Charged anisotropic model with embedding and a linear equation of state

Mathias, Alberto K; Sunzu, Jefta M.; Maharaj, S. D.; Mkenyeleye, Jason M.

doi:10.1007/s12043-022-02503-y

Cited by 6 publications

(2 citation statements)

References 54 publications

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“…To infer the stability of the accepted CTOV models for the three stars, the following conditions should be fulfilled 17 , 18 : The density and the pressure should be positive, finite, and have regular behavior free from singularity within the stellar interior, i.e., . According to Figs.…”

Section: Resultsmentioning

confidence: 99%

“…Abellán et al 9 provided a generic framework for modeling general relativistic polytropes where both pressures satisfy a polytropic state equation and anisotropic pressure is present. Mathias et al 17 generated a core envelope star model in Karmarkar condition where the core is described as a quark matter and the envelope a neutron fluid 18 , generate a charged star model satisfying three layers with distinct equations of state 19 , constructed exact model for a dense stellar object utilizing the Einstein-Maxwell system of equations comprises three interior regions with distinct equations of state, and 20 established a two-layered model with a quadratic EoS in the envelope layer and a polytropic core. An alternative approach may be called a non-uniform polytrope to model the internal structure of stars and planets (e.g., 21 , 22 ).…”

Section: Introductionmentioning

confidence: 99%

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Compact stars with non-uniform relativistic polytrope

Nouh,

Foda,

Aboueisha

2024

Sci Rep

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This paper presents new relativistic composite polytropic models for compact stars by simultaneously solving Einstein field equations with the polytropic state equation to simulate the spherically symmetric, static matter distribution. Using a non-uniform polytropic index, we get the Tolman–Oppenheimer–Volkoff equation for the relativistic composite polytrope (CTOV). To analyze the star's structure, we numerically solve the CTOV equation and compute the Emden and mass functions for various relativistic parameters and polytropic indices appropriate for neutron stars. The calculation results show that, as the relativistic parameter approaches zero, we recover the well-known Lane-Emden equation from the Newtonian theory of polytropic stars; thus, testing the computational code by comparing composite Newtonian models to those in the literature yields good agreement. We compute composite relativistic models for the neutron star candidates Cen X-3, SAXJ1808.4-3658, and PSR J1614-22304. We compare the findings with various existing models in the literature. Based on the accepted models for PSR J1614-22304 and Cen X-3, the star's core radius is predicted to be between 50 and 60% percent of its total radius, while we found that the radius of the core of star SAXJ1808.4-3658 is around 30% of the total radius. Our findings show that the neutron star structure may be approximated by a composite relativistic polytrope, resulting in masses and radii that are quite consistent with observation.

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