2.1. TheARMCs studied in this paper have characteristic velocities in the range of thetypical sound speeds in coronal loops. Hence, these moving objects differ fromthe well-known rapid Alfv\'enic velocity jets from magnetic reconnection sites.This is also proven by the fact that ARMCs propagate along the active regionmagnetic structure (strands). The nature of the discovered statistical groupingof the ARMC events is not known.

Categorization model of moving small-scale intensity enhancements in solar active regions