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 10⁴⁹ − 10⁵² ergs.

中文翻译：

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中子星向第三家庭分支过渡的能量预算

考虑了以质量孪生为特征的状态方程（EoS）的紧凑型恒星向第三族的过渡。计算两组模型的重子数释放的能量，以保持静态紧凑恒星构型的过渡，以进行比较。选择的EoS是密度依赖的功能性DD2 EoS，其中排除了强子物质的模型校正，该过程经历了以恒定声速描述的相变为限定的夸克物质的相变。两组EoS模型具有不同的紧凑型恒星起始点，这些起始点使过渡时的能量和半径差最大化，同时满足了来自多信使天文学和经验核数据的最新约束。发现过渡时的最大能量预算在10的范围内⁴⁹  - 10 ⁵²尔格。