论文标题
具有全息多Quark核心的大型中子星星
Massive neutron stars with holographic multiquark cores
论文作者
论文摘要
核物质的阶段对于确定中子星的物理特性至关重要。在NS的核心中，密度和压力变得如此之大，以至于核物质可能会经历相过渡到一个脱卷相，由夸克和胶子及其颜色结合的状态组成。即使在超相关的重型离子碰撞中观察到了夸克 - 胶状等离子体\ cite {gyulassy，andronic}，但仍不清楚中子恒星内是否存在异国情调的夸克物质。最新的结果来自各种扰动理论计算与天文学观察的组合\ cite {demorest，antoniadis}表明，（异国情调的）夸克物质可能存在于2.0太阳能大量高于2.0太阳能（$ m _ {\ odot} $ _ {\ odot} $）的核心内。我们在参考文献中重新审视全息模型{bch，bhp}，并实施多Quark核物质的状态〜（EOS）方程，以插入高密度EOS在高密度下已知的核EOS的PQCD EOS。对于模型的足够大的能量密度量表〜（$ε_{s} $），发现多Quark相比过渡点上方的刚性核物质比热力学相比。具有全息多Quark核心的NS可能在$ 1.96-2.23〜（1.64-2.10）M _ {\ odot} $和Radii $ 14.3-11.8〜（14.0-11.1.1）$ km $ 14.3-11.8〜（14.0-11.1）$ km for $ε_{s} = 26〜（28）$ GEEV/fm $ gm $ gm $^} $ 14.3-11.8〜（14.0-11.1）$ 14.3-11.8〜（14.0-11.1）$ 14.3-11.8〜（14.0-11.1）$ 14.3-11.8〜（14.0.0-11.1）$ 14.3-11.8〜（14.0-11.1）研究了某些类型的Baryonic EOS的质子 - 巴里子级分的作用；较大的质子分数可以将多Quark核心的NS半径降低不到一公里。
Phases of nuclear matter are crucial in the determination of physical properties of neutron stars~(NS). In the core of NS, the density and pressure become so large that the nuclear matter possibly undergoes phase transition into a deconfined phase, consisting of quarks and gluons and their colour bound states. Even though the quark-gluon plasma has been observed in ultra-relativistic heavy-ion collisions\cite{Gyulassy, Andronic}, it is still unclear whether exotic quark matter exists inside neutron stars. Recent results from the combination of various perturbative theoretical calculations with astronomical observations\cite{Demorest, Antoniadis} shows that (exotic) quark matter could exist inside the cores of neutron stars above 2.0 solar masses ($M_{\odot}$)~\cite{Annala:2019puf}. We revisit the holographic model in Ref.~\cite{bch, bhp} and implement the equation of states~(EoS) of multiquark nuclear matter to interpolate the pQCD EoS in the high-density region with the nuclear EoS known at low densities. For sufficiently large energy density scale~($ε_{s}$) of the model, it is found that multiquark phase is thermodynamically prefered than the stiff nuclear matter above the transition points. The NS with holographic multiquark core could have masses in the range $1.96-2.23~(1.64-2.10) M_{\odot}$ and radii $14.3-11.8~(14.0-11.1)$ km for $ε_{s}=26~(28)$ GeV/fm$^{3}$ respectively. Effects of proton-baryon fractions are studied for certain type of baryonic EoS; larger proton fractions could reduce radius of the NS with multiquark core by less than a kilometer.
