  The thin shell collapse leading to the formation of charged rotating black
holes in three dimensions is analyzed in the light of a recently developed
Hamiltonian formalism for these systems. It is proposed to demand, as a way to
reconcile the properties of an infinitely extended solenoid in flat space with
a magnetic black hole in three dimensions, that the magnetic field should
vanish just outside the shell. The adoption of this boundary condition results
in an exterior solution with a magnetic field different from zero at a finite
distance from the shell. The interior solution is also found and assigns
another interpretation, in a different context, to the magnetic solution
previously obtained by Cl\'{e}ment and by Hirschmann and Welch.
