Stable and self-consistent compact star models in teleparallel gravity

Abstract

In the framework of Teleparallel Gravity, we derive a charged non-vacuum solution for a physically symmetric tetrad field with two unknown functions of radial coordinate. The field equations result in a closed-form adopting particular metric potentials and a suitable anisotropy function combined with the charge. Under these circumstances, it is possible to obtain a set of configurations compatible with observed pulsars. Specifically, boundary conditions for the interior spacetime are applied to the exterior Reissner-Nordström metric to constrain the radial pressure that has to vanish through the boundary. Starting from these considerations, we are able to fix the model parameters. The pulsar $\text{PSR J 1614–2230}$, with estimated mass $M=1.97\pm 0.04M_{⊚},$ and radius $R=9.69\pm 0.2$ km is used to test numerically the model. The stability is studied, through the causality conditions and adiabatic index, adopting the Tolman-Oppenheimer-Volkov equation. The mass-radius $(M,R)$ relation is derived. Furthermore, the compatibility of the model with other observed pulsars is also studied. We reasonably conclude that the model can represent realistic compact objects.

21 pages, 14 figures, accepted for publication in EPJC

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• Deflection angle and lensing signature of covariant f(T) gravity
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• Realistic neutron star models in $f(T)$ gravity
• The key role of Lagrangian multiplier in mimetic gravitational theory in the frame of isotropic compact star
• Big Bang Nucleosynthesis constraints on $f(T,T_G)$ gravity
• New anisotropic star solutions in mimetic gravity
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• Mass of compact stars in f(T) gravity
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• Isotropic stellar model in mimetic theory
• The general expression for $f(T)$ in a charged cylindrical spacetime with diverse dimensions
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