AI 中文总结
研究类似脉冲星的致密恒星内部是流体还是固体，基于奇异子星模型构建潮汐形变建模框架，发现固态和流体奇异子星潮汐可变形性有差异，建模内部应变积累，其结果或能结合电磁辐射检验致密恒星的固态性质。
AI 中文摘要
致密恒星的潮汐可变形性编码了致密物质的状态方程，引力波观测已开始在流体内部假设下对其进行约束。然而，类似脉冲星的致密恒星内部是流体还是固体在很大程度上仍未得到检验。在这项工作中，基于奇异子星模型，我们构建了一个固态致密恒星潮汐形变建模框架。采用剪切模量μ = 10³⁴ erg/cm³，我们发现1.4 M⊙的固态和流体奇异子星在潮汐可变形性上存在约40%的相对差异。我们还对双星合并过程中的内部应变积累进行了建模，发现其在恒星中心附近达到峰值。当引力波频率达到几百Hz时，会发生大规模破裂并释放高达约10⁴⁶ erg的弹性能量，足以驱动短γ射线暴前身。这种固液转变改变了潮汐响应并影响引力辐射的波形和相位。结合前身电磁辐射，这些引力波特征提供了一个多信使途径来检验类似脉冲星的致密恒星的固态性质。
英文摘要
The tidal deformability of compact stars encodes the equation of state of dense matter, and gravitational-wave observations such as GW170817 have begun to constrain it under the assumption of a fluid interior. Yet whether the interior of pulsar-like compact stars is fluid or solid remains largely untested, despite the distinct tidal responses the two states predict. In this work, based on the strangeon-star model, we develop a framework for modeling tidal deformation in solid compact stars. Adopting a shear modulus of $μ= 10^{34}\,\mathrm{erg}\,\mathrm{cm}^{-3}$, we find a relative difference of approximately $40\%$ in tidal deformability between solid and fluid strangeon stars of $1.4\,M_\odot$, corresponding to a $\sim 10\%$ deviation from the universal I--Love relation. We further model the accumulation of internal strain during binary inspiral and find that it peaks near the stellar center. When the gravitational-wave frequency reaches several hundred $\rm Hz$, large-scale fracturing occurs and can release up to $\sim 10^{46}\,\mathrm{erg}$ of elastic energy, sufficient to power short $γ$-ray-burst precursors. This solid-to-fluid transition alters the tidal response and imprints on the waveform and phase of the emitted gravitational radiation. Combined with the precursor electromagnetic emission, these gravitational-wave signatures offer a multi-messenger avenue to test the solid nature of pulsar-like compact stars.
Comments13 pages, 9 figures
