Role of <i>f</i>(<i>G</i>) gravity in the study of non-static complex systems

Yousaf, Z.; Bhatti, M. Z.; Nasir, M. M. M.

doi:10.1139/cjp-2021-0328

Cited by 12 publications

(4 citation statements)

References 59 publications

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“…Similarly, we observed the simplest pattern of evolution in the non-dissipative case such that the complexity factor Y TF becomes zero by neglecting the effect of the electromagnetic part and modified components due to  ( ) f gravity. Here, it is necessary to mention that in the non-dissipative case, complexity increases in the presence of charge as compared to previous work by Yousaf and his collaborators [103]. We also observe that the shear-free condition corresponds to the result q = 0 (zero dissipation) if at the same time, both these cases of homogenous expansion, as well as the homologous condition, exist.…”

Section: Discussionsupporting

confidence: 66%

Complexity of charged anisotropic spherically symmetric fluids in f() gravity

Yousaf

Bhatti

Nasir

2023

Commun. Theor. Phys.

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The previous ideology of complexity factor for the dynamical spheres \cite{herrera2018definition,yousaf2022role} is extended for the influence of charge. A non-dissipative and dissipative dynamical spherically symmetric self-gravitating structure is examined in the presence of Maxwell $f(\mathcal{G})$ gravity to examine the complexity factor. The pattern of evolution is studied with the minimal complexity constraint. The complexity factor remains the same for the structure of fluid distribution, while we examine homologous constraints for the most basic evolution pattern. We calculate the structure scalars which play an important role in order to understand the fundamental properties of the system. The fluid is geodesic as well as shearing for the dissipative case and there is a large number of solutions. In the non-dissipative fluid distribution, a shear-free, homogeneous, and isotropic, geodesic fluid correlates with the evolving homologous and vanishing complexity condition. The implication of the condition of vanishing complexity factor and stability are discussed at the end.

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Section: Discussionsupporting

confidence: 66%

Complexity of charged anisotropic spherically symmetric fluids in f() gravity

Yousaf

Bhatti

Nasir

2023

Commun. Theor. Phys.

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“…In (11) ,they also tried to explore the f (G, T 2 ) theory upon the complexity of time-dependent dissipative as well as non-dissipative spherically symmetric celestial structures. The concept of complexity for dynamical spherically symmetric dissipative self-gravitating configuration is also generalized in the scenario of f (G) gravity by Yousaf et al (12) . Whereas in the dissipative scenario, the fluid is still geodesic but shearing and has a large range of solutions, an isotropic, geodesic, homogeneous, and shear-free fluid distribution that satisfies the vanishing complexity constraint and proceeds homologously corresponds to such a fluid.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of Bianchi Type-III Universe with Time-Varying Deceleration Parameter in f (G) Gravity

Basumatary,

Dewri

2023

IJST

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Objectives: To explore Bianchi type-III cosmological models in f (G) gravity theory with time-varying deceleration parameters. Methods: In this paper, to get the exact solution of the field equation in the presence of perfect fluid, we consider: (i) the relation that shear scalar (σ )is proportional to the expansion scalar(θ ), resulting in C = B n . (ii) time-varying deceleration parameter, q = −1 + 1 √ t suggested by Dewri (1) , indicating an accelerated expansion of the universe. (iii) the power-law f (G) model, which is compatible with the recent observational data. Also, along with the graphical representation, the geometrical and physical aspects are examined. Findings: In this study, the model transit from the early decelerating phase(q > 0) to the present accelerating phase (q < 0), and in support of that, violation of the strong energy condition with negative pressure is observed, ultimately indicating the presence of the dark energy. It is worthwhile to mention that the contribution of dark energy initially lies in the phantom domain(ω < −1). After a period of time, it extends to the quintessence domain(ω > −1) and later approaches to Λ cold dark matter (CDM) model (ω = −1) at a late time. Novelty: The universe's evolution has been explored in the framework of f (G) gravity, identifying the cosmological parameters of the model obtained in this work. The negative pressure and the falling of strong energy conditions suggest its consistency with the recent cosmological observation of the dark energy universe, and the findings of this study may contribute to a deeper comprehension of the universe's accelerated expansion.

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“…They explored some relativistic configurations satisfying the zero CF condition and also exhibited some analytic solutions under the influence of tidal forces. Recently, Yousaf and his collaborators investigated the role of modified corrections in the analysis of static charged anisotropic, as well as for dynamical dissipative complex configurations [69,70]. The authors determined the vanishing of the CFs to provoke the stability of the relativistic fluids and found corresponding analytical solutions.…”

Section: Introductionmentioning

confidence: 99%

A measure of complexity for axial self-gravitating static fluids

Farwa¹,

Yousaf²,

Bhatti³

2022

Phys. Scr.

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One of the feasible potential candidates for illustrating the accelerating expansion of the cosmos can be taken through the notion of modiﬁed gravity. Within the context of metric f(R) gravity, the contribution of this work features a better understanding of complexity factors for anisotropic static ﬂuid composition in axially symmetric spacetime. This is a generalization of the work done by Herrera et al. [Phys. Rev. D 99, 044049 (2019)]. We formulate generalized dynamical and ﬁeld equations for anisotropic source in our analysis. We will compute three distinct complexity factors (YTF 1, YTF 2, YTF 3) after incorporating structure scalars via orthogonal breakdown of the curvature tensor. The diﬀerential equations for the conformal tensor are assessed in terms of these complexity factors for the physical illustration. It is inferred that all these factors vanish for the matter spheroid provided with energy homogeneity and isotropic pressure. Nonetheless, the vanishing of these factors might be observed in different scenarios. This happened because energy inhomogeneity and pressure anisotropy cancel out each other in the description of complexity factors. Certain exact solutions of this nature have been reported and studied. All of the outcomes would reduce to general relativity within usual limits.

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Role of f(G) gravity in the study of non-static complex systems

Cited by 12 publications

References 59 publications

Complexity of charged anisotropic spherically symmetric fluids in f() gravity

Complexity of charged anisotropic spherically symmetric fluids in f() gravity

Dynamics of Bianchi Type-III Universe with Time-Varying Deceleration Parameter in f (G) Gravity

A measure of complexity for axial self-gravitating static fluids

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