The solar corona host one of the most impulse events of the Solar System: solar flares. In a nutshell a flare is a impulse, intermittent and localized event that can cause solar temperature to increase up to 107 K.  Moreover, their spatial coincidence of flares with magnetic structures at the solar surface clearly indicates that their energy originates from the Sun’s magnetic field with magnetic reconnection as one of the possible physical origins of the phenomena.

Systematic studies of flares observed from the extreme ultraviolet to soft X-rays revealed (Dennis, 1985; Aschwanden, 2011 and references there in) showed that  the frequency distribution of solar flare energy release follows a well-defined power law, spanning 8 orders of magnitude in flare energy.

Lu & Hamilton proposed, for the first time, in 1991 a way to explain the observed power-laws assuming that solar flares are avalanches of several reconnection events occurring in a solar coronal loop.

To explore this concept, we have developed an avalanche model for solar flares, using magnetic field lines as the main dynamical element. Our model represents a coronal loop as a bundle of interwoven magnetic flux strands. It is a 2D cellular automaton with anisotropic connectivity, where the “field lines” represent the strands of the coronal loop. The model simulates the system's dynamics through random deformation of these strands, with magnetic reconnection occurring whenever two strands intersect at a lattice site and form an angle exceeding a predefined threshold.

We have shown that this system produces avalanches of reconnection events characterized by scale-free size distributions that compare very well with existing observations (Morales & Charbonneau, 2008 and 2009).  In this work we focus on the temporal characteristics of the model. We study three different definitions of waiting time plus the statistics of onset and release time.