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Round table discussion of session G: MHD convection and dynamos

Published online by Cambridge University Press:  01 August 2006

Juri Toomre
Juri Toomre*
Affiliation:
JILA & Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder CO 80309-0440, USA. email: jtoomre@jila.colorado.edu
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Abstract

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Vigorous discussion ensued about conditions under which both small-scale and global-scale dynamo action would be realized within real stars where the flow fields are expected to be highly turbulent and the magnetic Prandtl numbers small. Our nearest star reminds us that intricate boundary-layer phenomena may have to also be considered, such as the presence of a tachocline of rotational shear at the base of the solar convection zone revealed by helioseismology, which suggests that an interface dynamo may be at work to produce the observed 22-year cycles of large-scale magnetic activity.

Keywords

Magnetic fieldsSun: magnetic fieldsstars: magnetic fields(magnetohydrodynamics:) MHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 494 - 495
Copyright
Copyright © International Astronomical Union 2007