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We study the toroidal magnetic flux budget of the axisymmetric part of a 3Dmean-field dynamo model of Solar Cycles 23 and 24. The model simulates theglobal solar dynamo that includes effects of the formation and evolution ofbipolar magnetic regions emerging on the solar surface. Our analysis shows thatthe hemispheric magnitude of the net axisymmetric toroidal magnetic field inthe bulk of the convection zone is partly defined by the surface parameters ofthe differential rotation and the axisymmetric radial magnetic field. Thecontribution of the rotational radial shear to the net axisymmetric toroidalfield production has the same magnitude and it goes nearly sin-phase with theeffect of the latitudinal differential rotation. For our model, the effect ofthe radial shear to the net axisymmetric toroidal magnetic field is determinedmostly by the near equatorial regions that are slightly above and below thebottom of the convection zone. Also, we find that the toroidal field generationrate depends strongly on the latitudinal profile of the axisymmetric radialmagnetic field near the poles. We find that the magnitude of the axisymmetrictoroidal flux generation rate in the 3D dynamo model is by about 10 percenthigher than in the axisymmetric 2D mean-field dynamo model, due to the bipolaractive regions.

Toroidal Magnetic Flux Budget in Mean-Field Dynamo Model of Solar Cycles 23 and 24