Influence of $$f\,(R)$$ f ( R ) models on the existence of anisotropic self-gravitating systems

Yousaf, Z.; Sharif, M.; Ilyas, M.; Bhatti, M. Z.

doi:10.1140/epjc/s10052-017-5280-0

“…Recently, some of the physical properties of different strange compact stars were studied in the framework of different modified gravity theories and it was concluded that all these strange stars under consideration are stable, matter content is realistic and obeys all the energy conditions [37][38][39]. In favor of modeling static objects, supposition of spherical symmetry geometry is very useful and natural while there are more options in the choice of matter content.…”

Section: Introductionmentioning

confidence: 99%

Charged compact stars in $$f({\mathcal {G}})$$ f ( G ) gravity

Ilyas

¹

2018

Self Cite

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This work is devoted to investigate some of the interior configuration of static anisotropic spherical stellar charged structures in the regime of f (G) gravity, where G is the Gauss Bonnet invariant. The structure of particular charged stars is analyzed with the help of solution obtained by Krori and Barua under different viable models in f (G) gravity theory. The behavior of some physical aspects is investigated with the help of plots and the viability of our modeling is analyzed through different energy conditions. We have also studied some behavior of these realistic charged compact stars and discuss some aspects like density variation, evolution of stresses, different forces, stability of these stars, measure of anisotropy, equation of state parameters and the distribution of charges.

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“…ese types of feasible models are f(R) � R + cR 2 [102] and f(R) � R + cR(R + αR 2 ) [42], in which one of them is recognized as quadratic curvature formulation of the generic function of Ricci scalar R and the other is the modified form of the prior model in terms of cubic corrections. Several reasonable outcomes of these models have been devoted in the literature [53,[103][104][105][106] for the physical evaluation of the collapsing star and the stable equilibrium condition of the star at the theoretical as well as the astrophysical backgrounds.…”

Section: Evolution Of Matter Density Pressure and Electric Fieldmentioning

confidence: 99%

“…e same author and his collaborators [52] determined the physical aspects of compact stellar bodies for KB line-element in modified f(R, ϕ) context. Yousaf et al [53] investigated the impacts of different viable f(R) paradigms on the existence of anisotropic stellar compact objects and found that these paradigms are well behaved at the astrophysical and the theoretical scales. e physical features of anisotropic spherically symmetric strange stars with quintessence field were discussed by Abbas et al [54] for the specific pattern of the f(R) � R + λR 2 model.…”

Section: Introductionmentioning

confidence: 99%

Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity

Nazar

¹

,

Abbas

²

2021

Advances in Astronomy

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In the present article, we have investigated a new family of nonsingular solutions of static relativistic compact sphere which incorporates the characteristics of anisotropic fluid and electromagnetic field in the context of minimally coupled f R theory of gravity. The strange matter MIT bag model equation of state (EoS) has been considered along with the usual forms of the Karori–Barua KB metric potentials. For this purpose, we derived the Einstein–Maxwell field equations in the assistance of strange matter EoS and KB type ansatz by employing the two viable and cosmologically well-consistent models of f R = R + γ R 2 and f R = R + γ R R + α R 2 . Thereafter, we have checked the physical acceptability of the proposed results such as pressure, energy density, energy conditions, TOV equation, stability conditions, mass function, compactness, and surface redshift by using graphical representation. Moreover, we have investigated that the energy density and radial pressure are nonsingular at the core or free from central singularity and always regular at every interior point of the compact sphere. The numerical values of such parameters along with the surface density, charge to radius ratio, and bag constant are computed for three well-known compact stars such as CS1 SAXJ 1808 . 4 − 3658 ( x ˜ = 7.07 km , CS2 VelaX − 1 x ˜ = 9.56 km , and CS3 4U1820 − 30 x ˜ = 10 km and are presented in Tables 1–6. Conclusively, we have noticed that our presented charged compact stellar object in the background of two well-known f R models obeys all the necessary conditions for the stable equilibrium position and which is also perfectly fit to compose the strange quark star object.

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“…A lot of discussion about the complexity has been assessed in various fields of science. Now in this attention several researchers have given systematic work that is shown in [1][2][3][4][5][6][7][8][9][10].…”

Section: Introductionmentioning

confidence: 99%

Complexity factor for static anisotropic self-gravitating source in f(R) gravity

Abbas

¹

,

Nazar

²

2018

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In a recent paper, Herrera (Phys Rev D 97: 044010, 2018) have proposed a new definition of complexity for static self-gravitating fluid in general relativity. In the present article, we implement this definition of complexity for static self-gravitating fluid to case of f (R) gravity. Here, we found that in the frame of f (R) gravity the definition of complexity proposed by Herrera, entirely based on the quantity known as complexity factor which appears in the orthogonal splitting of the curvature tensor. It has been observed that fluid spheres possessing homogenous energy density profile and isotropic pressure are capable to diminish their the complexity factor. We are interested to see the effects of f (R) term on complexity factor of the self-gravitating object. The gravitating source with inhomogeneous energy density and anisotropic pressure have maximum value of complexity. Further, such fluids may have zero complexity factor if the effects of inhomogeneity in energy density and anisotropic pressure cancel the effects of each other in the presence of f (R) dark source term. Also, we have found some interior exact solutions of modified f (R) field equations satisfying complexity criterium and some applications of this newly concept to the study of structure of compact objects are discussed in detail. It is interesting to note that previous results about the complexity for static self-gravitating fluid in general relativity can be recovered from our analysis if f (R) = R, which general relativistic limit of f (R) gravity.

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Influence of $$f\,(R)$$ f ( R ) models on the existence of anisotropic self-gravitating systems

Cited by 60 publications

References 109 publications

Charged compact stars in $$f({\mathcal {G}})$$ f ( G ) gravity

Charged compact stars in $$f({\mathcal {G}})$$ f ( G ) gravity

Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity

Complexity factor for static anisotropic self-gravitating source in f(R) gravity

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Influence of $$f\,(R)$$ f ( R ) models on the existence of anisotropic self-gravitating systems

Cited by 60 publications

References 109 publications

Charged compact stars in $$f({\mathcal {G}})$$ f ( G ) gravity

Charged compact stars in $$f({\mathcal {G}})$$ f ( G ) gravity

Model of Charged Anisotropic Strange Stars in Minimally Coupled f R Gravity

Complexity factor for static anisotropic self-gravitating source in f(R) gravity

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Product

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Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity