  Charged stars have the potential of becoming charged black holes or even
naked singularities. It is presented a set of numerical solutions of the
Tolman-Oppenheimer-Volkov equations that represents spherical charged compact
stars in hydrostatic equilibrium. The stellar models obtained are evolved
forward in time integrating the Einstein-Maxwell field equations. It is assumed
an equation of state of a neutron gas at zero temperature. The charge
distribution is taken as been proportional to the rest mass density
distribution. The set of solutions present an unstable branch, even with charge
to mass ratios arbitrarily close to the extremum case. It is performed a direct
check of the stability of the solutions under strong perturbations, and for
different values of the charge to mass ratio. The stars that are in the stable
branch oscillates and do not collapse, while models in the unstable branch
collapse directly to form black holes. Stars with a charge greater or equal
than the extreme value explode. When a charged star is suddenly discharged, it
don't necessarily collapse to form a black hole. A non-linear effect that gives
rise to the formation of an external shell of matter (see Ghezzi and Letelier
2005), is negligible in the present simulations. The results are in agreement
with the third law of black hole thermodynamics and with the cosmic censorship
conjecture.
