  In solving the solar coronal heating problem, it is crucial to comprehend the
mechanisms by which energy is conveyed from the photosphere to the corona.
Recently, magnetic tornadoes, characterized as coherent, rotating magnetic
field structures extending from the photosphere to the corona, have drawn
growing interest as a possible means of efficient energy transfer. Despite its
acknowledged importance, the underlying physics of magnetic tornadoes remains
still elusive. In this study, we conduct a three-dimensional radiative
magnetohydrodynamic simulation that encompasses the upper convective layer and
extends into the corona, with a view to investigating how magnetic tornadoes
are generated and efficiently transfer energy into the corona. We find that a
single event of magnetic flux concentration merger on the photosphere gives
rise to the formation of a single magnetic tornado. The Poynting flux
transferred into the corona is found to be four times greater in the presence
of the magnetic tornado, as compared to its absence. This increase is
attributed to a reduction in energy loss in the chromosphere, resulting from
the weakened magnetic energy cascade. Based on an evaluation of the fraction of
the merging events, our results suggest that magnetic tornadoes contribute
approximately 50% of the Poynting flux into the corona in regions where the
coronal magnetic field strength is 10 G. Potentially, the contribution could be
even greater in areas with a stronger coronal magnetic field.
