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The evolution of a coronal loop is studied by means of numerical simulationsof the fully compressible three-dimensional magnetohydrodynamic equations usingthe HYPERION code. The footpoints of the loop magnetic field are advected byrandom motions. As a consequence the magnetic field in the loop is energizedand develops turbulent nonlinear dynamics characterized by the continuousformation and dissipation of field-aligned current sheets: energy is depositedat small scales where heating occurs. Dissipation is non-uniformly distributedso that only a fraction of the coronal mass and volume gets heated at any time.Temperature and density are highly structured at scales which, in the solarcorona, remain observationally unresolved: the plasma of our simulated loop ismulti-thermal, where highly dynamical hotter and cooler plasma strands arescattered throughout the loop at sub-observational scales. Numericalsimulations of coronal loops of 50000 km length and axial magnetic fieldintensities ranging from 0.01 to 0.04 Tesla are presented. To connect thesesimulations to observations we use the computed number densities andtemperatures to synthesize the intensities expected in emission lines typicallyobserved with the Extreme ultraviolet Imaging Spectrometer (EIS) on Hinode.These intensities are used to compute differential emission measuredistributions using the Monte Carlo Markov Chain code, which are very similarto those derived from observations of solar active regions. We conclude thatcoronal heating is found to be strongly intermittent in space and time, withonly small portions of the coronal loop being heated: in fact, at any giventime, most of the corona is cooling down.

Observational Signatures of Coronal Loop Heating and Cooling Driven by Footpoint Shuffling