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All theories that attempt to explain the heating of the high temperatureplasma observed in the solar corona are based on short bursts of energy. Theintensities and velocities measured in the cores of quiescent active regions,however, can be steady over many hours of observation. One heating scenariothat has been proposed to reconcile such observations with impulsive heatingmodels is the "long nanoflare storm," where short duration heating events occurinfrequently on many sub-resolutions strands; the emission of the strands isthen averaged together to explain the observed steady structures. In thisLetter, we examine the emission measure distribution predicted for such a longnanoflare storm by modeling an arcade of strands in an active region core.Comparisons of the computed emission measure distributions with recentobservations indicate that that the long nanoflare storm scenario impliesgreater than 5 times more 1 MK emission than is actually observed for allplausible combinations of loop lengths, heating rates, and abundances. Weconjecture that if the plasma had "super coronal" abundances, the model may beable to match the observations at low temperatures.

Can a Long Nanoflare Storm Explain the Observed Emission Measure Distributions in Active Region Cores?