  The energy released in solar flares derives from a reconfiguration of
magnetic fields to a lower energy state, and is manifested in several forms,
including bulk kinetic energy of the coronal mass ejection, acceleration of
electrons and ions, and enhanced thermal energy that is ultimately radiated
away across the electromagnetic spectrum from optical to X-rays. Using an
unprecedented set of coordinated observations, from a suite of instruments, we
here report on a hitherto largely overlooked energy component -- the kinetic
energy associated with small-scale turbulent mass motions. We show that the
spatial location of, and timing of the peak in, turbulent kinetic energy
together provide persuasive evidence that turbulent energy may play a key role
in the transfer of energy in solar flares. Although the kinetic energy of
turbulent motions accounts, at any given time, for only $\sim (0.5-1)$\% of the
energy released, its relatively rapid ($\sim$$1-10$~s) energization and
dissipation causes the associated throughput of energy (i.e., power) to rival
that of major components of the released energy in solar flares, and thus
presumably in other astrophysical acceleration sites.
