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We compare spectra of the zonal harmonics of the large-scale magnetic fieldof the Sun using observation results and solar dynamo models. The main solaractivity cycle as recorded in these tracers is a much more complicatedphenomenon than the eigen solution of solar dynamo equations with the growthsaturated by a back reaction of the dynamo-driven magnetic field on solarhydrodynamics. The nominal 11(22)-year cycle as recorded in each mode has aspecific phase shift varying from cycle to cycle; the actual length of thecycle varies from one cycle to another and from tracer to tracer. Both theobservation and the dynamo model show an exceptional role of the axisymmetric$\ell_{5}$ mode. Its origin seems to be readily connected with the formationand evolution of sunspots on the solar surface. The results of observations anddynamo models show a good agreement for the low $\ell_{1}$ and $\ell_{3}$modes. The results for these modes do not differ significantly for theaxisymmetric and nonaxisymmetric models. Our findings support the idea that thesources of the solar dynamo arise as a result of both the distributed dynamoprocesses in the bulk of the convection zone and the surface magnetic activity.

Solar large-scale magnetic field and cycle patterns in solar dynamo