协变密度泛函状态方程系综中中子星内玻色子暗物质的贝叶斯约束

中文摘要 AI 辅助

我们利用当前的多信使观测数据，研究了与具有排斥性自相互作用的玻色子暗物质（DM）混合的中子星。暗物质组分被建模为一个复标量场，仅通过引力与重子物质耦合，从而允许暗核和暗晕两种构型。为了量化重子状态方程（EOS）的不确定性，我们将对 $(m_\chi,\lambda,F_\chi)$ 的三维扫描与27个基于DDME2的协变密度泛函EOS相结合，这些EOS覆盖了 $L_{\rm sym}=30,50,70$ MeV 和 $-600\le Q_{\rm sat}\le 1000$ MeV 的范围。在贝叶斯框架下，我们将这些模型与来自阿姆斯特丹和马里兰/伊利诺伊分析的NICER质量-半径测量以及GW170817潮汐形变约束进行对比。在对EOS系综进行贝叶斯证据加权后，与EOS相关的暗部门尺度 $\mu_\chi\equiv m_\chi/\lambda^{1/4}$ 在两组NICER数据中都被定位在约250 MeV附近。在 $(m_\chi,\lambda)$ 参数化中，边缘化的玻色子质量后验分布在 $m_\chi\simeq300$--$330$ MeV 处达到峰值，而 $\lambda$ 则保持广泛分布。由于玻色子EOS仅通过 $\mu_\chi$ 依赖于 $m_\chi$ 和 $\lambda$，它们各自的边缘分布取决于所采用的独立先验。推断出的DM分数更依赖于数据集，马里兰/伊利诺伊分析的后验模式接近4%，而阿姆斯特丹分析则接近12%。玻色子DM还将推断出的 $Q_{\rm sat}$ 从负值向中间值和正值移动，而 $L_{\rm sym}$ 的响应较弱。这表明DM引起的致密化与重子物质的高密度刚度之间存在模型依赖的权衡。这些约束仍然取决于所选的EOS族以及对所有源采用共同有效 $F_\chi$ 的假设。

英文摘要

We investigate neutron stars admixed with repulsively self-interacting bosonic dark matter (DM) using current multi-messenger observations. The dark component is modeled as a complex scalar field coupled to baryonic matter only through gravity, allowing dark-core and dark-halo configurations. To quantify baryonic equation-of-state (EOS) uncertainties, we combine a three-dimensional scan over $(m_χ,λ,F_χ)$ with 27 DDME2-based covariant density-functional EOSs spanning $L_{\rm sym}=30,50,70$ MeV and $-600\le Q_{\rm sat}\le 1000$ MeV. The models are confronted in a Bayesian framework with NICER mass--radius measurements from the Amsterdam and Maryland/Illinois analyses and the GW170817 tidal-deformability constraint. After Bayesian evidence weighting over the EOS ensemble, the EOS-relevant dark-sector scale $μ_χ\equiv m_χ/λ^{1/4}$ is localized around 250 MeV for both NICER data sets. In the $(m_χ,λ)$ parameterization, the marginalized boson-mass posterior peaks at $m_χ\simeq300$--$330$ MeV, while $λ$ remains broadly distributed. Since the bosonic EOS depends on $m_χ$ and $λ$ only through $μ_χ$, their separate marginals are conditional on the adopted independent priors. The inferred DM fraction is more data-set dependent, with posterior modes near 4% for Maryland/Illinois and 12% for Amsterdam. Bosonic DM also shifts the inferred $Q_{\rm sat}$ from negative toward intermediate and positive values, whereas the response of $L_{\rm sym}$ is weaker. This indicates a model-dependent trade-off between DM-induced compactification and the high-density stiffness of baryonic matter. These constraints remain conditional on the selected EOS family and the assumption of a common effective $F_χ$ for all sources.

发表机构

• University of Wrocław（弗罗茨瓦夫大学）
• Institute of Theoretical Physics, University of Wrocław（弗罗茨瓦夫大学理论物理研究所）
• Alikhanyan National Science Laboratory (Yerevan Institute of Physics)（阿利哈尼扬国家科学实验室（埃里温物理研究所））
• Frankfurt Institute for Advanced Studies（法兰克福高级研究所）

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