  The main focus of this paper is to discuss the solutions of
Einstein-Maxwell's field equations for compact stars study. We have chosen the
MIT bag model equation of state for the pressure-energy density relationship
and conformal Killing vectors are used to investigate the appropriate forms for
metric coefficients. We impose the boundary conditions, by choosing the Bardeen
model to describe as an exterior spacetime. The Bardeen model may provide the
analysis with some interesting results. For example, the extra terms involved
in the asymptotic representations as compared to the usual Reissner-Nordstrom
case may influence the mass of a stellar structure. Both energy density and
pressure profiles behave realistically except a central singularity. It is
shown that the energy conditions are satisfied in our study. The equilibrium
conditions through TOV equation and stability criteria through Adiabatic index
for the charged stellar structure study are investigated. Lastly, we have also
provided a little review of the case with Reissner-Nordstrom spacetime as an
exterior geometry for the matching condition. In both cases, the masses obey
the Andreasson's limit $\sqrt{M} \leq \sqrt{R}/3+\sqrt{R/9+q^2/3R}$ requirement
for a charged star. Conclusively, the results show that Bardeen model geometry
provides more massive stellar objects as compared to usual Reissner-Nordstrom
spacetime. In particular, the current study supports the existence of realistic
massive structures like PSR J $1614-2230$.
