AI 中文总结
研究致密双星系统形成历史，探讨偏心NSBH合并参数测量对其形成渠道推断的影响，发现精确测量有效自旋参数等能增加相关系统比例，改进质量测量可更好约束质量分布，还能测试种群水平偏心率分布。
AI 中文摘要
致密双星系统的形成历史一直是天体物理学中的关键开放性问题之一。理论研究通常支持中子星-黑洞（NSBH）系统的孤立双星演化，这往往产生近圆形轨道。然而，近期对引力波事件GW200105的分析表明其源具有可测量的偏心率，暗示其他形成渠道也可能有贡献。研究表明，偏心NSBH合并的内在参数，如组成质量和自旋，比利用LIGO-Virgo-KAGRA（LVK）天文台对圆形合并的测量要好得多。本文探索这种偏心率增强的参数测量如何影响NSBH形成渠道的推断。发现对有效自旋参数χeff更精确的测量增加了能可靠识别负值的系统比例，在第五次LVK观测运行（O5）中，对于各向同性分布的种群，每约2.5次偏心NSBH探测就能清晰测量一次自旋-轨道未对齐事件。改进的NS质量测量为NS质量分布提供了更好的约束能力，可能揭示结构并收紧其上下质量的界限。同样，通过偏心率增强测量改善了对依赖金属丰度的BH质量分布的恢复。最后表明，到O5结束时可以测试为动力学形成渠道提出的种群水平偏心率分布。
英文摘要
The formation history of compact binary systems remains one of the key open questions in astrophysics. Theoretical studies generally favor isolated binary evolution for neutron star-black hole (NSBH) systems, which tends to produce nearly circular orbits. However, recent analyses of the gravitational-wave event GW200105 indicate that its source has measurable eccentricity, suggesting that alternative formation channels may also contribute. It has been shown that the intrinsic parameters of eccentric NSBH mergers, such as the component masses and spins, are much better measured than circular mergers with LIGO-Virgo-KAGRA (LVK) observatories. We explore how such eccentricity-enhanced parameter measurements can affect the inference of NSBH formation channels. We find that sharper measurements of the effective spin parameter $χ_{\rm eff}$ increase the fraction of systems for which negative values can be confidently identified, allowing for the clear measurement of a spin-orbit misaligned event every $\sim 2.5$ eccentric NSBH detections for an isotropically distributed population in the fifth LVK observing run (O5). Improved NS mass measurements provide better constraining power for NS mass distributions, potentially revealing structure and tightening the bounds that can be drawn on their upper and lower masses. Similarly, the recovery of a metallicity-dependent BH mass distribution is improved by eccentricity-enhanced measurements. Finally, we show that the proposed population-level eccentricity distribution for dynamical-formation channels can be tested by the end of O5.
Comments12 pages, 6 figures, 3 tables. Comments are welcome
