On the role of density inhomogeneity and local anisotropy in the fate of spherical collapse

Herrera, L.; Prisco, A. Di; Hernández‐Pastora, J. L.; Santos, N. O.

doi:10.1016/s0375-9601(97)00874-8

Cited by 172 publications

(107 citation statements)

References 16 publications

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“…The noticeable behavior of the "effective inertial mass" as named by m T played with an extension on the universal theory of energy for the local surface , the detail is given in [8,18,19] …”

Section: The Formulation Of Tolman Mass and The Mass Functionmentioning

confidence: 99%

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

Abbas

Nazar

2018

Eur. Phys. J. C

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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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Section: The Formulation Of Tolman Mass and The Mass Functionmentioning

confidence: 99%

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

Abbas

Nazar

2018

Eur. Phys. J. C

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“…Also, from the field equations and the definition of the Weyl tensor it can be easily shown that (see [21] for details)…”

Section: The Weyl Tensormentioning

confidence: 99%

Relativistic gravitational collapse in noncomoving coordinates: The post-quasistatic approximation

et al. 2002

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A general, iterative, method for the description of evolving self-gravitating relativistic spheres is presented. Modeling is achieved by the introduction of an ansatz, whose rationale becomes intelligible and finds full justification within the context of a suitable definition of the post-quasistatic approximation. As examples of application of the method we discuss three models, in the adiabatic case.

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“…The investigation of the final stellar phase has been a focus of great interest for many relativistic astrophysicists and gravitational theorists. In this respect, various authors [54][55][56][57] explored the problem of GC by taking some realistic configurations of matter and geometry. In the context of f (R) gravity, various results have been found in the literature as regards collapsing stellar interiors and black holes [58][59][60][61].…”

Section: Introductionmentioning

confidence: 99%

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

et al. 2017

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This paper aims to explore some realistic configurations of anisotropic spherical structures in the background of metric f (R) gravity, where R is the Ricci scalar. The solutions obtained by Krori and Barua are used to examine the nature of particular compact stars with three different modified gravity models. The behavior of material variables is analyzed through plots and the physical viability of compact stars is investigated through energy conditions. We also discuss the behavior of different forces, equation of state parameter, measure of anisotropy and Tolman-Oppenheimer-Volkoff equation in the modeling of stellar structures. The comparison from our graphical representations may provide evidence for the realistic and viable f (R) gravity models at both theoretical and the astrophysical scale.

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On the role of density inhomogeneity and local anisotropy in the fate of spherical collapse

Abstract: We obtain an expression for the active gravitational mass of a collapsing fluid distribution, which brings out the role of density inhomogeneity and local anisotropy in the fate of spherical collapse.

Cited by 172 publications

References 16 publications

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

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

Relativistic gravitational collapse in noncomoving coordinates: The post-quasistatic approximation

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

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