  The investigation of dynamics of the small scale magnetic field on the Sun
photosphere is necessary to understand the physical processes occurring in the
higher layers of solar atmosphere due to the magnetic coupling between the
photosphere and the corona. We present a simulation able to address these
phenomena investigating the statistics of magnetic loops reconnections. The
simulation is based on N-body model approach and is divided in two
computational layers. We simplify the convection problem, interpreting the
larger convective scale, mesogranulation, as the result of the collective
interaction of convective downflow of granular scale. The N-body advection
model is the base to generate a synthetic time series of nanoflares produced by
interacting magnetic loops. The reconnection of magnetic field lines is the
result of the advection of the magnetic footpoints following the velocity field
generated by the interacting downflows. The model gives a quantitative idea of
how much energy is expected to be released by the reconfiguration of magnetic
loops in the quiet Sun.
