Modeling theoretical charged compact stellar structures under zero complexity factor constraint in Einstein’s gravity scenario

Abstract This study applies the concept of a complexity factor, originally formulated for static spherically symmetric spacetimes, to a system containing a charged fluid. The analysis commences by formulating the Einstein field equations for the anisotropic fluid and subsequently evaluating two distinct mass functions. The scalar $${Y}_{TF}$$ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msub> <mml:mi>Y</mml:mi> <mml:mrow> <mml:mi>TF</mml:mi> </mml:mrow> </mml:msub> </mml:math> is selected as the complexity factor under Herrera’s formalism due to the incorporation of the key factors for dynamical complexity, which are pressure anisotropy and energy density inhomogeneity. Furthermore, the field equations are solved by imposing several constraints, one of them being the requirement of vanishing complexity. Using two different expressions for the radial metric potential, we obtain two independent solutions. We then determine the unknowns in these models by applying the junction conditions with the Reissner–Nordström metric as the exterior spacetime. Multiple stellar candidates’ observational data is assumed to check the acceptability of the obtained solutions graphically. It is concluded that both the suggested models depict stable and physically viable fluid configurations. These findings ultimately show that how well the vanishing complexity requirement behave in achieving feasible charged anisotropic fluid solutions.