标题： 动态潮汐在合并椭圆中子星双星中的可观测性 显示英文标题

标题： Observability of dynamical tides in merging eccentric neutron star binaries

摘要： 虽然动力潮汐仅在圆形吸积的最后几圈轨道中变得相关，但轨道偏心率可以通过在每次近距离相遇时激发潮汐振荡来在吸积的早期阶段增加其影响。 我们使用后牛顿数值模拟研究了动力潮汐对偏心中子星双星轨道演化的影响，并构建了一个解析随机模型，该模型能够再现数值结果。 我们的研究揭示了动力潮汐与近日点距离的强烈依赖关系，在大偏心率情况下，传递给动力潮汐的能量与通过引力波（GWs）耗散的能量之比在分离距离为$r_\mathrm{p}\lesssim50$公里时超过$\sim1\%$。 我们证明了动力潮汐对轨道演化的影响可以表现为引力波信号中的相位偏移。 我们表明，引力波相位偏移的信噪比在设计密度下，对于距离为$40$兆秒差距的偏心中子星双星，使用单个aLIGO探测器可以达到$8$的可检测阈值。 这需要在双星形成时具有接近$1$的偏心率，使得潮汐可变形性合理，并且 f 模频率为$500$和$1.73$kHz（分别为$700$和$1.61$kHz）的近日点距离为$r_\mathrm{p0}\lesssim68$km（$r_\mathrm{p0}\lesssim76$km）。 相位偏移的观测将使能够独立于潮汐可变形性测量中子星的 f 模频率，从而为中子星地震学和状态方程的性质提供重要的见解。 我们还探讨了区分等半径双星和双星系统的潜力，这可能提供揭示核状态方程中强一阶相变的机会。 显示英文摘要

摘要： While dynamical tides only become relevant during the last couple of orbits for circular inspirals, orbital eccentricity can increase their impact during earlier phases of the inspiral by exciting tidal oscillations at each close encounter. We investigate the effect of dynamical tides on the orbital evolution of eccentric neutron star binaries using post-Newtonian numerical simulations and construct an analytic stochastic model that reproduces the numerical results. Our study reveals a strong dependence of dynamical tides on the pericenter distance, with the fractional energy transferred to dynamical tides over that dissipated in gravitational waves (GWs) exceeding $\sim1\%$ at separations $r_\mathrm{p}\lesssim50$ km for large eccentricities. We demonstrate that the effect of dynamical tides on orbital evolution can manifest as a phase shift in the GW signal. We show that the signal-to-noise ratio of the GW phase shift can reach the detectability threshold of $8$ with a single aLIGO detector at design densitivity for eccentric neutron star binaries at a distance of $40$ Mpc. This requires a pericenter distance of $r_\mathrm{p0}\lesssim68$ km ($r_\mathrm{p0}\lesssim76$ km) at binary formation with eccentricity close to $1$ for a reasonable tidal deformability and f-mode frequency of $500$ and $1.73$ kHz ($700$ and $1.61$ kHz), respectively. The observation of the phase shift will enable measuring the f-mode frequency of neutron stars independently from their tidal deformability, providing significant insights into neutron star seismology and the properties of the equation of state. We also explore the potential of distinguishing between equal-radius and twin-star binaries, which could provide an opportunity to reveal strong first-order phase transitions in the nuclear equation of state.