标题： 低质量黑洞-中子星合并的特征 显示英文标题

标题： Signatures of Low Mass Black Hole-Neutron Star Mergers

摘要： GW230529事件的最新观测表明黑洞-中子星双星系统可能包含低质量黑洞。由于较低质量的系统更有利于潮汐破坏，这类事件是多信使观测的有希望的候选者。在这项研究中，我们采用了五种有限温度、成分相关的物质状态方程，并展示了十个质量比分别为$q = 2.6$和$5$的三维广义相对论流体动力学模拟结果。其中两项模拟针对的是GW230529事件的啁啾质量和有效自旋参数，而其余八项则包含稍高质量的黑洞，包括自旋（$a_{BH} = 0.7$）和非自旋（$a_{BH} = 0$）模型。我们通过分析引力波和喷出物质的性质，讨论了状态方程、自旋和质量比对黑洞-中子星合并的影响。对于低质量比模型，我们发现对于最软的状态方程模型没有快速移动的喷出物，但较硬模型会产生大约$10^{-6}M_\odot$的快速移动喷出物，预计会对电磁对应体做出贡献。值得注意的是，高质量比模型产生的总动力学喷出物几乎相同，但比低质量比系统快移动喷出物多$52$倍。此外，我们观察到黑洞自旋往往会减少快速移动喷出物的数量，同时显著增加总喷出物的质量。最后，我们注意到随着中子星紧凑性降低，盘的质量往往增加。 显示英文摘要

摘要： The recent observation of the GW230529 event indicates that black hole-neutron star binaries can contain low-mass black holes. Since lower mass systems are more favourable for tidal disruption, such events are promising candidates for multi-messenger observations. In this study, we employ five finite-temperature, composition-dependent matter equations of state and present results from ten 3D general relativistic hydrodynamic simulations for the mass ratios $q = 2.6$ and $5$. Two of these simulations target the chirp mass and effective spin parameter of the GW230529 event, while the remaining eight contain slightly higher-mass black holes, including both spinning ($a_{BH} = 0.7$) and non-spinning ($a_{BH} = 0$) models. We discuss the impact of the equation of state, spin, and mass ratio on black hole-neutron star mergers by examining both gravitational-wave and ejected matter properties. For the low-mass ratio model we do not see fast-moving ejecta for the softest equation of state model, but the stiffer model produces on the order of $10^{-6}M_\odot$ of fast-moving ejecta, expected to contribute to an electromagnetic counterpart. Notably, the high-mass ratio model produces nearly the same amount of total dynamical ejecta, but yields $52$ times more fast-moving ejecta than the low-mass ratio system. In addition, we observe that the black-hole spin tends to decrease the amount of fast-moving ejecta while increasing significantly the total ejected mass. Finally, we note that the disc mass tends to increase as the neutron star compactness decreases.