标题： 首次非破坏性中子星-黑洞和双黑洞合并模拟的直接比较 显示英文标题

标题： First direct comparison of non-disrupting neutron star-black hole and binary black hole merger simulations

摘要： 我们首次直接比较了全广义相对论中的中子星-黑洞和黑洞-黑洞合并的数值模拟。 我们关注一个物体不自旋的配置，并且在中子星-黑洞系统中最可能的质量比范围内（q=6）。 在这个参数空间区域，中子星在合并前不会被潮汐破坏，我们表明这两种类型的合并看起来非常相似。 中子星的存在对引力波信号的影响不仅无法被下一代引力波探测器检测到，而且在数值模拟中也小到无法测量：即使下落、合并和衰减信号在两种双星系统中都完全一致。 合并后的残余物的特性同样相似，最终黑洞的质量差异小于dM< 5×10^{-4}M_BH，它们的自旋差异小于da< 10^{-3}M_BH。 混合双星的近日点进动率与之前发表的双黑洞结果一致，我们利用 inspiral 波形对数值模拟的准确性进行了独立于每种双星类型所做算法选择的约束。 总体而言，我们的结果表明，非破坏性中子星-黑洞合并由黑洞-黑洞合并非常良好地建模，并且鉴于缺乏质量抛射、吸积盘形成或引力波信号的差异，只有电磁前身信号才能证明总质量约为10Msun的低自旋系统中中子星的存在，至少直到引力波探测器的灵敏度达到与提议的爱因斯坦望远镜相当的水平。 显示英文摘要

摘要： We present the first direct comparison of numerical simulations of neutron star-black hole and black hole-black hole mergers in full general relativity. We focus on a configuration with non spinning objects and within the most likely range of mass ratio for neutron star-black hole systems (q=6). In this region of the parameter space, the neutron star is not tidally disrupted prior to merger, and we show that the two types of mergers appear remarkably similar. The effect of the presence of a neutron star on the gravitational wave signal is not only undetectable by the next generation of gravitational wave detectors, but also too small to be measured in the numerical simulations: even the plunge, merger and ringdown signals appear in perfect agreement for both types of binaries. The characteristics of the post-merger remnants are equally similar, with the masses of the final black holes agreeing within dM< 5 10^{-4}M_BH and their spins within da< 10^{-3}M_BH. The rate of periastron advance in the mixed binary agrees with previously published binary black hole results, and we use the inspiral waveforms to place constraints on the accuracy of our numerical simulations independent of algorithmic choices made for each type of binary. Overall, our results indicate that non-disrupting neutron star-black hole mergers are exceptionally well modeled by black hole-black hole mergers, and that given the absence of mass ejection, accretion disk formation, or differences in the gravitational wave signals, only electromagnetic precursors could prove the presence of a neutron star in low-spin systems of total mass ~10Msun, at least until the advent of gravitational wave detectors with a sensitivity comparable to that of the proposed Einstein Telescope.