  We model the hydrodynamic evolution of the plasma confined in a coronal loop,
30000 km long, subject to the heating of nanoflares due to intermittent
magnetic dissipative events in the MHD turbulence produced by loop footpoint
motions. We use the time-dependent distribution of energy dissipation along the
loop obtained from a hybrid shell model, occurring for a magnetic field of
about 10 G in corona; the relevant heating per unit volume along the loop is
used in the Palermo-Harvard loop plasma hydrodynamic model. We describe the
results focussing on the effects produced by the most intense heat pulses,
which lead to loop temperatures between 1 and 1.5 MK.

Astrophysics