  In this work we study the case of deconfinement in compact star interiors in
the presence of a strong first order phase transition associated to a critical
end point in the QCD phase diagram. Neutron stars fulfilling these conditions
show a third branch in the mass-radius diagram with the first and second
branches being the white dwarfs and neutron stars configurations. The
transition to the third branch can be reached by a pure hadronic neutron star
through an induced collapse releasing energy that corresponds to a mass-energy
difference between the second and third branch configurations. Physical
outcomes of this phenomenon that can potentially explain the already detected
astrophysical signals are discussed. In particular we present energy
estimations for the case of a fast radio burst, seen as a double-peak structure
in the object's light curve.
