论文标题
中子恒星动力学状态状态QCD方程：核-2Sc连续性和不断发展的有效耦合
Phenomenological QCD equations of state for neutron star dynamics: Nuclear-2SC continuity and evolving effective couplings
论文作者
论文摘要
我们通过为中子星动力学构建QCD状态方程来描述夸克 - 哈德隆的连续性，涵盖了广泛的电荷化学电位（$μ_Q$）和温度（$ t $）。基于核-2SC的连续性场景，我们匹配核和两种味的色彩效力（2Sc）夸克的状态方程，其中匹配的baryon密度为$ n_b \ simeq 1.5n_0 $（$ n_0 \ simeq 0.16 \ simeq 0.16 \，{\ rm fm fm fm^{\ rm fm^{ - 3} $：夸克物质模型中的有效矢量和diquark耦合演变为$ n_b，μ_q，t $的函数，其低密度值受核物质性能和中子星形radii的约束，其高密度行为由两极质量质量（$ 2M_ \ odot $）约束。耦合取决于$ n_b $，我们检查了核-2Sc连续性的光滑程度，并在低温下发现了与核和2SC熵相匹配的问题。为了进行连续性方案，我们通过制作耦合（$ n_b，μ_q，t $） - 依赖来实施平滑匹配。实际上，这增加了我们称为“ x”的现象学贡献。在现象学匹配之后，我们将其余的作为我们的预测。用这些不断发展的耦合计算的2SC和颜色塑料（CFL）相称为2SCX和CFLX。 CFLX出现在$ n_b \ simeq 2 $ - $ 4N_0 $左右，与常规CFL相反，对$（μ_Q，t）$的依赖性不高。为了检查我们的建模的天体物理后果，我们添加了带电的叶子和中微子，并研究了与原子恒星和中子恒星合并相关的Lepton级分的物质组成。中微子的丰度和热效应减少了陌生部分和状态方程。对于$ t \ simeq 30 $ meV的中微子捕获的中子星，带有Lepton分数$ y_l \ simeq 0.05 $，质量比其冷静态对应物大于$ \ sim 0.1m_ \ odot $。
We delineate the quark-hadron continuity by constructing QCD equations of state for neutron star dynamics, covering the wide range of charge chemical potential ($μ_Q$) and temperatures ($T$). Based on the nuclear-2SC continuity scenario, we match equations of state for nuclear and two-flavor color-superconducting (2SC) quark matter, where the matching baryon density is $n_B\simeq 1.5n_0$ ($n_0\simeq 0.16\, {\rm fm^{-3}}$: nuclear saturation density). The effective vector and diquark couplings in a quark matter model evolve as functions of $n_B, μ_Q, T$, whose low density values are constrained by the nuclear matter properties and neutron star radii, with the high density behavior by the two-solar mass ($2M_\odot$) constraint. With couplings dependent on $n_B$, we examined how smooth the nuclear-2SC continuity can be, and found problems in matching nuclear and 2SC entropies at low temperatures. To proceed with the continuity scenario, we enforce smooth matching by making the couplings ($n_B, μ_Q, T$)-dependent. In effect, this adds phenomenological contributions which we call "X". After the phenomenological matching, we take the rest as our predictions. The 2SC and color-flavor-locked (CFL) phases computed with these evolving couplings are called 2SCX and CFLX. The CFLX appears around $n_B\simeq 2$-$4n_0$ and, in contrast to the conventional CFL, has non-negligible dependence on $(μ_Q,T)$. To examine the astrophysical consequences of our modeling, we add charged leptons and neutrinos, and study the composition of matter for lepton fractions relevant for protoneutron stars and neutron star mergers. The abundance of neutrinos and thermal effects reduce the strangeness fraction and stiffen equations of state. For a neutrino trapped neutron star at $T\simeq 30 $ MeV with a lepton fraction $Y_L\simeq 0.05$, the mass is larger than its cold static counterpart by $\sim 0.1M_\odot$.
