According to the general theory of relativity, a massive body induces curvature in the surrounding spacetime. In this study, the surface curvature (SC) of neutron stars is computed using various curvature quantities derived from the relativistic mean-field, density-dependent RMF, and Skyrme-Hartree-Fock equations of states. Neutron star properties, including mass, radius, compactness, and central density, are calculated utilizing the Tolman-Oppenheimer-Volkoff equations. The analysis reveals a significant cubic correlation between the SC and compactness for the canonical 1.4 $M_{\odot}$ neutron star, with a correlation coefficient of 0.99, indicating an almost linear relationship. A similarly significant inverse cubic correlation is observed between the SC and the radius of the canonical star. However, these correlations diminish for the maximum mass NS. Furthermore, a universal relation between the SC and the dimensionless tidal deformability ($Λ$) for the canonical neutron star is established. Using the tidal deformability constraint of GW170817 ($Λ_{1.4} = 190_{-120}^{+390}$), the surface curvature is limited to SC$_{1.4} (10^{14}) = 2.87^{+0.30}_{-0.78}$ at a confidence level 90\%. Furthermore, the tidal deformability constraint of the secondary component in the GW190814 event ($Λ_{1.4} = 616_{-158}^{+273}$) offers a more stringent limit, with the result of SC$_{1.4} (10^{14}) = 2.03^{+0.27}_{-0.36}$. These findings indicate that the GW190814 event imposes more rigorous constraints on SC compared to GW170817.
General gravitational properties of neutron stars: curvature invariants, binding energy, and trace anomaly
Goethe Universität（法兰克福歌德大学）；Instituto de Astronomía, Universidad Nacional Autónoma de México（墨西哥国立自治大学天文研究所）；School of Mathematics, Trinity College（都柏林三一学院数学学院）；Frankfurt Institute for Advanced Studies（法兰克福高等研究院）
Impact of Anisotropy on Neutron Star Structure and Curvature
Sardar Patel University（萨达尔·帕特el大学）；Istanbul Technical University（伊斯坦布尔理工大学）；P. D. Patel Institute of Applied Science, CHARUSAT（P. D. 帕特el应用科学学院，CHARUSAT）
Curvature-slope correlation of nuclear symmetry energy and its imprints on the crust-core transition, radius and tidal deformability of canonical neutron stars
Brightness temperature constraints on coherent processes in magnetospheres of neutron stars
我们讨论的约束条件，所观察到的亮度温度施加在相干过程中的恒星和快速射电暴（FRB），特别是相干曲率发射的聚束的假设。我们估计一束电荷$Ze$通过同步辐射和/或曲率发射可以产生的峰值亮度温度为$k_B T \sim (Z e)^2/λ$，其中$λ$是典型的发射波长。我们表明，一堆的静电能量所需的产生观察到的亮度温度是过高的，总{ \it散装}能量的顺序。我们比较了自由电子激光机制（Lyutikov 2021）的相应要求，发现在这种情况下，约束更容易满足。
