双黑洞层级形成的唯象物理建模 1：基于球状星团模拟的 GWTC 合成宇宙
Physics-based phenomenological modeling of binary black hole hierarchical formation 1: Synthetic universes from globular cluster simulations for GWTC
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中文总结 AI 辅助
该研究通过三成分模型（球状星团模拟、孤立双星场通道和中等质量各向同性成分）迭代拟合GWTC-5.0双黑洞数据，预测质量谱断裂和自旋分布特征，为层级形成提供可检验的物理归一化框架。
中文摘要 AI 辅助
我们使用三个成分对 GWTC-5.0 双黑洞普查进行迭代建模。首先，来自 Rapster 球状星团模拟的物理归一化星族覆盖了星团质量、金属丰度、形成红移、致密度和原生黑洞自旋。层级并合能够重现高质量事件及其更大的有效自旋弥散，前提是黑洞以零原生自旋诞生。其次，一个唯象场（孤立双星）通道提供了低质量、优先对齐的星族。该通道的加入使星团致密度的似然函数变得平坦，从而允许普通的致密球状星团诞生半径，而无需类似核星团的条件。最后，在 $15$--$30 M_\odot$ 范围内的残余张力促使引入一个中等质量的各向同性成分，代表在星团中再处理的场遗迹。这是一个假设，而非探测：当前的数值支持不足以进行可靠的证据比较。物理归一化将高质量率转换为 $\hat{f}_{\rm GC}\simeq0.39\\%$，局部率 $R_{\rm cl}\simeq9.1$ 和 $R_{\rm field}\simeq16.0$ Gpc$^{-3}$ yr$^{-1}$。该模型预测了在 $35$ 和 $70 M_\odot$ 附近关联的质量谱断裂、由第一代与第二代配对产生的 $q\simeq0.5$ 特征，以及在 $45 M_\odot$ 以上急剧展宽的对称有效自旋分布。随着引力波普查的增长，这些相关的、质量分辨的预测可以被检验。
英文摘要
We iteratively model the GWTC-5.0 binary-black-hole census with three components. First, a physically normalized population from Rapster globular-cluster simulations spans cluster mass, metallicity, formation redshift, compactness, and natal black-hole spin. Hierarchical mergers reproduce higher-mass events and their larger effective-spin dispersion, provided black holes are born with zero natal spin. Second, a phenomenological field (isolated-binary) channel supplies the low-mass, preferentially aligned population. Its inclusion flattens the cluster compactness likelihood, permitting ordinary dense globular-cluster birth radii without requiring nuclear-cluster-like conditions. Finally, residual tension at $15$--$30 M_\odot$ motivates an intermediate-mass isotropic component representing field remnants reprocessed in clusters. This is a hypothesis, not a detection: current numerical support precludes a reliable evidence comparison. Physical normalization converts the high-mass rate into $\hat{f}_{\rm GC}\simeq0.39\%$, with local rates $R_{\rm cl}\simeq9.1$ and $R_{\rm field}\simeq16.0$ Gpc$^{-3}$ yr$^{-1}$. The model predicts linked mass-spectrum breaks near $35$ and $70 M_\odot$, a $q\simeq0.5$ feature from first-plus-second-generation pairings, and a symmetric effective-spin distribution that broadens sharply above $45 M_\odot$. These correlated, mass-resolved predictions can be tested as the gravitational-wave census grows.
发表机构
- Center for Computational Relativity and Gravitation, Rochester Institute of Technology（罗切斯特理工学院计算相对论与引力中心）
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