  In this paper, we investigate a simple model where two, initially
unconnected, flux systems are forced to interact in response to the imposed
boundary driving by solving the non-ideal 3D MHD equations numerically. The
reconnection rate of the dynamical process is determined and compared with the
corresponding rate for the potential evolution of the magnetic field. This
shows that the dynamic reconnection rate is about a factor of two smaller than
the potential (perfect, instantaneous) rate for realistic solar driving
velocities demonstrating that this three-dimensional magnetic reconnection
process is fast.
  The energy input for a fixed advection distance is found to be independent of
the driving velocity. The Joule dissipation associated with the reconnection
process is also found to be basically dependent on the advection distance
rather than driving velocity. This implies that the timescale for the event
determines the effect the heating has on the temperature increase.
  Finally, the numerical experiments indicate that the observational structure
of the reconnection site changes dramatically depending on the phase of the
evolution of the passage of the two flux sources. In the initial phase, where
the sources become connected, the heating is confined to a compact region. For
the disconnecting phase the energy gets distributed over a larger area due to
the reconnected field line connectivity.
