发表机构
University of Southampton（南安普顿大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究探讨有限反应速率对含超子物质的中子星振荡谱的影响，将非轻子弱相互作用速率纳入相对论扰动方程，揭示体黏性耗散对振荡模式及潮汐响应的作用，为相关引力波模型构建提供基础。
AI 中文摘要
双中子星并合过程中，恒星振荡模式的潮汐激发为探测超核密度下的致密物质组成提供了有力工具。化学平衡在恒星扰动计算中发挥着关键作用，但常被忽略：若化学平衡时标与振荡时标相当，黏性效应会阻尼振荡模式；若反应速率快，部分模式会因恢复力消失而完全消失。然而，这类计算通常假设要么是瞬时化学平衡，要么无平衡（冻结组成）。基于此，我们研究有限反应速率对含超子物质的中子星振荡谱的影响。我们计算主导的非轻子弱相互作用速率，并通过复的、频率相关的动力学声速将其纳入相对论扰动方程。我们表明，有限速率效应自然表现为体黏性耗散，修改基模（f模）和重力模（g模）的特性。我们进一步通过将恒星扰动与近区边界条件匹配，研究其对潮汐响应的影响，证明黏性耗散如何引发潮汐滞后。这些结果提供了连接微观反应率与体黏性及双致密星潮汐动力学的一致框架，为将黏性耗散纳入双中子星并合的引力波模型迈出了一步。
英文摘要
Tidal excitations of stellar oscillation modes during binary neutron-star inspirals offer a powerful probe of the composition of dense matter at supranuclear densities. Chemical equilibration plays a crucial, but often neglected, role in stellar perturbation calculations. If the chemical equilibration timescale is comparable to the oscillation timescale, then viscous effects can damp the modes. If the reactions are fast, some modes can completely disappear since their restoring force vanishes. Typically, these calculations, however, assume either instantaneous chemical equilibrium or no equilibration (frozen composition). Motivated by this, we investigate the effects of finite reaction rates on the oscillation spectrum of neutron stars containing hyperonic matter. We calculate the dominant non-leptonic weak interaction rates and incorporate them into the relativistic perturbation equations through a complex, frequency-dependent dynamical sound speed. We show that finite-rate effects naturally manifest as bulk-viscous dissipation, modifying the properties of both the fundamental ($f$) and gravity ($g$) modes. We further examine the impact on the tidal response by matching stellar perturbations to near-zone boundary conditions, demonstrating how viscous dissipation gives rise to a tidal lag. These results provide a consistent framework connecting microscopic reaction rates and the resulting bulk viscosity to the tidal dynamics of compact binaries, and represent a step towards incorporating viscous dissipation into gravitational-wave models of binary neutron-star inspirals.
Comments14 pages, 7 figures, comments are welcome
