LAUSR

The present paper deals the effect of charge configurations on relativistic compact stellar structures with isotropic matter distribution in the context of modified $$f(\mathcal {G})$$ gravity, where $$\mathcal {G}$$ being the Gauss–Bonnet invariant term. For this purpose, we start by deriving the hydrostatic equilibrium equations known as Tolman–Oppenheimer–Volkoff equations, together with Einstein–Maxwell field equations by considering the standard choice of two realistic $$f(\mathcal {G})$$ gravity models $$f(\mathcal {G})= \alpha _1 \mathcal {G}^{n_1}$$ and $$f(\mathcal {G})= \alpha _2\mathcal {G}^{n_2}(\beta _2 \mathcal {G}^{m_2}+1)$$. Further, these modified charged Tolman–Oppenheimer–Volkoff equations are numerically integrated by the simplified phenomenological MIT bag model $$p=a(\rho -4\mathbf{b} )$$ equation of state. Moreover, we have discussed physical features like energy density, pressure, mass and charge of relativistic structures by choosing the appropriate values of the model parameters. It is observed that in the context of modified $$f(\mathcal {G})$$ gravity, stellar structure candidates follow physically accepted phenomena, and consequently, the resulting outcome is in well agreement with the experimental data which depicts viability of our considered models.