Talk abstract

In this work we present results of 3D MHD numerical simulations of solar active regions. The main goal is to follow the storage of free magnetic energy due to conversion of kinetic energy associated to horizontal plasma motions. The free magnetic energy is stored as electric currents which develop mainly on the regions where the motion is applied. These electric currents can later be dissipated, heating and accelerating the plasma, and could give rise to two of the most energetic phenomena occurring in the solar atmosphere: flares and coronal mass ejections. We investigate the evolution of magnetic energy and the distribution of electric currents in the simulation box.