Calculation of the coronal heating rate by dissipation of magnetic energy

The observations made during the last years have shown that the solar corona is a very inhomogeneus medium composed by a wide variety of magnetic loops. Moreover, the magnetic field plays a very important role in the energy balance of the region. We suggest that the stationary heating of the solar corona is produced by dissipation of magnetohydrodinamic turbulence. We derive an estimation of the coronal heating rate which is comparable to the rates of conductive and radiative cooling.Asociación Argentina de Astronomí