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The global scales of solar convection are studied through three-dimensionalsimulations of compressible convection carried out in spherical shells ofrotating fluid which extend from the base of the convection zone to within 15Mm of the photosphere. Such modelling at the highest spatial resolution to dateallows study of distinctly turbulent convection, revealing that coherentdownflow structures associated with giant cells continue to play a significantrole in maintaining the strong differential rotation that is achieved. Thesegiant cells at lower latitudes exhibit prograde propagation relative to themean zonal flow, or differential rotation, that they establish, and retrogradepropagation of more isotropic structures with vortical character at mid andhigh latitudes. The interstices of the downflow networks often possess strongand compact cyclonic flows. The evolving giant-cell downflow systems can bepartly masked by the intense smaller scales of convection driven closer to thesurface, yet they are likely to be detectable with the helioseismic probingthat is now becoming available. Indeed, the meandering streams and varyingcellular subsurface flows revealed by helioseismology must be samplingcontributions from the giant cells, yet it is difficult to separate out thesesignals from those attributed to the faster horizontal flows ofsupergranulation. To aid in such detection, we use our simulations to describehow the properties of giant cells may be expected to vary with depth, how theirpatterns evolve in time, and analyze the statistical features of correlationswithin these complex flow fields.

Structure and Evolution of Giant Cells in Global Models of Solar Convection