论文标题
核物质和中子星的统一弱/强耦合框架
Unified weak/strong coupling framework for nuclear matter and neutron stars
论文作者
论文摘要
使用弱相互作用核子的摘要方法可以很好地描述与核饱和密度相当的密度的凝结核物质。在较高的密度下，重叠的核子之间的强烈相互作用变得很重要。我们建议，相互作用将不断切换到该区域中的全息模型。为了实施此功能，我们构建了各种模型用于低密度核物质的状态（EOSS）的混合方程，并且全息V-QCD模型用于非扰动高密度核物质以及夸克物质。我们仔细检查了紧凑型恒星天体物理学的所有现有限制，并讨论了它们对混合EOSS的影响。多亏了V-QCD EOS核物质的刚度，我们获得了一个可行的混合eoss的大家庭。我们发现，由于强烈的一阶解束过渡，中子恒星中的夸克物质岩心是不稳定的，并且可以预测潮汐变形性以及中子星的半径上的界限。通过依靠普遍关系，我们还限制了中子星合并产生的引力波的特征峰值频率。
Ab initio methods using weakly interacting nucleons give a good description of condensed nuclear matter up to densities comparable to the nuclear saturation density. At higher densities palpable strong interactions between overlapping nucleons become important; we propose that the interactions will continuously switch over to follow a holographic model in this region. In order to implement this, we construct hybrid equations of state (EoSs) where various models are used for low density nuclear matter, and the holographic V-QCD model is used for non-perturbative high density nuclear matter as well as for quark matter. We carefully examine all existing constraints from astrophysics of compact stars and discuss their implications for the hybrid EoSs. Thanks to the stiffness of the V-QCD EoS for nuclear matter, we obtain a large family of viable hybrid EoSs passing the constraints. We find that quark matter cores in neutron stars are unstable due to the strongly first order deconfinement transition, and predict bounds on the tidal deformability as well as on the radius of neutron stars. By relying on universal relations, we also constrain characteristic peak frequencies of gravitational waves produced in neutron star mergers.
