  Solar active regions and the processes that occur in them have been
extensively studied and analyzed and many types of models and characterizations
have been proposed for the occurrence of different eruptive events that take
place in the solar atmosphere. The most characteristic of these regions are
those that have opposite magnetic polarity, which, in their majority, generate
explosive events such as the so-called solar flares. The flares are intense
explosions occurring in the solar atmosphere with adverse effects on the Earth
and the technology developed by humans, and they are also determining factors
in the so-called space weather. For this reason, attempts have been made to
predict the occurrence of these events. In the present study, we developed a
predictive model of solar flares higher than M5 based on the articles proposed
by Korsos, et al. (2014, 2015) using the relationship between the flares and
the bipolar active regions. The analysis took into account the areas of the
umbrae of opposite polarity, their average magnetic field, and the magnetic
barycenter from each sunspot in the region for a sample of three active regions
to find the temporal variation due to the evolution of the sunspots, thus
confirming previous results reported in the literature. We made a statistical
analysis to determine whether after a flare occurs, another can arise in the
subsequent hours.
