强子中子星、夸克星和混合星的非径向振荡：$f$、$p$ 和 $g$ 模频率的计算
Non-radial oscillations of hadronic neutron stars, quark stars, and hybrid stars : Calculation of $f$, $p$, and $g$ mode frequencies
AI总结：
本研究计算了强子星、夸克星和混合星的非径向振荡频率，发现组成显著影响频率，但质量标度f模频率随致密性普遍变化，且g模频率与潮汐形变率线性相关，可支持混合星存在并揭示夸克排斥强度。
摘要：
与致密星相关的致密物质的组成和状态方程（EoS）尚无定论。然而，对致密星结构性质的某些观测约束有助于我们在相当程度上限制EoS。此外，引力星震学可以给出致密星组成和EoS的概念。下一代引力波（GW）探测器很可能探测到GW的多个振荡模频率。在本工作中，我们计算了基模（$f$）和第一压力模（$p_1$）的频率（分别为$f_f$和$f_{p1}$），对应不同的组成，即强子星（HS）、夸克星和混合星物质。对于混合星，我们还研究了重力模（$g$）的频率（$f_g$）。对于每个相，我们还研究了1.4 $M_{\odot}$和2.01 $M_{\odot}$致密星的振荡频率与其他不同性质之间的相关性。我们发现，致密星的各种可能组成显著影响振荡频率。然而，质量标度的角$f$模频率（$\omega_f M$）对所有强子星、夸克星和混合星都随致密性（$C$）普遍变化。用不同组成得到的典型1.4 $M_{\odot}$致密星的$f$模频率（$f_{f_{1.4}}$）与典型半径（$R_{1.4}$）和潮汐形变率（$\Lambda_{1.4}$）相当相关，而$f_{p_{1.4}}$与对称能量斜率参数相关性良好。我们还表明，混合星的$f_{g_{1.4}}$几乎随$\Lambda_{1.4}$线性变化。如果探测到$g$模，它们不仅能支持混合星的存在，而且$f_g$可能有助于理解混合星中夸克排斥的强度。
英文摘要：
The composition and equation of state (EoS) of dense matter relevant to compact stars are quite inconclusive. However, certain observational constraints on the structural properties of compact stars help us constrain the EoS to a fair extent. Moreover, gravitational asteroseismology gives a notion of the composition and EoS of compact stars. The next generation gravitational wave (GW) detectors are likely to detect several oscillation mode frequencies of the GWs. In this work we compute the fundamental ($f$) and the first pressure ($p_1$) mode frequencies ($f_f$ and $f_{p1}$, respectively) with different compositions viz., hadronic, quark, and hybrid star (HS) matter. For HSs, we also study the gravity ($g$) mode frequency ($f_g$). For each phase we also study the correlation between the oscillation frequencies of 1.4 $M_{\odot}$ and 2.01 $M_{\odot}$ compact stars with other different properties. We find that various possible composition of compact stars substantially affects the oscillation frequencies. However, the mass-scaled angular $f$ mode frequency ($ω_f M$) varies universally with compactness ($C$) for all hadronic, quark and hybrid stars. The $f$ mode frequency ($f_{f_{1.4}}$) of the canonical 1.4 $M_{\odot}$ compact star, obtained with different composition, is quite correlated with the canonical radius ($R_{1.4}$) and tidal deformability ($Λ_{1.4}$) while $f_{p_{1.4}}$ is well correlated with slope parameter of the symmetry energy. We also show that $f_{g_{1.4}}$ of the HSs varies almost linearly with $Λ_{1.4}$. Should $g$ modes be detected, they could not only support the existence of HSs, but $f_g$ could be useful to understand the strength of quark repulsion in HSs.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
