  This study simulates the characteristics of spherically symmetric,
anisotropic compact stellar bodies with electrical charge within the context of
the $f(Q)$ theory of gravity. Employing the Krori-Barua metric ansatz (K.D.
Krori, J. Barua, J. Phys. A: Math. Gen. 8 (1975) 508) along with a linear form
of $f(Q)$ model, {\it viz.}, $f(Q)=\alpha_{0}+\alpha_{1}Q$, we obtain a
tractable set of exact relativistic solutions of the field equations. A
specific form of charge $(q=q_{0}r^{3})$ is considered here for the present
analysis. Using the data sets of $\rho$ and $p_{r}$ along with the method of
curve fitting, we have obtained the best fit equation of state in the model,
which is incorporated in the numerical solutions of the TOV equations to
determine the maximum mass and radius in this scenario. With increasing charge
intensity $(q_{0})$ from 0.0002 to 0.0006, the maximum mass ranges from
$2.838-2.869~M_{\odot}$, and the corresponding radii range from
$12.0039-12.0822~Km$. Moreover, the predicted radii of some recently observed
pulsars and GW 190814 show that our model also complies with the estimated
radii based on the observational results. Our model is found to satisfy all the
characteristic features, such as behaviour of matter variables, causality
condition, energy constraints and stability criteria, which are pertinent in
the context of a stable stellar configuration to emerge as a viable and
physically acceptable stellar model in the framework of $f(Q)$ gravity.
