发表机构
Johns Hopkins University; Indian Institute of Astrophysics; Inter-University Centre for Astronomy and Astrophysics; Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências da Universidade de Lisboa; Departamento de Física, Faculdade de Ciências da Universidade de Lisboa（约翰斯·霍普金斯大学; 印度天体物理研究所; 大学间天文与天体物理中心; 里斯本大学理学院空间科学与天体物理研究所; 里斯本大学理学院物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该论文提出一个以包围质量函数参数化黑洞周围暗物质环境的新框架，研究其对准正则模、潮汐洛夫数及极端质量比旋进引力波通量的影响，发现不同观测对晕结构具有互补敏感性。
AI 中文摘要
天体物理黑洞（BHs）并非孤立的真空天体，而是预期存在于复杂环境中，例如暗物质（DM）晕和重子分布。此类环境可改变黑洞周围的时空几何，并在引力波（GW）信号上留下可观测印记，包括准正则模（QNM）频谱的偏移、潮汐洛夫数（TLNs）以及极端质量比旋进（EMRIs）的旋进动力学。我们开发了一个描述暗物质包裹黑洞时空的一般框架，直接以包围质量函数参数化几何，而非传统的基于密度的轮廓。这种基于质量的表述自然与总引力场相关联，可容纳几种常见晕轮廓作为极限情况，并纳入基本物理一致性要求，如正则性、因果性和适当的渐近行为。在此框架内，我们研究了环境对QNM、TLN和来自EMRI的引力波通量的印记。我们发现对晕结构的互补敏感性：QNM主要探测环境内部区域，而静态TLN对其外部结构更敏感。相比之下，EMRI通量通过其对轨道运动和引力波传播的影响来探测物质分布。我们的结果确立了包围质量表述作为一个灵活且物理可控的框架，用于连接天体物理环境模型与精密引力波可观测。
英文摘要
Astrophysical black holes (BHs) are not isolated vacuum objects but are expected to reside within complex environments, such as dark matter (DM) halos and baryonic distributions. Such environments can modify the spacetime geometry surrounding the BH and leave observable imprints on gravitational-wave (GW) signals, including shifts in the quasinormal mode (QNM) spectrum, tidal Love numbers (TLNs), and the inspiral dynamics of extreme-mass-ratio inspirals (EMRIs). We develop a general framework for describing DM-dressed BH spacetimes by parameterizing the geometry directly in terms of the enclosed mass function, rather than the traditional density-based profile. This mass-based formulation is naturally connected to the total gravitational field, accommodates several common halo profiles as limiting cases, and incorporates basic physical consistency requirements such as regularity, causality, and appropriate asymptotic behavior. Within this framework, we investigate the environmental imprints on QNMs, TLNs, and GW fluxes from EMRIs. We find a complementary sensitivity to the halo structure: QNMs predominantly probe the inner regions of the environment, whereas static TLNs are more sensitive to its outer structure. EMRI fluxes, in contrast, probe the matter distribution through its influence on the orbital motion and GW propagation. Our results establish the enclosed-mass formulation as a flexible and physically controlled framework for connecting astrophysical environment models with precision GW observables.
Comments18 pages, 12 figures, 1 table
