发表机构
Institute for Basic Science (IBS)（基础科学研究院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出利用致密双星旋进引力波信号中的D函数，通过回归框架重建暗物质密度分布与状态方程，为探测暗物质宏观性质提供新途径。
AI 中文摘要
我们研究了嵌入在流体静力学平衡的扩展暗物质（DM）构型中的致密双星系统的引力波（GW）特征。如果一颗中子星被一个质量足够大且范围足够广的包层所包围，那么旋进的伴星除了标准的引力波能量损失外，还会经历动力学摩擦（DF）。我们表明，这种环境效应可以通过一个引力波可观测量——$D$函数——来隔离，该函数直接表征了由周围介质引起的额外耗散功率。由于包层的密度由暗物质状态方程连同恒星边界条件直接决定，$D$函数的频率依赖性提供了关于暗区宏观性质的直接信息。我们开发了一个基于回归的框架，以在引力波旋进观测所探测的密度范围内重建密度分布和暗物质状态方程。使用具有代表性的暗物质模型作为基准，我们证明了该方法能够准确恢复输入的状态方程，同时在很大程度上独立于暗物质的微观实现。我们的结果表明，未来对致密双星的引力波观测可以提供对暗物质状态方程的探测手段。
英文摘要
We investigate the gravitational wave (GW) signatures of compact binaries embedded in extended dark matter (DM) configurations in hydrostatic equilibrium. If a neutron star is surrounded by a sufficiently massive and extended envelope, an inspiraling companion experiences dynamical friction (DF) in addition to the standard GW energy loss. We show that this environmental effect can be isolated through a GW observable, the $D$-function, which directly characterizes the additional dissipative power induced by the surrounding medium. Since the density of the envelope is directly determined by the DM equation of state together with the stellar boundary conditions, the frequency dependence of the $D$-function provides direct information about the macroscopic properties of the dark sector. We develop a regression-based framework to reconstruct both the density profile and the DM equation of state over the density range probed by observations of the GW inspiral. Using representative DM models as benchmarks, we demonstrate that the method accurately recovers the input equation of state while remaining largely independent of the microscopic realization of DM. Our results show that future GW observations of compact binaries can provide a probe of the equation of state of DM.
Comments35 pages, 8 figures
