标题： 评估均匀旋转对中子星结构的影响 显示英文标题

标题： Assessing the impact of uniform rotation on the structure of neutron stars

摘要： 近期实验室实验和天文观测的推动下，中子星物理的理解取得了显著进展。NICER的脉冲轮廓建模改进了我们对中子星质量和半径的认识，而引力波探测则揭示了中子星结构的关键见解。尤其是LIGO-Virgo合作组提取的潮汐变形率以及NICER最近确定的恒星半径，都表明在中间密度下存在相对较软的状态方程（EOS）。此外，PREX合作组和脉冲星定时测量的结果则表明，EOS在接近饱和密度和当前可达到的最高密度附近是较硬的。但这些极高密度下EOS到底可以有多硬呢？最近发生在“低质量间隙”附近的致密天体事件引发了关于是否存在非常重的中子星的问题。受此发现的启发，并考虑到理论模型的新改进，我们探讨了这些大质量天体可能是快速旋转中子星的可能性。我们研究了旋转如何影响最大中子星质量和它们相关的半径，并讨论了这对状态方程可能产生的影响。 显示英文摘要

摘要： Driven by recent laboratory experiments and astronomical observations, significant advances have deepened our understanding of neutron-star physics. NICER's Pulse Profile Modeling has refined our knowledge of neutron star masses and radii, while gravitational-wave detections have revealed key insights into the structure of neutron stars. Particularly relevant is the extraction of the tidal deformability by the LIGO-Virgo collaboration and the most recent determination of stellar radii by NICER, both suggesting a relatively soft equation of state (EOS) at intermediate densities. Additionally, measurements from the PREX collaboration and from pulsar timing suggest instead that the EOS is stiff in the vicinity of saturation density and at the highest densities accessible to date. But how stiff can the EOS be at these very high densities? Recent events featuring compact objects near the "lower mass gap" have raised questions about the existence of very massive neutron stars. Motivated by this finding and in light of new refinements to theoretical models, we explore the possibility that these massive objects may indeed be rapidly rotating neutron stars. We explore how rotation affects both the maximum neutron star mass and their associated radii, and discuss the implications they may have on the equation of state.