论文标题
迅速旋转的紧凑型恒星具有解反性相变
Rapidly Spinning Compact Stars with Deconfinement Phase Transition
论文作者
论文摘要
我们研究了迅速旋转的紧凑型恒星，其状态方程是通过使用仪表/重力二元性，具有强耦合的核物质和脱糊状夸克物质之间的一阶相变。我们考虑一个模型家族，该系列允许纯粹统一旋转的恒星，质量约为$ 2.9 \，\ mathrm {m} _ \ odot $，因此与二级组件（$ 2.59^{+0.08} _ {+0.09} _ { - 0.09} $}的解释兼容。 GW190814是中子之星。这些恒星的核饱和度密度几倍，因此强耦合和非扰动效应变得至关重要。我们构建模型，其中最大静态（旋转）星$ m _ {\ mathrm {tov}} $（$ m _ {\ mathrm {max}} $）是由世俗的不稳定性或相变诱导的倒塌确定的。我们找到$ M _ {\ MathRM {Max}}/M _ {\ Mathrm {\ Mathrm {tov}} $的最大值，如果相变确定$ M _ {\ Mathrm {Maxrm {Max}} $，这将我们的拟合结果转移到$ m _ {\ mathrm {max}}}}} $ { 1.227^{+0.031} _ { - 0.016} $，一个值略高于Breu-Rezzolla绑定$ 1.203^{+0.022} _ { - 0.022} $从模型中推断出的，而没有相位过渡。
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, which allow purely hadronic uniformly rotating stars with masses up to approximately $2.9\, \mathrm{M}_\odot$, and are therefore compatible with the interpretation that the secondary component ($2.59^{+0.08}_{-0.09}\, \mathrm{M}_\odot$) in GW190814 is a neutron star. These stars have central densities 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 $M_{\mathrm{TOV}}$ ($M_{\mathrm{max}}$) is either determined by the secular instability or a phase transition induced collapse. We find largest values for $M_{\mathrm{max}}/M_{\mathrm{TOV}}$ in cases where the phase transition determines $M_{\mathrm{max}}$, which shifts our fit result to $M_{\mathrm{max}}/M_{\mathrm{TOV}} = 1.227^{+0.031}_{-0.016}$, a value slightly above the Breu-Rezzolla bound $1.203^{+0.022}_{-0.022}$ inferred from models without phase transition.
