  In a recent computational campaign [Ng et al., Astrophys. J. 747, 109, 2012]
to investigate a three-dimensional model of coronal heating using reduced
magnetohydrodynamics (RMHD), we have obtained scaling results of heating rate
versus Lundquist number based on a series of runs in which random photospheric
motions are imposed for hundreds to thousands of Alfv\'en time in order to
obtain converged statistical values. Using this collection of numerical data,
we have performed additional statistical analysis related to the formation of
current sheets and heating events, or nanoflares [Parker, Astrophys. J. 330,
474, 1988]. While there have been many observations of the energy distribution
of solar flares, there have not been many results based on large-scale
three-dimensional direct simulations due to obvious numerical difficulties. We
will present energy distributions and other statistics based on our
simulations, calculated using a method employed in [Dmitruk & G\'omez,
Astrophys. J., 484, L83, 1997]. We will also make comparisons of our results
with observations.
