论文标题
根据中子星向第三家族分支的过渡的能源预算
On the energy budget of the transition of a neutron star into the third family branch
论文作者
论文摘要
考虑到具有群众双胞胎的状态方程（EOS）的紧凑型恒星向第三家族的过渡。计算两组模型以进行比较的静态紧凑型恒星配置以保存静态紧凑型恒星配置的过渡的能量。选择的EOS是与密度依赖性功能DD2 EOS具有排除的HADRONIC物质模型校正，该模型校正会遭受相变，以通过恒定的声音接近速度描述的Quark物质。这两组EOS模型具有不同的紧凑型星质量围绕，可在过渡时最大化能量和半径差异，同时从多时间天文学和经验核数据中实现最新的限制。发现过渡时的最大能源预算范围在$ 10^{49} $ - $ 10^{52} $ ergs的范围内。
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.
