  One candidate-model for heating the solar corona is magnetic reconnection
that embodies Ohmic dissipation of current sheets. When numerous small-scaled
magnetic reconnection occur, then it is possible to heat the corona. Due to the
limitations of current instrumentation, nanoflares cannot be resolved. But
their importance is evaluated via statistics by finding the power-law index of
the energy distribution. This method is however biased due to technical and
physical reasons. We aim to overcome limitations imposed by observations and
statistical analysis. This way, we will identify, and study the small scale
impulsive events. We employ a three-dimensional magnetohydrodynamic (3D-MHD)
simulation using the \bifrost code. We also employ a new technique to identify
the evolution of 3D Joule heating events in the corona. Then, we derive
parameters describing the heating events in these locations. We report on the
identification of heating events. We obtain the distribution of duration,
released energy, and volume. We also find weak power-law correlation between
these parameters. In addition, we extract information about geometrical
parameters of 2D slices of 3D events, and about the evolution of resolved Joule
heating compared to the total Joule heating and the magnetic energy in the
corona. Even though the energy power index is less than 2, when classifying the
energy release into three categories regarding with respect to the energy
release (pico-, nano-, and micro-events), we find that nano-events release $82
\ \%$ of the resolved energy. This fraction corresponds to an energy flux
larger than the one needed to heat the corona. It seems that the most popular
population is the one containing short-lived, with small spatial extend events.
