  Transition of a compact star into the third family for an equation of state
(EoS) featuring mass twins is considered. The energy released at a baryon
number conserving transition for static compact stars configurations is
computed for two sets of models for comparison. The EoS of choice is the
density dependent functional DD2 EoS with excluded model correction for
hadronic matter which suffers a phase transition into deconfined quark matter
described by a constant speed of sound approach. The two sets of EoS models
feature different compact star mass onsets that maximize the energy and radius
difference at the transition while simultaneously fulfilling state-of-the-art
constraints from multi-messenger astronomy and empirical nuclear data. It is
found that the maximal energy budget at the transitions falls in the range of
$10^{49}$ - $10^{52}$ ergs.
