  The Gauss-Codazzi method is used to discuss the gravitational collapse of a
charged Reisner-Nordstr\"om domain wall. We solve the classical equations of
motion of a thin charged shell moving under the influence of its own
gravitational field and show that a form of cosmic censorship applies. If the
charge of the collapsing shell is greater than its mass, then the collapse does
not form a black hole. Instead, after reaching some minimal radius, the shell
bounces back. The Schrodinger canonical formalism is used to quantize the
motion of the charged shell. The limits near the horizon and near the
singularity are explored. Near the horizon, the Schrodinger equation describing
evolution of the collapsing shell takes the form of the massive wave equation
with a position dependent mass. The outgoing and incoming modes of the solution
are related by the Bogolubov transformation which precisely gives the Hawking
temperature. Near the classical singularity, the Schrodinger equation becomes
non-local, but the wave function describing the system is non-singular. This
indicates that while quantum effects may be able to remove the classical
singularity, it may also introduce some new effects.
