Abstract
In the present article, we have obtained a new solution for the charged compact star model through the gravitational decoupling (GD) by using a complete geometric deformation (CGD) approach (Ovalle, Phys Lett B 788:213, 2019). In this approach, the initial decoupled system is separated into two subsystems namely Einstein–Maxwell’s system and quasi-Einstein system. We solve Einstein–Maxwell’s system by taking well known Tolman–Kuchowicz spacetime geometry in the context of the perfect fluid matter distribution. On the other hand, the second system introduce the anisotropy inside the matter distribution which is solved by taking an EOS in theta components. The boundary conditions have been derived to determine the constants parameter. To support the mathematical and physical analysis of the present GD solution, we have plotted all the graphs for the compact objects PSR J1614-2230, 4U1608-52 and Cen X-3 corresponding to the constant alpha =0.001, 0.0012 and 0.0014, respectively. Moreover, we also studied the equilibrium and stability of the solution. The present study shows that the GD technique is a very significant tool to generalize the solution in a more complex form or one matter distribution to another matter distribution.
Highlights
Density in order to solve the system
For solving of this system, we propose a linear equation of state (EOS) in θ along with the one deformation function f (r )
In order to verify the viable feasibility of the stress-energy tensor, we need to study whether the compact stellar structure is consistent with the inequalities (94)–(96) or not? For this purpose, we plot the Fig. 7 for the above energy conditions and we observe that our stellar compact objects are consistent with all the energy conditions and ratifies that the physical acceptability of gravitational decoupling solution for compact objects
Summary
More recently MGD approach was used to discover the higher dimensional compact objects [130] and extent in the context of Lovelock [131] and modified f (R, T ) [91] gravity theories as well as in cosmological problems [132] Through this GD approach, we can extend any well behaved isotropic solution (as discussed above) of the Einstein field equation into anisotropic or charged, as well as both anisotropic-charged domains by adding extra source θi j in the original energy-momentum tensor Ti j or by defining the action for total energy tensor.
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