Hostname: page-component-848d4c4894-ttngx Total loading time: 0 Render date: 2024-05-26T05:57:19.056Z Has data issue: false hasContentIssue false
  • English
  • Français

Magnetohydrodynamic 3-D Models of the Solar Convection Zone

Published online by Cambridge University Press:  30 March 2016

Allan Sacha Brun
Allan Sacha Brun*
Affiliation:
DSM/DAPNIA/SAp, CEA-Saclay, 91191 Gif-sur-Yvette, France

Extract

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.

We have conducted 3-D simulations of the complex magnetohydrodynamics of the solar convective envelope in spherical shells using our anelastic spherical harmonics (ASH) code (Brun & Toomre 2002). We here briefly discuss the properties of the kinetic and current helicities established in such systems.

Type
I. Joint Discussions
Information
Highlights of Astronomy , Volume 13 , 2005 , pp. 94
Copyright
Copyright © Astronomical Society of Pacific 2005

References

Brun, A.S. & Toomre, J. 2002, ApJ, 570, 865.CrossRefGoogle Scholar
Brun, A.S., Miesch, M.S. & Toomre, J. 2004, ApJ 614, 1073.CrossRefGoogle Scholar
Pevtsov, A.A, Canfield, R.C. & Latushko, S.M. 2001, ApJ, 549, L261.CrossRefGoogle Scholar