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Various scenarios for the equatorward migration of sunspots

Published online by Cambridge University Press:  24 September 2020

Detlef Elstner Open the ORCID record for Detlef Elstner [Opens in a new window] ,
Yori Fournier  and
Rainer Arlt
Detlef Elstner
Affiliation:
Leibniz-Institute for Astrophysics Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: mailto:delstner@aip.de
Yori Fournier
Affiliation:
Leibniz-Institute for Astrophysics Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: mailto:delstner@aip.de
Rainer Arlt
Affiliation:
Leibniz-Institute for Astrophysics Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany email: mailto:delstner@aip.de
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Abstract

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The profile of the differential rotation together with the sign of the alpha-effect determine the dynamo wave direction. In early models of the solar dynamo the dynamo wave often leads to a poleward migration of the activity belts. Flux transport by the meridional flow or the effect of the surface shear layer are possible solutions. In a model including the corona, we show that various migrations can be obtained by varying the properties of the corona. A new dynamo of Babcock-Leighton type also leads to the correct equatorward migration by the non-linear relation between flux density and rise time of the flux.

Keywords

solar dynamosolar corona

References

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