Solar poloidal magnetic field generation rate from observations and mean-field dynamos

Abstract To estimate the hemispheric flux generation rate of the large-scaleradial magnetic field in the solar cycles 23 and 24 we use the photosphericobservations of the solar magnetic fields and results of the mean-fielddynamo models. Our analysis suggests that the hemispheric flux generationrate can be determined by the turbulent diffusion of the dynamo generatedmagnetic field at the solar equator. Observational data suggest thatspeed of magnetic field reconnection across equator, which representsthe effect of the latitudinal turbulent diffusion, can be insufficientto explain the magnitude of the hemispheric poloidal flux generationrate in the solar cycles 23 and 24. In addition, the results of dynamomodel show the powerful impact of the radial turbulent diffusion ofthe large-scale poloidal magnetic field on the hemispheric magneticflux generation rate and the global magnetic field distribution insidethe convection zone.