中子星中的暗物质：全广义相对论下的双流体 $f$-模振荡
Dark matter in neutron stars: two-fluid $f$-mode oscillations in full general relativity
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中文总结 AI 辅助
本研究在全广义相对论下计算中子星与暗物质混合的f模振荡，发现核心暗物质主导阻尼时间随暗物质分数按F^-2规律急剧缩短，而晕暗物质则相反，为区分暗物质与软核方程提供新探针。
中文摘要 AI 辅助
暗物质核心和软的核状态方程可以产生相似的质量-半径特征，这促使通过 $f$-模谱进行互补探测。我们在全广义相对论框架下，计算了与自相互作用玻色子暗物质（DM）混合的冷、非旋转中子星的四极 $f$-模频率和引力波阻尼时间。我们的双流体研究覆盖了21种核状态方程，包括核子、超子、$\triangle$-混合以及超子-$\triangle$组合成分，暗物质质量分数 $F_{\rm DM}=1$-$20\\%$。主序列分别采用 $\u03bb=\u03c0$ 和玻色子质量 $500$ 和 $100\\,\mathrm{MeV}$ 用于核心和晕研究。独立的正常物质（NM）和暗物质位移通过度规耦合，产生NM主导和DM主导的 $f$-模分支，其辐射阻尼由出射波边界条件决定。在 $1.4\\,M_\odot$ 质量下，核心DM主导的阻尼时间从 $F_{\rm DM}=1\\%$ 时的 $10^3\\,\mathrm{s}$ 量级减少到 $20\\%$ 时的 $1\\,\mathrm{s}$ 量级，大致遵循经验性的 $F_{\rm DM}^{-2}$ 依赖关系，而NM主导的阻尼时间保持在 $0.12$-$0.33\\,\mathrm{s}$ 范围内。晕DM主导的阻尼反而随暗物质分数增加而增加：在相同恒星质量和 $F_{\rm DM}=20\\%$ 时，暗物质半径接近 $88\\,\mathrm{km}$，频率降至 $0.14\\,\mathrm{kHz}$，阻尼时间达到约 $450\\,\mathrm{s}$。选定的高质量核心序列表现出强烈的DM主导阻尼时间上升，这无法由领先的质量四极诊断重现。代表性的核心计算显示，DM主导对玻色子自耦合的敏感性更高，并在 $\ell=3$ 时保留两个分支。在采用的非旋转、圆轨道双星预设下，没有评估的构型满足所有几何和微扰条件以实现受控的线性潮汐共振。
英文摘要
A dark-matter core and a soft nuclear equation of state can produce similar mass--radius signatures, motivating a complementary probe through the $f$-mode spectrum. We compute quadrupolar $f$-mode frequencies and gravitational-wave damping times in full general relativity for cold, nonrotating neutron stars admixed with self-interacting bosonic dark matter (DM). Our two-fluid survey spans 21 nuclear equations of state covering nucleonic, hyperonic, $Δ$-admixed, and combined hyperon--$Δ$ compositions at $F_{\rm DM}=1$--$20\%$. The main sequences use $λ=π$ and boson masses of $500$ and $100\,\mathrm{MeV}$ for the core and halo studies, respectively. Independent normal-matter (NM) and DM displacements couple through the metric, yielding NM-led and DM-led $f$-mode branches whose radiative damping is determined by outgoing-wave boundary conditions. At $1.4\,M_\odot$, the core DM-led damping time decreases from order $10^3\,\mathrm{s}$ at $F_{\rm DM}=1\%$ to order $1\,\mathrm{s}$ at $20\%$, approximately following an empirical $F_{\rm DM}^{-2}$ dependence, while NM-led damping times remain within $0.12$--$0.33\,\mathrm{s}$. Halo DM-led damping instead increases with dark fraction: at the same stellar mass and $F_{\rm DM}=20\%$, dark radii approach $88\,\mathrm{km}$, frequencies fall to $0.14\,\mathrm{kHz}$, and damping times reach approximately $450\,\mathrm{s}$. Selected high-mass core sequences exhibit strong DM-led damping-time upturns not reproduced by the leading mass-quadrupole diagnostic. Representative core calculations show greater DM-led sensitivity to the bosonic self-coupling and retain both branches at $\ell=3$. Under the adopted nonrotating, circular-binary prescriptions, no evaluated configuration satisfies all geometric and perturbative conditions for a controlled linear tidal resonance.
发表机构
- Yonsei University（延世大学）
- Goethe Universität（歌德大学）
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