Nambu-Jona-Lasinio模型下中子星物质的退禁闭
Deconfinement of neutron star matter within the Nambu-Jona-Lasinio model
摘要：
我们研究了中子星条件下强子物质到夸克物质的退禁闭跃迁，假设跃迁过程中色味守恒。我们使用两阶段描述。对于强子相，我们使用不同的参数化的非线性Walecka模型，其中包括整个重子八重态。对于夸克物质相，我们采用包含色超导的SU（3）_f Nambu-Jona-Lasinio有效模型。脱限制被认为是一个一级相变，保存颜色和味道。它给出了一个短暂的瞬态无色夸克相，它不处于β平衡，并衰变到τ ~ tau_{weak} ~ 10^{-8} s的稳定组态。然而，尽管是非常短暂的，过渡到这个中间阶段决定了转变的开始内部的中子星。我们找到了中子星内部典型温度下的跃迁自由能量密度.我们还发现了临界质量以上的紧凑型恒星应该包含一个夸克核心，并在其下，他们是安全的，相对于突然过渡到夸克物质。而独立于强子状态方程（EOS）的刚度，我们发现强子星（没有被捕获的中微子）的临界质量在1.5 - 1.8太阳质量的范围内。这与MIT Bag模型中获得的结果一致。
英文摘要：
We study the deconfinement transition of hadronic matter into quark matter under neutron star conditions assuming color and flavor conservation during the transition. We use a two-phase description. For the hadronic phase we use different parameterizations of a non-linear Walecka model which includes the whole baryon octet. For the quark matter phase we use an SU(3)_f Nambu-Jona-Lasinio effective model including color superconductivity. Deconfinement is considered to be a first order phase transition that conserves color and flavor. It gives a short-lived transitory colorless-quark-phase that is not in beta-equilibrium, and decays to a stable configuration in tau ~ tau_{weak} ~ 10^{-8} s. However, in spite of being very short lived, the transition to this intermediate phase determines the onset of the transition inside neutron stars. We find the transition free-energy density for temperatures typical of neutron star interiors. We also find the critical mass above which compact stars should contain a quark core and below which they are safe with respect to a sudden transition to quark matter. Rather independently on the stiffness of the hadronic equation of state (EOS) we find that the critical mass of hadronic stars (without trapped neutrinos) is in the range of ~ 1.5 - 1.8 solar masses. This is in coincidence with previous results obtained within the MIT Bag model.
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