In the present article, we have constructed a static charged anisotropic compact star model of Einstein field equations for a spherically symmetric space-time geometry. Specifically, we have extended the charged isotropic Heintzmann solution to an anisotropic domain. To address this work, we have employed the gravitational decoupling through the so called minimal geometric deformation approach. The charged anisotropic model is representing the realistic compact objects such as R X J 1856 − 37 and S AX J 1808.4 − 3658(SS2). We have reported our results in details for the compact star R X J 1856 − 37 on the ground of physical properties such as pressure, density, velocity of sound, energy conditions, stability conditions, TolmanOppenheimer-Volkoff equation and redshift etc.

This work is focused in the study of analytic anisotropic solutions to Einstein's field equations, describing spherically symmetric and static configurations by way of the gravitational decoupling through the method of Minimal Geometric Deformation (MGD). For this we apply MGD to Heintzmann's solution obtaining two new analytic and well behaved anisotropic solutions, in which all their parameters such as the effective density, the effective radial and tangential pressure, as well as radial and tangential sound speed, fulfill each of the requirements for the physical acceptability available in the literature.

The present paper provides a new exact and analytic solution of the Einstein-Maxwell field equations describing compact anisotropic charged stars satisfying the MIT bag model equation of state for quark matter. The model is obtained by assuming the Tolman-Kuchowicz spacetime geometry (Tolman, in

The present work is focused on the investigation of the existence of compact structures describing anisotropic matter distributions within the framework of modified gravity theories, specifically f(R,T ) gravity theory. Additionally, we have taken f(R,T ) as a linear function of the Ricci scalar R and the trace of the energy-momentum tensor T as f (R, T )=R + 2χT ,where χ is a dimensionless coupling parameter, and the Lagrangian matter Lm = − 1 3 (2pt + pr), to describe the complete set of field equations for the anisotropic matter distribution. We follow the embedding class one procedure using Eisland condition to obtain a full space-time description inside the stellar configuration. Once the space-time geometry is specified we determine the complete solution of modified Einstein equations by using the MIT bag model equation of state pr = 1 3 (ρ − 4B) that describes the strange quark matter (SQM) distribution inside the stellar system, where B denotes a bag constant. The physical validity of our anisotropic solution is confirmed by executing several physical tests. It is worth mentioning that with the help of the observed mass values for the various strange star candidates we have predicted the exact radii by taking different values for χ and B. These predicted radii show monotonic decreasing nature as the parameter χ is moved from −0.8 to 0.8 progressively. In this case, our anisotropic stellar system becomes more massive and transforms into more dense compact stars. We also performed a detailed graphical analysis of the compact star. As a result, for χ < 0, the current modified f (R, T ) gravity seems promising to explain the observed massive compact astrophysical objects, similar to magnetars, massive pulsars, and Chandrasekhar super white dwarfs, which is not justified in the framework of general relativity. Finally, note that when χ = 0 general relativity results for anisotropic matter distributions are recovered.

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