Constraining the Surface Curvature of an Anisotropic Neutron Star

Abstract

The anisotropy of pressure arises due to the various complex phenomena that happen inside the neutron star (NS). In this study, we calculate the degree of anisotropy inside the NS using the scalar pressure anisotropy model. Macroscopic properties such as mass, radius, compactness, redshift, tidal deformability, the moment of inertia, and surface curvature (SC) are computed for the anisotropic NS with the equation of states spanning from relativistic to nonrelativistic cases. The variation of SC as the functions of the above-mentioned quantities are computed by changing the degree of anisotropy. Pressure anisotropy has significant effects on the magnitude of SC. The universal relations between the canonical SC$-\Lambda$ and SC$-\bar{I}$ are studied. From the GW170817 tidal deformability data constraints on SC are found to be SC${}_{1.4}(10^{14})=3.44_{-1.0}^{+0.4},2.85_{-1.20}^{+0.62},\mathrm{and}2.52_{-1.02}^{+0.61}$ for ${\lambda }_{\mathrm{BL}}=0.0,1.0$, and $2.0$ respectively.

8 pages, 6 figures, 1 table, Published in Phys. Rev. D

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Cited by in corpus (3)

• Implications of Fermionic Dark Matter Interactions on Anisotropic Neutron Stars
• Spacetime Curvature as a Probe of Exotic Core Phases in Neutron Stars within Modified Gravity
• Impact of Anisotropy on Neutron Star Structure and Curvature