events with the aid of modern high-resolution imaging and spectroscopic observations and modeling.

investigated the correspondence between X-ray observations of ARTBs with EUV brightening. It was found that the strongest ARTBs observed in EUV had a counterpart in X-rays, whereas weaker EUV ARTBs did not show any X-ray emission. This was attributed to the fact that no plasma is heated beyond 2 MK. Since the energy values of ARTBs were similar to micro-flares, i.e., six orders of magnitude lower than a flare, ARTBs are also referred as micro-flares [see, @hudson2004]. Hereafter, we shall be using micro-flares and ARTBs terms interchangeably.

Using the Hard X-ray observations recorded by The Reuven Ramaty High Energy Solar Spectroscopic Imager [RHESSI, @2002SoPh..210....3L], @2008ApJ...677.1385C performed a detailed statistical study of micro-flares and obtained frequency distributions of the peak energy [see also @2014ApJ...784..134R; @Sub_KT using Hi-C and AIA observations]. These distributions can be represented by power-law distributions with a negative power-law index between 1.5[–]{}1.6. Such distributions suggest that the process of energy release in micro-flares is similar to those in large flares, though the energy involved is about six orders of magnitude less. The process of the energy release in such micro-flaring events or flaring events can 