Magnetic Energy Dissipation in the Solar Corona

In this paper we discuss the problem of small scale generation in a nonuniform magnetized plasma. In a MHD framework, we show that the free-energy stored in the inhomogenous, large scale coronal magnetic fields can be transferred on smaller and smaller scales up to the dissipative ones. This energy transfer is induced by the presence of MHD waves of “modest” amplitude (i.e. for which the non-linear time is much longer than the Alfvén time) which are likely to be generated in the solar athmosphere.