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Facular Models, the K-Line, and Magnetic Fields

Published online by Cambridge University Press:  30 March 2016

G. A. Chapman
G. A. Chapman*
Affiliation:
Space Sciences Laboratory, The Aerospace Corporation

Extract

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Photospheric faculae are now believed to be closely associated with the small-scale solar magnetic field. In order to obtain reliable observations of solar magnetic fields, one needs to have a good description of faculae, which is presently lacking. The problem in obtaining good observational data is severe because faculae are usually not spatially resolved, particularly so in the case of spectroscopic observations. Proper use of spectroscopic observations also requires some knowledge of solar velocity fields and atomic physics in the case of a non LTE analysis. Many of these problems can be avoided by making use of the wings of the Ca II K-line. The wing of this line is unaffected by magnetic and velocity effects. The formation of the line has become increasingly well understood and most of the wing (with the exception of the inner 1 - 2 Å) is formed in LTE. The line is so strong that its formation spans the whole depth of the photosphere.

Type
Joint Dicussions
Information
Highlights of Astronomy , Volume 4 , Issue 2: Highlights of Astronomy. As presented at the XVIth General Assembly of the IAU, 1976 (Part II) , 1977 , pp. 261 - 264
Copyright
Copyright © Reidel 1977

References

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