Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-24T18:24:58.793Z Has data issue: false hasContentIssue false
  • English
  • Français

Turbulent Transport of Magnetic Fields and the Solar Dynamo

Published online by Cambridge University Press:  19 July 2016

L.L. Kichatinov
L.L. Kichatinov*
Affiliation:
Astrophysikalisches Institut Potsdam An der Sternwarte 16, D-O-1590 Potsdam, Germany

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 effect of anisotropic transport of the mean magnetic field by turbulence in a stratified rotating fluid is briefly discussed to find its qualitative correspondence to the observed field redistribution over a solar cycle. A kinematic model of a dynamo in a spherical shell is developed with the transport effect included to assess its importance in a more consistent way. The anisotropic transport brings the simulated field behavior closer to that observed on the Sun.

Type
1. The Solar Dynamo
Information
Symposium - International Astronomical Union , Volume 157: The Cosmic Dynamo , 1993 , pp. 13 - 17
Copyright
Copyright © Kluwer 1993 

References

Durney, B.R. and Latour, J: 1978, Geophys. Astrophas. Fluid Dyn. 9, 241 CrossRefGoogle Scholar
Kichatinov, L.L.: 1988, Astron. Nachr. 309, 197 CrossRefGoogle Scholar
Kichatinov, L.L.: 1991, Astron. Astrophys. 243, 483 Google Scholar
Libbrecht, K.G.: 1989, Astrophys. J. 336, 1092 CrossRefGoogle Scholar
Spitzer, L.: 1957, Astrophys. J. 125, 525 CrossRefGoogle Scholar
Stenflo, J.O.: 1988, Astrophys. Space Sci. 144, 321 CrossRefGoogle Scholar
Zeldovich, Ya.B.: 1957, Sov. Phys. JETP 4, 460 Google Scholar