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arXiv 2203.05461gr-qcastro-ph.HEnucl-th
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双中子星并合作为夸克-强子交叉状态方程探针

Binary neutron star mergers as a probe of quark-hadron crossover equations of state

Atul Kedia, Hee Il Kim, In-Saeng Suh, Grant J. Mathews

AI总结:

本研究首次模拟采用夸克-强子交叉状态方程的双中子星并合,发现其引力波频率呈双重特征,为探测高密度夸克物质提供关键证据。

摘要:

预计未来引力波(GW)探测器探测到的来自双中子星(NS)并合的引力辐射可以探测高密度状态方程(EOS)。我们首次进行了采用夸克-强子交叉(QHC)EOS各种参数化的双中子星并合模拟。这些EOS由强子EOS($n_{b} < 2~n_0$)和夸克物质EOS($n_{b} >~5~n_0$)的组合构建,其中$n_{b}$和$n_0$分别是重子数密度和核饱和密度。在交叉密度($2~ n_0 < n_{b} < 5~ n_0$)下,QHC EOS连续软化,同时保持比强子EOS和一级相变EOS更硬,达到强关联夸克物质的硬度。这种增强的硬度导致并合后中子星的寿命显著长于纯强子EOS的情况。我们发现这些EOS具有双重性质:其最大啁啾引力波频率$f_{max}$属于软EOS类别,而并合后阶段的主峰频率($f_{peak}$)介于软和硬强子EOS之间。在特征引力波频率中观测到这种双重性质将为QCD交叉密度下强相互作用夸克物质的存在提供关键证据。

英文摘要:

It is anticipated that the gravitational radiation detected in future gravitational wave (GW) detectors from binary neutron star (NS) mergers can probe the high-density equation of state (EOS). We perform the first simulations of binary NS mergers which adopt various parametrizations of the quark-hadron crossover (QHC) EOS. These are constructed from combinations of a hadronic EOS ($n_{b} < 2~n_0$) and a quark-matter EOS ($n_{b} >~5~n_0$), where $n_{b}$ and $n_0$ are the baryon number density and the nuclear saturation density, respectively. At the crossover densities ($2~ n_0 < n_{b} < 5~ n_0$) the QHC EOSs continuously soften, while remaining stiffer than hadronic and first-order phase transition EOSs, achieving the stiffness of strongly correlated quark matter. This enhanced stiffness leads to significantly longer lifetimes of the postmerger NS than that for a pure hadronic EOS. We find a dual nature of these EOSs such that their maximum chirp GW frequencies $f_{max}$ fall into the category of a soft EOS while the dominant peak frequencies ($f_{peak}$) of the postmerger stage fall in between that of a soft and stiff hadronic EOS. An observation of this kind of dual nature in the characteristic GW frequencies will provide crucial evidence for the existence of strongly interacting quark matter at the crossover densities for QCD.

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。

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