  We investigate intensity variations and energy deposition in five coronal
loops in active region cores. These were selected for their strong variability
in the AIA/SDO 94 {\AA} intensity channel. We isolate the hot Fe XVIII and Fe
XXI components of the 94 {\AA} and 131 {\AA} by modeling and subtracting the
"warm" contributions to the emission. HMI/SDO data allow us to concentrate on
"inter-moss" regions in the loops. The detailed evolution of the inter-moss
intensity time series reveals loops that are impulsively heated in a mode
compatible with a nanoflare storm, with a spike in the hot 131 {\AA} signals
leading and the other five EUV emission channels following in progressive
cooling order. A sharp increase in electron temperature tends to follow closely
after the hot 131 {\AA} signal confirming the impulsive nature of the process.
A cooler process of growing emission measure follows more slowly. The Fourier
power spectra of the hot 131 {\AA} signals, when averaged over the five loops,
present three scaling regimes with break frequencies at (0.1/min) and
(0.7/min). The low frequency regime corresponds to 1/f noise; the intermediate
indicates a persistent scaling process and the high frequencies show white
noise. Very similar results are found for the energy dissipation in a 2-D
"hybrid" shell model of loop magneto-turbulence, based on reduced
magnetohydrodynamics, which is compatible with nanoflare statistics. We suggest
that such turbulent dissipation is the energy source for our loops.
