  A 2.5-dimensional magnetohydrodynamics simulation analysis of the energy
release for three different reconnection regimes is presented. The system under
investigation consists in a current-sheet located in a medium with a strong
density variation along the current layer: such system is modeled as it were
located in the high chromosphere/low solar corona as in the case of pre- flare
and coronal mass ejection (CME) configurations or in the aftermath of such
explosive phenomena. By triggering different magnetic-reconnection dynamics,
that is from a laminar slow evolution to a spontaneous non-steady turbulent
reconnection [1,2,3], we observe a rather different efficiency and temporal
behavior with regard to the energy fluxes associated with each of these
reconnection-driven evolutions. These discrepancies are fundamental
key-properties to create realistic models of the triggering mechanisms and
initial evolution of all those phenomena requiring fast (and high power)
magnetic reconnection events within the solar environment.
  1. G. Lapenta, Phys. Rev. Lett. 100, 235001 (2008). 2. L. Bettarini, and G.
Lapenta, ApJ Submitted (2009). 3. M. Skender, and G. Lapenta, Phys. Plasmas
submitted (2009).
