AI 中文总结
在RMF框架下，采用TW99参数化方案，研究发现奇异介子凝聚会改变大质量原中子星的物态方程，降低其转动惯量峰值并使峰值向高密度移动，为原中子星转动演化的引力波研究提供约束。
AI 中文摘要
我们在相对论平均场（RMF）框架内研究奇异介子（σ*和φ）对大质量原中子星（PNSs）结构和转动性质的影响。采用每重子熵S=1、轻子分数YL=0.4的TW99参数化方案，我们求解TOV方程并通过Hartle-Thorne近似计算转动惯量。在八种参数化方案中，TW99因给出最大最大质量而被选用。结果表明，奇异介子会软化高密度下的物态方程，降低最大质量和半径。转动惯量在低于最大质量的中心密度处达到峰值，奇异介子将该峰值向更高密度移动，同时略微降低其数值。对于质量低于2.1倍太阳质量的PNSs，转动惯量的相对变化可忽略不计，但在2.7倍太阳质量时降至约-0.6，表明奇异效应对最大质量恒星最为显著。本研究结果为大质量PNSs的转动演化及其潜在的引力波信号提供了有用约束。
英文摘要
We investigate the effects of strange mesons (sigma-star and phi) on the structural and rotational properties of massive proto neutron stars (PNSs) within the relativistic mean-field (RMF) framework. Using the TW99 parametrization with entropy per baryon S=1 and lepton fraction YL=0.4, we solve the TOV equations and compute the moment of inertia via the Hartle-Thorne approximation. Among eight parametrizations, TW99 is chosen as it gives the largest maximum mass. Our results show that strange mesons soften the equation of state at high densities, reducing both the maximum mass and radius. The moment of inertia peaks at a lower central density than the maximum mass, and strange mesons shift this peak toward higher densities while slightly lowering its value. The relative change in I is negligible for PNSs below 2.1 solar mass, but decreases to about -0.6 at 2.7 solar mass, indicating that strangeness effects are most relevant for the most massive stars. Our findings provide useful constraints on the rotational evolution of massive PNSs and their potential gravitational-wave signatures.
Comments8 pages, 6 figures
