  The coronal heating has remained a puzzle for decades since its observation
in 1940. Several space missions have been planned to resolve this conundrum in
the past and many more intend to target this issue in the future. The unfolding
of this issue will not only advance the fundamentals of astrophysical science
but also promise an improvement in space weather prediction. Its origin has
been debated without complete convergence; the acoustic waves,
magneto-hydrodynamic waves, and micro/nano-flares are the strongest candidates
so far to explain the mystery of coronal heating. However, none of these
processes significantly justifies the million-degree temperature of the solar
corona and the problem remains unsolved to date. Here, we propose a new
physical mechanism to explain the observed heating of the solar corona. The
statistical energy created during the interaction of the spin magnetic moment
of the plasma particles with the turbulent and continuously evolving coronal
magnetic field could substantiate the observed million-degree coronal
temperature.
