Gravitationally decoupled charged anisotropic solutions in Rastall gravity

This paper develops the stellar interior geometry for charged anisotropic spherical matter distribution by developing an exact solution of the field equations of Rastall gravity using the notion of gravitational decoupling. The main purpose of this investigation is the extension of the well-known isotropic model within the context of charged isotropic Rastall gravity solutions. The second aim of this work is to apply gravitational decoupling via a minimal geometric deformation scheme in Rastall gravity. Finally, the third one is to derive an anisotropic version of the charged isotropic model previously obtained by applying gravitational decoupling technology. We construct the field equations which are divided into two sets by employing the geometric deformation in radial metric function. The first set corresponds to the seed (charged isotropic) source, while the other one relates the deformation function with an extra source. We choose a known isotropic solution for spherical matter configuration including electromagnetic effects and extend it to an anisotropic model by finding the solution of the field equations associated with a new source. We construct two anisotropic models by adopting some physical constraints on the additional source. To evaluate the unknown constants, we use the matching of interior and exterior spacetimes. We investigate the physical feasibility of the constructed charged anisotropic solutions by the graphical analysis of the metric functions, density, pressure, anisotropy parameter, energy conditions, stability criterion, mass function, compactness, and redshift parameters. For the considered choice of parameters, it is concluded that the developed solutions are physically acceptable as all the physical aspects are well-behaved

Physical Behavior of Anisotropic Compact Stars in f(R,T,RμvTμv) Gravity

This paper investigates the behavior of anisotropic compact stars in the background of $R+\alpha R_{\mu\nu}T^{\mu\nu}$ gravity model. For this purpose, we use Krori-Barua metric solutions where constants are calculated using masses and radii of compact stars like Her X-1, SAX J 1808.4-3658 and 4U1820-30. We analyze regular behavior of effective energy density, radial and transverse pressures in the interior of compact stars. We also discuss energy conditions, effect of anisotropic factor and stability criteria of these stars. It is concluded that the considered compact star models satisfy all the energy conditions and remain stable against the anisotropic effect in this gravity.The accepted manuscript in pdf format is listed with the files at the bottom of this page. The presentation of the authors' names and (or) special characters in the title of the manuscript may differ slightly between what is listed on this page and what is listed in the pdf file of the accepted manuscript; that in the pdf file of the accepted manuscript is what was submitted by the author

Anisotropic quark stars in f(R, T) gravity

Abstract The aim of this paper is to analyze the nature of anisotropic spherically symmetric relativistic star models in the framework of f(R, T) gravity. To discuss the features of compact stars, we consider that in the interior of the stellar system, the fluid distribution is influenced by MIT bag model equation of state. We construct the field equations by employing Krori–Barua solutions and obtain the values of unknown constants with the help of observational data of Her X-1, SAX J 1808.4-3658, RXJ 1856-37 and 4U1820-30 star models. For a viable f(R, T) model, we study the behavior of energy density, transverse as well as radial pressure and anisotropic factor in the interior of these stars for a specific value of the bag constant. We check the physical viability of our proposed model and stability of stellar structure through energy conditions, causality condition and adiabatic index. It is concluded that our model satisfies the stability criteria as well as other physical requirements, and the value of bag constant is in well agreement with the experimental value which highlights the viability of our considered model

Quantum corrected charged thin-shell wormholes surrounded by quintessence

Abstract In this manuscript, we inspect the stable geometry of thin-shell wormholes in the framework of static, spherically-symmetric quantum corrected charged black hole solution bounded by quintessence. In this regard, we develop thin-shell wormholes from two equivalent copies of black hole solutions through the cut and paste approach. Then, we employ the linearized radial perturbation to discuss the stability of the developed wormhole geometry by assuming variable equations of state. We obtain the maximum stable configuration for massive black holes for both barotropic and Chaplygin variables equations of state. It is found that the quantum correction affects the stability of thin-shell wormholes and the presence of charge over the geometry of black holes enhances the stable configuration of thin-shell wormholes