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.
In this paper, we extend the notion of complexity for the case of nonstatic self-gravitating spherically symmetric structures within the background of modified Gauss–Bonnet gravity (i.e. [Formula: see text] gravity), where [Formula: see text] denotes the Gauss–Bonnet scalar term. In this regard, we have formulated the equations of gravity as well as the relations for the mass function for anisotropic matter configuration. The Riemann curvature tensor is broken down orthogonally through Bel’s procedure to compose some modified scalar functions and formulate the complexity factor with the help of one of the scalar functions. The CF (i.e. complexity factor) comprehends specific physical variables of the fluid configuration including energy density inhomogeneity and anisotropic pressure along with [Formula: see text] degrees of freedom. Moreover, the impact of the dark source terms of [Formula: see text] gravity on the system is analyzed which revealed that the complexity of the fluid configuration is increased due to the modified terms.
This investigation aims to explore certain variables which are considered responsible for generating pressure anisotropy in dynamical spherically symmetric stellar systems against the background of the stringy-inspired Gauss–Bonnet modification of general relativity. We explore the hydrostatic equilibrium of self-gravitating systems by taking into account the modified form of Tolman–Oppenheimer–Volkoff for the quadratic-f(G) gravitational model. In this respect, we formulate a differential equation in terms of the Weyl curvature scalar, also described as an evolution equation, which is essential for understanding the evolution of the stellar structure. Finally, we conclude that the existence of some fluid variables such as shear, heat flux and the irregular behavior of energy density in the presence of an extra degree f(G)-terms in the fluid flow that are the elements that cause anisotropy in the initially isotropic stellar structure. The comparison of the presented results with those of the classical model shows that they are physically relevant and compatible.
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