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Magnetic confinement in the solar interior

Published online by Cambridge University Press:  12 August 2011

Toby S. Wood
Toby S. Wood*
Affiliation:
Baskin School of Engineering, University of California Santa Cruz, 1156 High Street, Santa Cruz, CA 95064 email: tsw25@soe.ucsc.edu
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Abstract

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The observed uniform rotation of the Sun's radiative interior can be explained by the presence of a global-scale interior magnetic field, provided that the field remains confined below the convection zone. In high latitudes, such magnetic confinement is possible by means of persistent downwelling, driven by the convection zone's turbulent stresses.

Keywords

MHDSun: abundancesSun: interiorSun: magnetic fieldsSun: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 409 - 410
Copyright
Copyright © International Astronomical Union 2011

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