Hostname: page-component-cd9895bd7-p9bg8 Total loading time: 0 Render date: 2024-12-25T16:33:00.477Z Has data issue: false hasContentIssue false

Magnetic confinement in the solar interior

Published online by Cambridge University Press:  12 August 2011

Toby S. Wood*
Affiliation:
Baskin School of Engineering, University of California Santa Cruz, 1156 High Street, Santa Cruz, CA 95064 email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Gough, D. O. & McIntyre, M. E. 1998, Nature, 394, 755CrossRefGoogle Scholar
Kitchatinov, L. L. & Rüdiger, G. 2008, AN, 329, 372Google Scholar
Schou, J., et al. 1998, ApJ, 505, 390CrossRefGoogle Scholar
Spiegel, E. A. & Zahn, J.-P. 1992, A&A, 265, 106Google Scholar
Tobias, S. M., Brummell, N. H., Clune, T. L., & Toomre, J. 2001, ApJ, 549, 11831203CrossRefGoogle Scholar
Wood, T. S. & McIntyre, M. E. 2010, J. Fluid Mech., submittedGoogle Scholar