Influence of three parameters on decoupled charged compact stars generated by dark matter and their predicted radii in f(R,T) gravity theory

Abstract

In the context of $f(R,T)$ gravity theory we have obtained an exact non-singular solution to the field equations for the anisotropic charged stellar system. The method of minimal geometrical deformation (MGD) with regard to the gravitational decoupling approach is employed to reduce the field equations into two sets of equations governed by the seed system and the new source system. An isotropic charged fluid configuration with modified Durgapal–Fuloria potential as a metric ansatz is considered for the seed system whereas density profile of Pseudo-Isothermal dark matter (PI-DM) is taken into account to mimic a component of the new source system. The anisotropy feature that essentially arises in the effective system is one of the important consequences of the gravitational decoupling approach. With this approach we get the solution to gravitationally decoupled field equations which describes the physical characteristics of an effective anisotropic and charged system. The effective system is found to be stable with regard to Herrera’s cracking concept, adiabatic condition, and Harrison–Zeldovich–Novikov criteria. The influence of the MGD parameter, coupling constant, and dark matter density parameter on the physical features and stability of the effective system have been analyzed and shown graphically. The mass–radius relation of the effective system is inspected in connection to the observational constraint of the massive stars such as pulsars and massive secondary companions involved in gravitational wave events. The maximum mass of the star is apparently constrained with the increasing values of the $f(R,T)$-gravity coupling constant, MGD parameter, DM density parameter, and charge. Enabling all the set of parameters the range of predicted radii of the observed massive stars was found to be 9.77 km–12.00 km.