  DG CVn is a binary system in which one of the components is an M type dwarf
ultra fast rotator, only three of which are known in the solar neighborhood.
Observations of DG CVn by the Swift satellite and several ground-based
observatories during its super-flare event on 2014 allowed us to perform a
complete hard X-ray - optical follow-up of a super-flare from the red-dwarf
star. The observations support the fact that the super-flare can be explained
by the presence of (a) large active region(s) on the surface of the star. Such
activity is similar to the most extreme solar flaring events. This points
towards a plausible extrapolation between the behaviour from the most active
red-dwarf stars and the processes occurring in the Sun.
