Electromagnetic field and complexity of relativistic fluids in f (G) gravity

Abstract

The principal idea behind this manuscript is to inspect the complexity of dissipating as well as non-dissipating self-gravitating sources which are coupled with locally anisotropic charged matter. The gravitational equations in the regime of $f(\mathbb {G})$ ($\mathbb {G}$ is the Gauss-Bonnet invariant) theory have elaborated for the imperfectly charged stellar configuration to scrutinize the charged object in the presence of $f(\mathbb {G})$ corrections. The impact of charge distribution on the connection between density inhomogeneity, Weyl tensor and pressure anisotropy is investigated. By incorporating the constraints of QH (i.e., the quasi-homologous) evolution and CF = 0, (where CF denotes the complexity factor) multiple analytical solutions to the $f(\mathbb {G})$ equations of gravity are developed defining the imperfectly charged compact spherical matter. Some of these stellar models (exact solutions) portray a spherical collapsing configuration of a charged fluid in which there arise a cavity about the fluid center, while other models exhibit a fluid configuration wherein the sphere is totally filled by the fluid. These interior solutions to $f(\mathbb {G})$ gravitational equations may exhibit some appealing astrophysical phenomenons.

Spatially Hyperbolic Gravitating Sources in Λ-Dominated Era

“…Upon using Equation (41) in Equation ( 16), the conformal flat model of our system (after considering e −λ = 2g − 1) can be recast as…”

“…This single tool deals with different aspects of the system, providing a lot of information about the evolution of the system, e.g., shear and expansion evolution, inhomogeneity, complexity, etc., can be dealt with through these structure scalars [34][35][36]. Yousaf and his collaborators [16,[37][38][39][40][41] computed the modified version of these scalars by invoking extra curvature terms and described their influences in understanding the evolutionary mechanisms of adiabatic and non-adiabatic relativistic structures. Herrera [42] introduced a new concept of complexity factor in terms of one of these scalars for the static anisotropic spherical objects.…”

Role of <i>f</i>(<i>R,T</i>) Gravity in Bianchi Type-V Dark Energy Model with Electromagnetic Field based on Lyra Geometry

“…Also is the four-velocity vector in a co-moving coordinate system satisfies the condition . The non-vanishing components of the source of for the given line element are as follows: (12) Now by contracting eq. ( 6), it reduces to…”

“…Because of their capacity to explain the observed faster expansion of the Universe, modified gravity theories have sparked much attention in recent years. The essential ideas among them are And gravity [9][10][11][12][13][14][15][16][17][18][19][20][21][22]. The most prevailing significant theory in the current cosmological model of the Universe, examined with the FRW model and Bianchi type models, is The Lagrangian is a function of Ricci scalar R. The trace of the stress-energy tensor T. Many authors [23][24][25][26][27][28][29][30][31][32][33] have recently studied the dark energy model in gravity based on different contexts so far.…”

Spatially Hyperbolic Gravitating Sources in $Λ$-Dominated Era

“…This single tool deals with different aspects of the system providing a lot of information about evolution of the system, e.g., shear and expansion evolution, inhomogeneity, complexity, etc can be dealt with these structure scalars [34][35][36]. Yousaf and his collaborators [17,[37][38][39][40][41] computed the modified version of these scalars by invoking extra curvature terms and described their influences in understanding evolutionary mechanism of adiabatic and non-adiabatic relativistic structures. Herrera [42] introduced a new concept of complexity factor in terms of one of these scalars for the static anisotropic spherical objects.…”