An anisotropic version of Tolman VII solution in f(R, T) gravity via gravitational decoupling MGD approach

Azmat, Hina; Zubair, M.

doi:10.1140/epjp/s13360-021-01081-z

Cited by 72 publications

(24 citation statements)

References 72 publications

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“…These conditions are called the continuity of first and second fundamental across the boundary of the star, respectively. In order to invoke the junction conditions we must smoothly match the interior Class I spacetime (43) with exterior vacuum spacetime described by the exterior Schwarzschild solution. The matching yields the vanishing of radial pressure at the surface r = R and fixes the arbitrary constants in the solution.…”

Section: Solution Generated By Isotropization Techniquementioning

confidence: 99%

“…where m G R (R) = M s represents the total mass of the object with radius R for the Class I spacetime (43) described by source T i j . The conditions ( 48)-(50) determine the constants A, B, and D as…”

Section: Solution Generated By Isotropization Techniquementioning

confidence: 99%

“…We would like to comment here that the gravitational potentials (75) and (76) and matter variables described by Eqs. (77)-(80) represent a new version of Class I anisotropic solutions (43) corresponding to the Einstein field equations ( 7)-( 9), whose complexity factor ŶT F is the same as the complexity factor Y T F given by Eq. ( 73).…”

Section: Complexity Factor Generated By Minimally Deformed Class I So...mentioning

confidence: 99%

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Isotropization of embedding Class I spacetime and anisotropic system generated by complexity factor in the framework of gravitational decoupling

et al. 2022

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In this work, we present a hierarchical solution-generating technique employing the Minimum Gravitational Decoupling (MGD) Method and the generalized concept of Complexity as applied to Class I spacetime for bounded compact objects in classical general relativity. Starting off with an anisotropic seed solution described by Class I spacetime, we apply the MGD technique with the constraint that the effective anisotropy vanishes which leads to an isotropic model. In addition, we produce a second family of solutions in which the Complexity factor [Herrera (Phys Rev D 97:044010, 2018)] for the seed solution and its MGD counterpart are the same. We discuss the physical plausibility of both classes of solutions as candidates for physically realizable compact objects.

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Section: Solution Generated By Isotropization Techniquementioning

confidence: 99%

Section: Solution Generated By Isotropization Techniquementioning

confidence: 99%

Section: Complexity Factor Generated By Minimally Deformed Class I So...mentioning

confidence: 99%

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Isotropization of embedding Class I spacetime and anisotropic system generated by complexity factor in the framework of gravitational decoupling

et al. 2022

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“…Static spherically symmetric wormholes in f (R, T ) gravity were proposed by Zubair et al [19]. Azmat and Zubair [20] have adopted gravitational decoupling by a minimal geometric deformation (MGD) approach and have developed an anisotropic version of the well-known Tolman VII isotropic solution in the framework of f (R, T ) gravity.…”

Section: Introductionmentioning

confidence: 99%

Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Rej¹,

Bhar²,

Govender

2021

Eur. Phys. J. C

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In this current study, our main focus is on modeling the specific charged compact star SAX J 1808.4-3658 (M = 0.88 $$M_{\odot }$$ M ⊙ , R = 8.9 km) within the framework of $$f(R,\,T)$$ f ( R , T ) modified gravity theory using the metric potentials proposed by Tolman–Kuchowicz (Tolman in Phys Rev 55:364, 1939; Kuchowicz in Acta Phys Pol 33:541, 1968) and the interior spacetime is matched to the exterior Reissner–Nordström line element at the surface of the star. Tolman–Kuchowicz metric potentials provide a singularity-free solution which satisfies the stability criteria. Here we have used the simplified phenomenological MIT bag model equation of state (EoS) to solve the Einstein–Maxwell field equations where the density profile ($$\rho $$ ρ ) is related to the radial pressure ($$p_{\mathrm{r}}$$ p r ) as $$p_{\mathrm{r}}(r) = (\rho - 4B_{\mathrm{g}})/3$$ p r ( r ) = ( ρ - 4 B g ) / 3 . Furthermore, to derive the values of the unknown constants $$a,\, b,\, B,\, C$$ a , b , B , C and the bag constant $$B_{\mathrm{g}}$$ B g , we match our interior spacetime to the exterior Reissner–Nordström line element at the surface of stellar system. In addition, to check the physical validity and stability of our suggested model we evaluate some important properties, such as effective energy density, effective pressures, radial and transverse sound velocities, relativistic adiabatic index, all energy conditions, compactness factor and surface redshift. It is depicted from our current study that all our derived results lie within the physically accepted regime which shows the viability of our present model in the context of $$f(R,\,T)$$ f ( R , T ) modified gravity.

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“…We have investigated the viability and stability of strange quark stars in the presence of a massive scalar field [49,50]. The scheme of decoupling via MGD has been applied in the context of SBD as well as other modified theories to obtain well-behaved anisotropic spacetimes [51][52][53][54][55][56][57][58][59][60].…”

Section: Introductionmentioning

confidence: 99%

Decoupled Embedding Class-One Strange Stars in Self-Interacting Brans–Dicke Gravity

Sharif

Majid

2021

Universe

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This work aims to extend two isotropic solutions to the anisotropic domain by decoupling the field equations in self-interacting Brans–Dicke theory. The extended solutions are obtained by incorporating an additional source in the isotropic fluid distribution. We deform the radial metric potential to disintegrate the system of field equations into two sets such that each set corresponds to only one source (either isotropic or additional). The system related to the anisotropic source is solved by employing the MIT bag model as an equation of state. Further, we develop two isotropic solutions by plugging well-behaved radial metric potentials in Karmarkar’s embedding condition. The junction conditions at the surface of the star are imposed to specify the unknown constants appearing in the solution. We examine different physical characteristics of the constructed quark star models by using the mass and radius of PSR J1903+327. It is concluded that, in the presence of a massive scalar field, both stellar structures are well-behaved, viable and stable for smaller values of the decoupling parameter.

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An anisotropic version of Tolman VII solution in f(R, T) gravity via gravitational decoupling MGD approach

Cited by 72 publications

References 72 publications

Isotropization of embedding Class I spacetime and anisotropic system generated by complexity factor in the framework of gravitational decoupling

Isotropization of embedding Class I spacetime and anisotropic system generated by complexity factor in the framework of gravitational decoupling

Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Decoupled Embedding Class-One Strange Stars in Self-Interacting Brans–Dicke Gravity

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