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Charged stars have the potential of becoming charged black holes or evennaked singularities. It is presented a set of numerical solutions of theTolman-Oppenheimer-Volkov equations that represents spherical charged compactstars in hydrostatic equilibrium. The stellar models obtained are evolvedforward in time integrating the Einstein-Maxwell field equations. It is assumedan equation of state of a neutron gas at zero temperature. The chargedistribution is taken as been proportional to the rest mass densitydistribution. The set of solutions present an unstable branch, even with chargeto mass ratios arbitrarily close to the extremum case. It is performed a directcheck of the stability of the solutions under strong perturbations, and fordifferent values of the charge to mass ratio. The stars that are in the stablebranch oscillates and do not collapse, while models in the unstable branchcollapse directly to form black holes. Stars with a charge greater or equalthan the extreme value explode. When a charged star is suddenly discharged, itdon't necessarily collapse to form a black hole. A non-linear effect that givesrise to the formation of an external shell of matter (see Ghezzi and Letelier2005), is negligible in the present simulations. The results are in agreementwith the third law of black hole thermodynamics and with the cosmic censorshipconjecture.Comment: 27 pages, 14 figures, 4 tables, paper accepte

Relativistic structure, stability, and gravitational collapse of charged neutron stars