Competing Local and Non-Local alpha-effects for a Simplified Flux Transport Dynamo Model

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• Peter Mann (University of Cambridge)
• Tuesday 27 October 2009, 13:00-14:00
• MR14, DAMTP, Pav. F.

If you have a question about this talk, please contact Dr. Aurélien Crida.

The solar magnetic field is maintained by a hydromagnetic dynamo, and it is generally accepted that strong toroidal magnetic field is produced at the tachocline below the solar convection zone. The location of production of the poloidal field via the alpha-effect is still in question. One such location is the solar surface, where decay of bipolar magnetic regions produces poloidal magnetic field, this is known as the Babcock-Leighton mechanism. Another possible location is the base of the solar convection zone. Recent work has looked at the competition in the solar dynamo between surface and deep-seated alpha-effects. The alpha-effects studied were local effects. However, flux-transport dynamo calculations use non-local poloidal source terms, that is, they act at the surface but are proportional to the toroidal field at the base of the convection zone. We will discuss the effects of non-local competing alpha-effects on the dynamo equations to explore the validity of this type of model. We will also include the effects of meridional circulation.

This talk is part of the DAMTP Astro Lunch series.

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