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On Facular Models

Published online by Cambridge University Press:  14 August 2015

David E. Rees
David E. Rees*
Affiliation:
Dept. of Applied Mathematics, University of Sydney, Sydney, N.S.W. 2006, Australia

Abstract

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Weakenings of 14 FeI lines observed in photospheric faculae by Chapman and Sheeley (1968) have been analyzed using Unno's (1956) LTE theory of Zeeman triplet formation. These observations can be explained by a facula-photopshere temperature excess of ≲250 K in the layers ~ 100-400 km above τ5000 = 1. The inferred magnetic field in the faculae is ~ 1000 G.

Type
Part V: The Chromosphere in Active Regions
Information
Symposium - International Astronomical Union , Volume 56: Chromospheric Fine Structure , 1974 , pp. 177 - 178
Copyright
Copyright © Reidel 1974 

References

Chapman, G. A.: 1970, Solar Phys. 14, 315.CrossRefGoogle Scholar
Chapman, G. A. and Sheeley, N. R.: 1968, Solar Phys. 5, 442.Google Scholar
Unno, W.: 1956, Publ. Astron. Soc. Japan 8, 108.Google Scholar