  All theories that attempt to explain the heating of the high temperature
plasma observed in the solar corona are based on short bursts of energy. The
intensities and velocities measured in the cores of quiescent active regions,
however, can be steady over many hours of observation. One heating scenario
that has been proposed to reconcile such observations with impulsive heating
models is the "long nanoflare storm," where short duration heating events occur
infrequently on many sub-resolutions strands; the emission of the strands is
then averaged together to explain the observed steady structures. In this
Letter, we examine the emission measure distribution predicted for such a long
nanoflare storm by modeling an arcade of strands in an active region core.
Comparisons of the computed emission measure distributions with recent
observations indicate that that the long nanoflare storm scenario implies
greater than 5 times more 1 MK emission than is actually observed for all
plausible combinations of loop lengths, heating rates, and abundances. We
conjecture that if the plasma had "super coronal" abundances, the model may be
able to match the observations at low temperatures.
