Evidence
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In Babcock–Leighton dynamo models, the poloidal flux generated at the surface must be transported back to the base of the convection zone, and a poleward meridional circulation at the solar surface provides the required return path.
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A mean-field Babcock-Leighton solar dynamo model with long-term variability ↗
At the same time, the magnetic field of the following spot will also decay and connect with the polar magnetic field, which has opposite polarity. This process will at some point annihilate the flux in the polar region, causing a poloidal polarity reversal. In this case the poloidal and toroidal fie…
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At the same time, the magnetic field of the following spot will also decay and connect with the polar magnetic field, which has opposite polarity. This process will at some point annihilate the flux in the polar region, causing a poloidal polarity reversal. In this case the poloidal and toroidal fields regeneration processes are spatially separated (recall Figure 1 h to Figure 1 j); a mechanism transporting the new polar surface magnetic flux generated by the Babcock-Leighton mechanism to the bottom of the convection zone is necessary. Facing this requirement, initially a meridional circulation flow was assumed in Babcock-Leighton dynamo modeling. As a matter of fact, a poleward meridional flow is indeed observed at the solar surface ( Duvall Jr,, 1979 ) .