A simplified numerical model of coronal energy dissipation based on   reduced MHD
  A 3D model intermediate between cellular automata (CA) models and the reduced magnetohydrodynamic (RMHD) equations is presented to simulate solar impulsive events generated along a coronal magnetic loop. The model consists of a set of planes distributed along a magnetic loop between which the information propagates through Alfven waves. Statistical properties in terms of power-laws for energies and durations of dissipative events are obtained, and their agreement with X-ray and UV flares observations is discussed. The existence of observational biases is also discussed. 
E. Buchlin, V. Aletti, S. Galtier, M. Velli, G. Einaudi, J.-C. Vial