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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 the transition of 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 corrections 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 multimessenger astronomy and empirical nuclear data. The maximal energy budget at the transitions was found to fall in the range of  10 49  − 10 52   ergs.

The energy budget of the transition of a neutron star into the third family branch