Gravitational waves from inspiraling binary neutron stars provide unique access to ultradense nuclear matter and offer the ability to constrain the currently unknown neutron star equation-of-state through tidal measurements. This, however, requires the availability of accurate and efficient tidal waveform models. In this paper we present phenomgsf, a new phenomenological tidal phase model for the inspiral of neutron stars in the frequency domain, which captures the gravitational self-force informed tidal contributions of the time-domain effective-one-body model teobresums. phenomgsf is highly faithful and computationally efficient, and by choosing a modular approach, it can be used in conjunction with any frequency-domain binary black hole waveform model to generate the complete phase for a binary neutron star inspiral. phenomgsf is valid for neutron star binaries with unequal masses and mass ratios between 1 and 3, and dimensionless tidal deformabilities up to 5000. Furthermore, phenomgsf does not assume universal relations or parametrized equations of state, hence allowing for exotic matter analyses and beyond standard model physics investigations. We demonstrate the efficacy and accuracy of our model through comparisons against teobresums, numerical relativity waveforms and full Bayesian inference, including a reanalysis of the binary neutron star observation GW170817.

中文翻译：

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引力自力增强潮汐的现象学模型


来自吸气双中子星的引力波提供了获得超致密核物质的独特途径，并提供了通过潮汐测量来约束目前未知的中子星状态方程的能力。然而，这需要准确高效的潮汐波形模型。在本文中，我们提出了 phenomgsf，这是一种用于中子星在频域中螺旋的新的现象学潮汐相位模型，它捕获了时域有效单体模型 teobresums 的引力自力知情潮汐贡献。PHenomGSF 具有高度的忠实度和计算效率，通过选择模块化方法，它可以与任何频域双黑洞波形模型结合使用，以生成双中子星螺旋的完整相位。PHenomGSF 适用于质量不等且质量比在 1 到 3 之间的中子星双星，以及高达 5000 的无量纲潮汐变形能力。此外，phenomgsf 不假设普遍关系或参数化状态方程，因此允许进行奇异物质分析和超越标准模型物理学的研究。我们通过与 teobresums、数值相对论波形和完整的贝叶斯推理的比较，包括对双中子星观测GW170817的重新分析，证明了我们模型的有效性和准确性。