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Solar eruptive events, like flares and coronal mass ejections, arecharacterized by the rapid release of energy that can give rise to emission ofradiation across the entire electromagnetic spectrum and to an abruptsignificant increase in the kinetic energy of particles. These energeticphenomena can have important effects on the Space Weather conditions andtherefore it is necessary to understand their origin, in particular, what isthe eruptive potential of an active region (AR). In these case studies, wecompare two distinct methods that were used in previous works to investigatethe variations of some characteristic physical parameters during the pre-flarestates of flaring ARs. These methods consider: i) the magnetic flux evolutionand the magnetic helicity accumulation, and ii) the fractal and multi-fractalproperties of flux concentrations in ARs. Our comparative analysis is based ontime series of photospheric data obtained by the Solar Dynamics Observatorybetween March 2011 and June 2013. We selected two distinct samples of ARs: oneis distinguished by the occurrence of more energetic M- and X-class flareevents, that may have a rapid effect on not just the near-Earth space, but alsoon the terrestrial environment; the second is characterized by no-flares orhaving just few C- and B-class flares. We found that the two tested methodscomplement each other in their ability to assess the eruptive potentials of ARsand could be employed to identify ARs prone to flaring activity. Based on thepresented case study, we suggest that using a combination of different methodsmay aid to identify more reliably the eruptive potentials of ARs and help tobetter understand the pre-flare states.

Comparative case study of two methods to assess the eruptive potential of selected active regions