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arXiv 2006.00839nucl-thastro-ph.HEastro-ph.SR
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利用中子星的多信使观测在夸克平均场模型中约束强子-夸克相变参数

Constraining hadron-quark phase transition parameters within the quark-mean-field model using multimessenger observations of neutron stars

Zhiqiang Miao, Ang Li, Zhenyu Zhu, Sophia Han

备注：
15 pages, 12 figures, 1 table, version accepted for publication in ApJ
发表信息：
ApJ 904, 103 (2020)
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摘要：

本文推广了夸克平均场模型，研究了中子星核内夸克物质的可能存在。将强子相的QMF与高密度夸克相的“恒声速”参数化相结合，实现了一个尖锐的强子-夸克相变。系统地研究了核对称性能量斜率参数$L$和无量纲相变参数（跃迁密度$n_{\rm trans}/n_0$、跃迁强度$Δ\varepsilon/\varepsilon_{\rm trans}$和夸克物质声速平方$c^2_{\rm QM}$）的相互作用对混合星性质的影响，特别是对最大质量$M_{\rm max}$和典型$1.4 \,M_{\odot}$星的半径和潮汐形变的影响.我们证明了对称能量斜率$L$和典型恒星半径$R_{1.4}$之间的强相关性，类似于之前在没有相变的中子星中发现的相关性。通过引入相变，我们得到了$1.4 \,M_{\odot}$星的最大质量（$M_{\rm max}< 3.6 \,M_{\odot}$）和半径（$R_{1.4}\gtrsim 9.6~\rm km$）的鲁棒极限，并发现在低密度$\lesssim 1.3-1.5 \, n_0$下发生的太弱的（$Δ\varepsilon/\varepsilon_{\rm trans}\lesssim 0.2$）相变是非常不利的.我们还表明，未来的测量半径和潮汐变形的$\sim 1.4 \,M_{\odot}$明星，以及质量测量非常大的恒星，可以帮助揭示夸克物质的存在和数量在紧凑的对象。

英文摘要：

We extend the quark mean-field (QMF) model for nuclear matter and study the possible presence of quark matter inside the cores of neutron stars. A sharp first-order hadron-quark phase transition is implemented combining the QMF for the hadronic phase with "constant-speed-of-sound" parametrization for the high-density quark phase. The interplay of the nuclear symmetry energy slope parameter, $L$, and the dimensionless phase transition parameters (the transition density $n_{\rm trans}/n_0$, the transition strength $Δ\varepsilon/\varepsilon_{\rm trans}$, and the sound speed squared in quark matter $c^2_{\rm QM}$) are then systematically explored for the hybrid star proprieties, especially the maximum mass $M_{\rm max}$ and the radius and the tidal deformability of a typical $1.4 \,M_{\odot}$ star. We show the strong correlation between the symmetry energy slope $L$ and the typical stellar radius $R_{1.4}$, similar to that previously found for neutron stars without a phase transition. With the inclusion of phase transition, we obtain robust limits on the maximum mass ($M_{\rm max}< 3.6 \,M_{\odot}$) and the radius of $1.4 \,M_{\odot}$ stars ($R_{1.4}\gtrsim 9.6~\rm km$), and we find that a too-weak ($Δ\varepsilon/\varepsilon_{\rm trans}\lesssim 0.2$) phase transition taking place at low densities $\lesssim 1.3-1.5 \, n_0$ is strongly disfavored. We also demonstrate that future measurements of the radius and tidal deformability of $\sim 1.4 \,M_{\odot}$ stars, as well as the mass measurement of very massive pulsars, can help reveal the presence and amount of quark matter in compact objects.

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