Title: Uniformly rotating neutron stars Show Chinese title

Title: 均匀旋转的中子星

Abstract: In this chapter we review the recent results on the equilibrium configurations of static and uniformly rotating neutron stars within the Hartle formalism. We start from the Einstein-Maxwell-Thomas-Fermi equations formulated and extended by Belvedere et al. (2012, 2014). We demonstrate how to conduct numerical integration of these equations for different central densities ${\it \rho}_c$ and angular velocities $\Omega$ and compute the static $M^{stat}$ and rotating $M^{rot}$ masses, polar $R_p$ and equatorial $R_{\rm eq}$ radii, eccentricity $\epsilon$, moment of inertia $I$, angular momentum $J$, as well as the quadrupole moment $Q$ of the rotating configurations. In order to fulfill the stability criteria of rotating neutron stars we take into considerations the Keplerian mass-shedding limit and the axisymmetric secular instability. Furthermore, we construct the novel mass-radius relations, calculate the maximum mass and minimum rotation periods (maximum frequencies) of neutron stars. Eventually, we compare and contrast our results for the globally and locally neutron star models. Show Chinese abstract

Abstract: 在本章中，我们回顾了在Hartle形式下静态和均匀旋转中子星的平衡构型的最新结果。 我们从Belvedere等人(2012, 2014)提出并扩展的爱因斯坦-麦克斯韦-托马斯-费米方程开始。 我们演示如何对不同中心密度${\it \rho}_c$和角速度$\Omega$的这些方程进行数值积分，并计算静态$M^{stat}$和旋转$M^{rot}$质量，极半径$R_p$和赤道半径$R_{\rm eq}$，偏心率$\epsilon$，转动惯量$I$，角动量$J$以及旋转构型的四极矩$Q$。 为了满足旋转中子星的稳定性准则，我们考虑了开普勒质量抛射极限和轴对称长期不稳定性。 此外，我们构建了新的质量-半径关系，计算了中子星的最大质量和最小旋转周期（最大频率）。 最终，我们比较和对比了全局和局部中子星模型的结果。