Hostname: page-component-586b7cd67f-dsjbd Total loading time: 0 Render date: 2024-12-01T12:43:50.285Z Has data issue: false hasContentIssue false
  • English
  • Français

The Interaction of Weak and Strong Fields on the Sun

Published online by Cambridge University Press:  12 April 2016

Harold Zirin
Harold Zirin*
Affiliation:
Big Bear Solar Observatory California Institute of Technology Pasadena, CA 91125, USA

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 problems associated with unresolved flux elements are discussed. It is pointed out that the hypothesis that these fields are strong does explain various problems of solar magnetic fields, but, as all invisible phenomena, is difficult to test. It is pointed out that Zeeman splitting measurements, which give the true field, have revealed field strengths down to the lower limit of conventional spectroscopy (about 400 gauss) for years. Not one spectrogram showing larger splitting in plages or network has been produced. The power-law distribution of weak-field strengths suggests a hierarchy of field strengths, and the simple arithmetic of weak-field elements and tiny pores is on the edge of ruling out strong fields, and further improvement in resolution should do so.

Observations in the 12μ lines have shown plage fields of a few hundred gauss and broadening of the σ components due to field variation within the field of view. These data have been explained away on the basis of height variation in the field, but the requisite transverse field strength or center-limb behavior are not observed.

Type
Session 4. Friendly Debate: The Relation of Quiet Sun to Active Regions
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 215 - 221
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Deming, D. et al.: 1988, Ap. J., 333 978 CrossRefGoogle Scholar
Rabin, D.: 1992, Ap. J., 391 832 CrossRefGoogle Scholar
Stenflo, J. O. 1973, Solar Phys., 32 41 Google Scholar
Wang, J., Zirin, H., and Shi, Z.: 1985, Solar Phys., 98 241 Google Scholar
Zirin, H.: 1986, Aust.J.Phys. 38 961 Google Scholar
Zirin, H.: 1992, BBSO #344, submitted to Ap. J.Google Scholar
Zirin, H. and Popp, B.: 1989,Ap. J., 340, 571 Google Scholar
Zirin, H. and Wang, H.: 1992, Ap. J., 385 L27 CrossRefGoogle Scholar