A New Charged Anisotropic Compact Star Model in General Relativity

Tamta, Ritu; Fuloria, Pratibha

doi:10.4236/jmp.2017.811104

Cited by 12 publications

(8 citation statements)

References 39 publications

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“…This generating function encompasses the important cases of charged perfect fluid when Δ = 0 [40] and neutral perfect fluid when Δ = 0, l = 0. Solutions with given Δ, a 1 and l are discussed [41][42][43], where the mass is used instead of y, [44][45][46][47][48][49][50]. There are also solutions with Δ = 0 [51,52].…”

Section: The Tangential Pressure and The Anisotropic Factormentioning

confidence: 99%

Generating solutions for charged stellar models in general relativity

Иванов

2021

Eur. Phys. J. C

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It is shown that the expressions for the tangential pressure, the anisotropy factor and the radial pressure in the Einstein–Maxwell equations may serve as generating functions for charged stellar models. The latter can incorporate an equation of state when the expression for the energy density is also used. Other generating functions are based on the condition for the existence of conformal motion (conformal flatness in particular) and the Karmarkar condition for embedding class one metrics, which do not depend on charge. In all these cases the equations are linear first order differential equations for one of the metric components and Riccati equations for the other. The latter may be always transformed into second order homogenous linear differential equations. These conclusions are illustrated by numerous particular examples from the study of charged stellar models.

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Section: The Tangential Pressure and The Anisotropic Factormentioning

confidence: 99%

Generating solutions for charged stellar models in general relativity

Иванов

2021

Eur. Phys. J. C

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“…Moreover the existence of a solid core or a 3A type superfluid may cause the star to be anisotropic [32]. There is another source that makes the star anisotropic: it is a strong magnetic field [33,34]. The slow rotation can be considered another source of anisotropy [35].…”

Section: Introductionmentioning

confidence: 99%

Stable and self-consistent compact star models in teleparallel gravity

Nashed

Capozziello

2020

Eur. Phys. J. C

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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 $$\textit{PSR J 1614-2230}$$ PSR J 1614 - 2230 , with estimated mass $$M= 1.97 \pm 0.04\, M_{\circledcirc },$$ M = 1.97 ± 0.04 M ⊚ , and radius $$R= 9.69 \pm 0.2$$ R = 9.69 ± 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.

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“…Panahi et al [40] presented a comparison of charge anisotropy with isotropy. Tamta and Fuloria [41] obtained solutions for Einstein Maxwell's field equations for charged anisotropic fluid. Ratanpal and Bhar [42] constructed models on anisotropic compact stars in the presence of charge.…”

Section: Introductionmentioning

confidence: 99%

Charged anisotropic compact star core-envelope model with polytropic core and linear envelope

2021

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This manuscript is related to the construction of relativistic core-envelope model for spherically symmetric charged anisotropic compact objects. The polytropic equation of state is considered for core, while it is linear in the case of envelope. We present that core, envelope and the Reissner Nordstr$$\ddot{o}$$ o ¨ m exterior regions of stars match smoothly. It has been verified that all physical parameters are well behaved in the core and envelope region for the compact stars SAX J1808.4-3658 and 4U1608-52. Various physical parameters inside star are discussed herein, non-singularity and continuity at the junction has been catered as well. Impact of charged compact object together with core-envelope model on the mass, radius and compactification factor is described by graphical representation in both core and envelop regions. The stability of the model is worked out with the help of Tolman–Oppenheimer–Volkoff equations and radial sound speed.

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A New Charged Anisotropic Compact Star Model in General Relativity

Cited by 12 publications

References 39 publications

Generating solutions for charged stellar models in general relativity

Generating solutions for charged stellar models in general relativity

Stable and self-consistent compact star models in teleparallel gravity

Charged anisotropic compact star core-envelope model with polytropic core and linear envelope

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