  We investigate an intensification mechanism for the magnetic field near the
base of the solar convection zone that does not rely on differential rotation.
Such mechanism in addition to differential rotation has been suggested by
studies of flux emergence, which typically require field strength in excess of
those provided by differential rotation alone. We study here a process in which
potential energy of the superadiabatically stratified convection zone is
converted into magnetic energy. This mechanism, know as explosion of magnetic
flux tubes, has been previously studied in the thin flux tube approximation as
well as two-dimensional MHD simulations, we expand the investigation to
three-dimensional MHD simulations. Our main result is that enough
intensification can be achieved in a three-dimensional magnetic flux sheet as
long as the spatial scale of the imposed perturbation normal to the magnetic
field is sufficiently large. When this spatial scale is small, the flux sheet
tends to rise toward the surface, resulting in a significant decrease of the
magnetic field amplification.
