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Exploring a different geometry for the solar tachocline in a kinematic solar dynamo model

Published online by Cambridge University Press:  01 November 2006

G. A. Guerrero  and
E. M. de Gouveia Dal Pino
G. A. Guerrero
Affiliation:
Department of Astronomy, Insituto de Astronomia, Geofísica e Ciências Atmosféricas, IAG-USP, Brazil email: [email protected], [email protected] Present address: IAG-USP, Rua do Matao, 1226, Sao Paulo, SP, Brazil
E. M. de Gouveia Dal Pino
Affiliation:
Department of Astronomy, Insituto de Astronomia, Geofísica e Ciências Atmosféricas, IAG-USP, Brazil email: [email protected], [email protected]
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Abstract

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Kinematic solar dynamo models (KSDM) that use a solar like differential rotation profile usually fail to reproduce the latitudinal distribution of the toroidal magnetic fields. Usually, it is assumed that it is the larger radial shear present in the solar tachocline at higher latitudes that is the responsible for such results. We here consider variations in the shape and thickness of the tachocline and find that a better distribution of the toroidal fields is obtained when the thickness of the tachocline is $d_1=0.02R_{\odot}$, a smaller value than that conventionally used.

Keywords

Solar magnetic fieldsMHDSolar dynamotachocline
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 45 - 48
Copyright
© 2006 International Astronomical Union