Hostname: page-component-586b7cd67f-rcrh6 Total loading time: 0 Render date: 2024-11-30T17:05:00.433Z Has data issue: false hasContentIssue false
  • English
  • Français

Helioseismic inferences

Published online by Cambridge University Press:  26 February 2010

Hiromoto Shibahashi
Hiromoto Shibahashi*
Affiliation:
Department of Astronomy, University of Tokyo, Tokyo 113-0033, Japan 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 brilliant outcome of some 30 years of helioseismology spreads over a wide range of topics. Some highlights relevant to the cause of the solar activity cycle are listed up. The rotation profile in the solar convective zone is discussed as an important source of the dynamo mechanism. The kinematic dynamo model is described in the linear approximation, and the condition for the solar type dynamo is derived. It is shown that comparison of this condition with the rotation profile determined from helioseismology is useful to identify the possible seats of the dynamo.

Keywords

magneothydrodynamics: MHDSun: activitySun: helioseismologySun: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S264: Solar and Stellar Variability: Impact on Earth and Planets , August 2009 , pp. 33 - 38
Copyright
Copyright © International Astronomical Union 2010

References

Leighton, R. B., Noyes, R. W., & Simon, G. W. 1962, ApJ, 135, 474CrossRefGoogle Scholar
Parker, E. N. 1955, ApJ, 122, 293CrossRefGoogle Scholar
Schou, J. et al. 1998, ApJ, 505, 390CrossRefGoogle Scholar
Yoshimura, H. 1975, ApJ, 201, 740CrossRefGoogle Scholar