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This paper uses the gravitational decoupling through the minimal geometric deformation approach and extends a known isotropic solution for a self-gravitating interior to two types of anisotropic spherical solutions in Rastall gravity in the presence of electromagnetic field. By deforming only the radial metric component, the field equations are decoupled into two sets, the first of which corresponds to an isotropic distribution of matter while the second set contains the anisotropic source. We obtain a solution of the first set by employing the charged isotropic Finch-Skea ansatz, whereas a solution for the second set is obtained by adopting two mimic constraints on the pressure and density. The matching conditions at the stellar surface are explored with the exterior geometry given by the deformed Reissner–Nordström spacetime. For the two fixed values of the Rastall and charge parameters, we investigate physical features of both solutions through graphical analysis of the energy conditions, equation of state parameters, surface redshift and compactness function. The stability of both solutions is also studied through the Herrera cracking approach and causality condition. We deduce that while both solutions are physically viable, only the solution corresponding to the pressure-like constraint is stable. • Gravitational decoupling approach is used to find charged exact solutions in Rastall gravity. • We obtain a solution by employing charged isotropic Finch-Skea ansatz. • Investigate physical viability of both solutions through graphical analysis of the physical quantities. • Stability of both solutions is also studied through the Herrera cracking approach and causality condition. • We deduce that both solutions are physically viable but only the first solution is stable. [ABSTRACT FROM AUTHOR]

The present manuscript throws light on the existence of an electrically charged compact stellar model and explores the behavior of complexity factor, proposed by Herrera (2018), against the selected model in the background of f (R , T) gravity (R is the Ricci scalar, while T is the trace of energy–momentum tensor). The set of f (R , T) field equations has been solved by choosing Adler Finch–Skea solution, where the presence of electromagnetic radiations have also been considered in the stellar interior. For the space–time continuity, the boundary conditions have been described by taking Reissner–Nordström solution as exterior space–time. The physical analysis has been made by choosing the radii of PSR J 1614-2230 and SAX J 1808.4-3658, which shows that the model is physically consistent in the realm of f (R , T) gravity, and we obtain more compact stellar configurations for negative values of coupling constant λ. The implications of λ on the total mass and complexity factor of the stellar model have been explored in details. The total mass has been found maximum for λ = − 0. 4 and minimum for λ = 0. 4. The complexity factor is increased for negative values of λ as compared to the other scenarios (i.e., λ ≥ 0). The comparison of anisotropy factor and complexity factor has been made, which indicates the presence of less anisotropy in pressure distribution and more inhomogeneity in energy density of the fluid configuration for negative values of λ. • We explored the behavior of complexity factor for an electrically charged compact stellar model. • Alder Finch–Skea solution is considered in the stellar interior with Reissner–Nordström solution as an exterior. • The physical analysis has been made for radii of PSR J 1614-2230 and SAX J 1808.4-3658. • We obtain more compact stellar configurations for coupling constant λ < 0. • Moreover, the comparison of anisotropy factor and complexity factor has been made. [ABSTRACT FROM AUTHOR]

• Two new exact and analytic solutions of the Einstein–Maxwell field equations describing compact anisotropic charged stars satisfying the Karmarkar condition in the background of Bardeen black hole geometry are studied. • The validity of the solutions is verified by performing several physical tests. • The solutions satisfy all the physical requirements necessary for well-behaved models. • The models represent neutron star in Vela X-1. In this paper, we present two new exact and analytic solutions of the Einstein–Maxwell field equations describing compact anisotropic charged stars satisfying the Karmarkar condition in the background of Bardeen black hole geometry. The solutions are composed of two parts: The inner region of the star is described by class I Karmarkar space-time, while exterior of the star is characterized by both the Bardeen and the Reissner–Nordstrom space-times. Physical analysis of the matter and thermodynamical variables show that the models are well-behaved. For our parametric set of values, we conclude that the Bardeen black hole metric can be used as an alternate to the exterior Reissner–Nordstrom metric. [ABSTRACT FROM AUTHOR]

• We have obtained a new parametric class of well-behaved solutions in embedding class I. • We use pressure anisotropy and Karmarkar condition for developing viable models of compact stars PSR J1614-2230 and SAX J1808.4-3658. • Our solutions satisfy the following stability conditions i.e., Herrera cracking condition, causality condition, Bondi condition, Zeldovich condition and stable static criteria (Harrison-Zeldovich-Novikov criterion) for both the stars in their respective ranges of parametric class. • Our solutions satisfy all energy conditions and equilibrium condition (TOV equation) which are essential for a physically viable stellar models. The aim of this paper is to explore a new parametric class of relativistic solutions to the Einstein field equations describing a spherically symmetric, static distribution of anisotropic fluid spheres to study the behavior of some of the cold stars in the setting of Karmarkar space-time continuum. We develop models of stellar objects for a range of parameter values of n and analyze their behavior through graphical representation. For each of these models, we have found that the metric potentials are well behaved inside the stellar interior and the physical parameters such as density, radial and tangential pressures, red-shift, radial speed, radial pressure density ratio and energy conditions display a continuous decrease from the center to surface of the stars whereas the mass, anisotropy, adiabatic indexes and compactification factor show a monotonous increase which imply that the proposed solution satisfy all the physical aspects of a realistic stellar objects. The stability of the solutions are verified by examining various stability aspects, viz., Zeldovich criteria, causality condition, Bondi condition, equilibrium condition (TOV-equation) and stable static criteria in connection to their cogency. [ABSTRACT FROM AUTHOR]