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Rotation of the solar convection zone from helioseismology

Published online by Cambridge University Press:  01 August 2006

Jørgen Christensen-Dalsgaard
Jørgen Christensen-Dalsgaard*
Affiliation:
Institut for Fysik og Astronomi, Aarhus Universitet, DK-8000 Aarhus C, Denmark email: jcd@phys.au.dk
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Abstract

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Helioseismology has provided very detailed inferences about rotation of the solar interior. Within the convection zone the rotation rate roughly shares the latitudinal variation seen in the surface differential rotation. The transition to the nearly uniformly rotating radiative interior takes place in a narrow tachocline, which is likely important to the operation of the solar magnetic cycle. The convection-zone rotation displays zonal flows, regions of slightly more rapid and slow rotation, extending over much of the depth of the convection zone and converging towards the equator as the solar cycle progresses. In addition, there is some evidence for a quasi-periodic variation in rotation, with a period of around 1.3 yr, at the equator near the bottom of the convection zone.

Keywords

Sun: oscillationsSun: helioseismologySun: rotationSun: interior
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 393 - 404
Copyright
Copyright © International Astronomical Union 2007

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