发表机构
Swarthmore College（斯沃斯莫尔学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过大样本参数化物态方程求解中子星f模，发现现有普适关系残差与物态方程刚度强相关，引入线性修正项后显著提升信噪比预测精度，而f模-潮汐形变度关系仍保持高度普适。
AI 中文摘要
在双中子星并合过程中或脉冲星发生星震（glitch）时，中子星基模（f模）的激发可产生引力波，这些引力波将被下一代探测器探测到，从而为中子星的引力波星震学打开大门。存在一些近似不依赖于物态方程（EOS）的“普适”关系，将f模与其他中子星性质联系起来。这些普适关系通常是通过相对较小、有选择性的EOS样本确定的。为了更全面地探索参数空间，我们通过在全广义相对论框架下求解线性化流体扰动方程，计算f模频率和阻尼时间，研究了一个包含大量分段参数化EOS的样本。我们利用该样本评估了先前提出的针对f模频率和阻尼时间的普适关系（URs）对EOS的敏感性。我们发现，仅依赖于中子星质量和半径组合的URs具有显著的残差，这与先前报道一致；但这些残差与EOS的整体刚度强相关。我们通过引入线性修正项来解释这种对EOS的残差依赖性，这些修正项依赖于EOS预测的特征半径以及中等质量处质量-半径曲线的斜率。为了评估我们新的修正项对可观测量的影响，我们考虑了类船帆座（Vela-like）脉冲星星震引起的引力波发射情形，并证明对于此类事件，使用现有的单参数UR预测的信噪比会被高估或低估高达约10%，而使用我们改进的三参数UR则几乎可以精确恢复。相反，我们发现f模与潮汐形变度之间的URs在其残差中仅表现出极小的EOS依赖性相关性，并且总体上仍然高度不依赖于EOS。
英文摘要
Excitations of the neutron star (NS) fundamental mode (f-mode) during a binary NS inspiral or from a glitching pulsar can produce gravitational waves (GWs) that will be detectable with the next generation of detectors, opening the door to GW asteroseismology of neutron stars. There exist approximately equation-of-state (EOS)-insensitive, or "universal," relations that relate the f-mode to other NS properties. These universal relations have typically been identified with relatively small, selective EOS samples. To more thoroughly explore the parameter space, we examine the f-modes for a large sample of piecewise-parametric EOSs by solving the linearized fluid perturbation equations for the f-mode frequency and damping time in full general relativity. We utilize our sample to evaluate the EOS-sensitivity of previously-proposed universal relations (URs) for both the f-mode frequency and damping time. We find that URs that depend on combinations of only NS mass and radius have significant residuals, as previously reported; but that these residuals are strongly correlated with the overall stiffness of the EOS. We account for this residual dependence on the EOS by introducing linear correction terms that depend on the characteristic radius predicted by the EOS and the slope of the mass-radius curve at intermediate masses. To assess the impact of our new correction terms on observables, we consider the case of GW emission due to a glitch in a Vela-like pulsar and demonstrate that the predicted signal-to-noise ratio for such an event is over/under-estimated by up to ~10% when using an existing, single-parameter UR, but is recovered nearly exactly with our improved 3-parameter UR. In contrast, we find that URs between the f-mode and tidal deformability exhibit only minimal EOS-dependent correlations in their residuals and overall remain highly EOS-insensitive.
