Despite of the large number of models and mechanisms proposed in the literature, the problem of the heating of the solar corona is still unsolved and represents one of the challenge of solar physics. In this context, a basic question to be addressed by any viable theoretical model concerns understanding the mechanism capable of transferring “efficiently” the energy from the large injection scales to the much smaller dissipative scales in an almost ideal plasma where these scales differ by many order of magnitude. ©2000 American Institute of Physics.