AI 中文总结
本研究用SEVN代码生成合成星表，结合TNG50模拟探究类银河系中HMXBs与BCO并合的关联，明确CE阶段和kick速度是决定并合数量的主要过程，得出BH-HMXBs与NS-HMXBs演化成并合BCOs的不同占比。
AI 中文摘要
大质量X射线双星（HMXBs）是连接大质量恒星双星与并合双致密天体（BCOs）形成的潜在中间阶段，但HMXBs后续演化成并合BCOs的具体条件仍存在争议。本研究聚焦于风馈送型HMXBs，通过种群合成代码SEVN生成合成星表，并将其分配给66个类银河系星系样本，以此探究这种关联。利用TNG50宇宙学模拟中的恒星粒子，根据粒子质量、年龄和金属丰度分配HMXBs，并追踪其后续向BCOs的演化。通过这种方式，本方法为建模银河系中的HMXBs提供了现实框架，明确考虑了双星系统的不同金属丰度和空间分布。本方法重现了从观测到的银河系HMXBs性质推断出的空间分布：它们的位置遵循旋臂，与测量的径向分布一致；年龄分布与观测结果吻合良好，显示黑洞HMXBs（BH-HMXBs）倾向于比中子星HMXBs（NS-HMXBs）更年轻。研究发现，在哈勃时间内演化成并合BCOs的HMXBs占比，BH-HMXBs为~0.2-3.2%（若限定在10^35 ≤ L_X ≤ 10^40 erg s^-1范围内则为~0.3-5.4%），NS-HMXBs为~3.6-23.4%（相同光度范围下为~3.5-26.0%）。研究表明，公共包层（CE）阶段和诞生时的 kick 速度是决定并合系统数量的主要过程；成功的BCO并合通常由经历过显著轨道硬化（早期CE）的系统产生，而稳定的质量转移往往产生宽轨道、不并合的双星，除非 kick 引发极端偏心率；金属丰度的作用次要但重要，它会调节致密遗迹质量和风驱动的轨道加宽。
英文摘要
High-mass X-ray binaries (HMXBs) constitute a potential intermediate phase connecting massive stellar binaries to the formation of coalescing binary compact objects (BCOs). Yet, the specific circumstances that allow HMXBs to later develop into merging BCOs are still under debate. In this study, we focus on wind-fed HMXBs and investigate this link by generating synthetic catalogs with the population-synthesis code SEVN and assigning them to a sample of 66 Milky Way-like galaxies. Using stellar particles drawn from the TNG50 cosmological simulation, we assign HMXBs according to particle mass, age, and metallicity, and follow their subsequent evolution to BCOs. In this way, our approach provides a realistic framework for modelling HMXBs in the Milky Way by explicitly accounting for the varied metallicities and spatial distributions of binary systems. Our method recovers the spatial distribution inferred from the observed properties of Galactic HMXBs: their positions follow the spiral arms and agree with the measured radial profile. The age distribution aligns well with observations and shows that BH-HMXBs tend to be younger than NS-HMXBs. We find that the fraction of HMXBs that evolve into merging BCOs within a Hubble time for BH-HMXBs is ~0.2-3.2% (or ~0.3-5.4% when restricting to 10^35 <= L_X <= 10^40 erg s^-1), while for NS-HMXBs is ~3.6-23.4% (or ~3.5-26.0% with the same luminosity cut). We show that common envelope (CE) episodes and natal-kick magnitudes are the primary processes determining the number of merging systems. Successful BCO mergers are typically produced by systems that experienced significant orbital hardening (early CE), whereas stable mass transfer often yields wide, non-merging binaries unless extreme eccentricities are induced by kicks. Metallicity plays a secondary but important role by modulating compact-remnant masses and wind-driven orbital widening.
Comments17 pages, 14 figures
