  Using multiwavelength imaging observations from the Atmospheric Imaging
Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) on 03 May 2012, we
present a novel physical scenario for the formation of a temporary X-point in
the solar corona, where plasma dynamics is forced externally by a moving
prominence. Natural diffusion was not predominant, however, a prominence driven
inflow occurred firstly, forming a thin current sheet and thereafter enabling a
forced magnetic reconnection at a considerably high rate. Observations in
relation to the numerical model reveal that forced reconnection may rapidly and
efficiently occur at higher rates in the solar corona. This physical process
may also heat the corona locally even without establishing a significant and
self-consistent diffusion region. Using a parametric numerical study, we
demonstrate that the implementation of the external driver increases the rate
of the reconnection even when the resistivity required for creating normal
diffusion region decreases at the X-point. We conjecture that the appropriate
external forcing can bring the oppositely directed field lines into the
temporarily created diffusion region firstly via the plasma inflows as seen in
the observations. The reconnection and related plasma outflows may occur
thereafter at considerably larger rates.
