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In this work we take advantage of eleven different sunspot group, sunspot,and active region databases to characterize the area and flux distributions ofphotospheric magnetic structures. We find that, when taken separately,different databases are better fitted by different distributions (as has beenreported previously in the literature). However, we find that all our databasescan be reconciled by the simple application of a proportionality constant, andthat, in reality, different databases are sampling different parts of acomposite distribution. This composite distribution is made up by linearcombination of Weibull and log-normal distributions -- where a pure Weibull(log-normal) characterizes the distribution of structures with fluxes below(above) $10^{21}$Mx ($10^{22}$Mx). We propose that this is evidence of twoseparate mechanisms giving rise to visible structures on the photosphere: onedirectly connected to the global component of the dynamo (and the generation ofbipolar active regions), and the other with the small-scale component of thedynamo (and the fragmentation of magnetic structures due to their interactionwith turbulent convection). Additionally, we demonstrate that the Weibulldistribution shows the expected linear behavior of a power-law distribution(when extended into smaller fluxes), making our results compatible with theresults of Parnell et al. (2009).

Small-Scale and Global Dynamos and the Area and Flux Distributions of Active Regions, Sunspot Groups, and Sunspots: A Multi-Database Study