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We argue that the magnetically closed corona evolves primarilyquasi-statically, punctuated by many localized bursts of activity associatedwith magnetic reconnection at a myriad of small current sheets. The sheets formby various processes that do not involve a traditional turbulent cascadewhereby energy flows losslessly through a continuum of spatial scales startingfrom the large scale of the photospheric driving. If such an inertial range isa defining characteristic of turbulence, then the magnetically closed corona isnot a turbulent system. It nonetheless has a complex structure that bears nodirect relationship to the pattern of driving.

How Turbulent is the Magnetically Closed Corona?