in detail, thanks to the availability of high-cadence high-resolution observations together with long-term synoptic recordings. On top of that, the Sun is an active star, where phenomena like sunspots, faculae, prominences, and flares are connected to the variability of magnetic fields at various levels of solar body and its atmosphere. The flares in particular are considered the most violent active phenomena, with a direct influence on the neighbourhood of the Earth, thereby being responsible for space weather events.

The flares on the Sun are a consequence of the reconnection of the entangled magnetic field above active regions [@2011LRSP....8....6S]. The phenomenon of a ‘flare’ consists of effects connected to intensive atmospheric heating, formation of particle beams, and release of coronal mass ejections. Flares on the Sun depict various energies with smaller ones occurring frequently whereas the large flares are rare [e.g. @1993SoPh..143..275C; @1995PASJ...47..251S; @2000ApJ...535.1047A]. Solar flares are observed at all wavelengths from radio waves to gamma-rays. However, they are mostly prominent at radio wavelengths due to the non-thermal processes in the plasma and at high-energy (EUV and X-rays) range of wavelengths due to the high temperature at a reconnection site [@2008LRSP....5....1B].

In the range of the visible light (VL), the flares 