The time evolution of a set of 22 M _ { \odot } unstable charged stars that collapse is computed integrating the Einstein-Maxwell equations .
The model simulate the collapse of an spherical star that had exhausted its nuclear fuel and have or acquires a net electric charge in its core while collapsing .
When the charge to mass ratio is Q / \sqrt { G } M \geq 1 the star do not collapse and spreads .
On the other hand , it is observed a different physical behavior with a charge to mass ratio 1 > Q / \sqrt { G } M > 0.1 .
In this case , the collapsing matter forms a bubble enclosing a lower density core .
We discuss an immediate astrophysical consequence of these results that is a more efficient neutrino trapping during the stellar collapse and an alternative mechanism for powerful supernova explosions .
The outer space-time of the star is the Reissner-Nordström solution that match smoothly with our interior numerical solution , thus the collapsing models forms Reissner-Nordström black holes .