We study rapidly spinning compact stars with equations of state featuring a first-order phase transition between strongly coupled nuclear matter and deconfined quark matter by employing the gauge/gravity duality. We consider a family of models that allow purely hadronic uniformly rotating stars with masses up to approximately 2.9 M _⊙, and are therefore compatible with the interpretation that the secondary component () in GW190814 is a neutron star. These stars have central densities that are several times the nuclear saturation density, so that strong coupling and non-perturbative effects become crucial. We construct models where the maximal mass of static (rotating) stars M _TOV (M _max) is either determined by the secular instability or a phase-transition induced collapse. We find the largest values for M _max/M _TOV in cases where the phase transition determines M _max, which shifts our fit result to , a value slightly above the Breu–Rezzolla bound inferred from models without phase transition.

我们通过利用轨距/重力对偶性研究状态方程式快速旋转的紧凑型恒星，该方程式具有强耦合核物质和无约束夸克物质之间的一阶相变。我们认为，一个家庭的模式，使纯粹的强子均匀旋转的恒星与群众多达约2.9中号 _⊙，并因此与解释，即二次成分（兼容于GW190814）是中子星。这些恒星的中心密度是核饱和密度的几倍，因此强耦合和非扰动效应变得至关重要。我们构建的模型中静态（旋转）恒星的最大质量M _TOV（M _max或由长期不稳定性决定，或由相变引起的坍塌决定。在相变确定M _max的情况下，我们找到了M _max / M _{TOV的最大值}，这将我们的拟合结果偏移到，该值略高于从没有相变模型推断出的Breu-Rezzolla界。