  Only a few red dwarf flaring stars in the solar neighbourhood have undergone
exceptional events called superflares. They have been detected with high-energy
satellites (i.e. Swift) and have been proven to be powerful events (both in
intensity and energy) and potentially hazardous for any extraterrestial life.
The physics of these events can be understood as an extrapolation of the (much)
weaker activity already occurring in the most powerful solar flares occurring
in the Sun. Nevertheless, the origin (why?) these superflares occur is
currently unknown. A recent study presents the optical and X-ray long-term
evolution of the emission by the super-flare from the red-dwarf star DG CVn
undertaken in 2014. In that paper we comment on the context of these
observations and on the properties that can be derived through the analysis of
them.
