中子星含反K介子凝聚的致密物质状态方程的贝叶斯推断
Bayesian Inference of dense matter equation of state of neutron star with antikaon condensation
AI总结：
本文采用 DDRH 场论模型进行贝叶斯分析，结合核物理与天体物理观测约束，研究了含反K介子凝聚的中子星致密物质状态方程，发现反K介子凝聚使状态方程软化并将最大质量限制在约2倍太阳质量。
摘要：
本文采用密度依赖相对论强子（DDRH）场论模型进行贝叶斯分析，以研究中子星内部存在 $K^-$ 和 $\bar{K}^0$ 反K介子凝聚的致密物质状态方程（EOS）。K介子部分的矢量耦合参数通过同位旋计数规则和夸克模型确定。我们的研究整合了多种约束条件，包括 $χ$EFT 计算、核饱和性质，以及来自脉冲星 PSR J0030+0451 和 PSR J0740+66 的天体物理观测和 GW170817 事件。我们展示了由这些约束条件推导出的模型参数的后验分布，从而探索核物质性质和中子星（NS）特征（如半径、潮汐形变、中心能量密度和声速）的分布。在 68(90)% 置信区间内，反K介子势确定为 $-129.36^{+12.53(+32.617)}_{-3.837(-5.696)}$ MeV。这与几项在 $-120$ 至 $-150$ MeV 范围内提供估计的研究一致。我们发现，由于反K介子凝聚导致 EOS 显著软化，最大中子星质量被限制在约 2M$_\odot$。这种软化导致声速显著下降。尽管 $K^-$ 反K介子凝聚在标准中子星内部不可行，但在更高的 NS 质量下变得可行。$K^-$ 和 $\bar{K}^0$ 的凝聚很可能存在于质量大于 2M$_\odot$ 的中子星内部。我们还讨论了在反K介子凝聚背景下，输入变量、EOS 的同标量和同矢量方面与特定 NS 性质之间的相互联系。
英文摘要：
In this paper, we employ the Density Dependent Relativistic Hadron (DDRH) field theoretical Model in a Bayesian analysis to investigate the equation of state (EOS) of dense matter featuring antikaon condensation for $K^-$ and $\bar{K}^0$ inside neutron stars. The vector coupling parameters within the kaonic sector are determined through the iso-spin counting rule and quark model. Our study integrates various constraints, including $χ$EFT calculations, nuclear saturation properties, and astrophysical observations from pulsars PSR J0030+0451 and PSR J0740+66 and from the GW170817 event. We present posterior distributions of model parameters derived from these constraints, enabling us to explore the distributions of nuclear matter properties and neutron star (NS) characteristics such as radii, tidal deformabilities, central energy densities, and speed of sound. The antikaon potential at the 68(90)\% confidence intervals is determined to be $-129.36^{+12.53(+32.617)}_{-3.837(-5.696)}$ MeV. This aligns with several studies providing estimates within the range of $-120$ to $-150$ MeV. We find that the maximum neutron star mass is constrained to around 2M$_\odot$ due to the significant softening of the EOS caused by antikaon condensation. This softening results in a considerable decrease in the speed of sound. Although antikaon condensation for $K^-$ is not feasible inside the canonical neutron stars, it becomes feasible for higher NS masses. The condensation of both $K^-$ and $\bar{K}^0$ is probably present in the interior of neutron star with mass greater than 2M$_\odot$. We also discuss the interconnections among input variables, isoscalar and isovector aspects of the EOS, and specific NS properties in the context of antikaon condensation.
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