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Analysis of Very High Excitation Fe I Lines (4f–5g) in the Solar Infrared Spectrum

Published online by Cambridge University Press:  03 August 2017

S. Johansson ,
G. Nave ,
M. Geller ,
A. J. Sauval  and
N. Grevesse
S. Johansson
Affiliation:
Department of Physics, University of Lund, Sölvegatan, 14, S-223 62 Lund, Sweden
G. Nave
Affiliation:
Blackett Laboratory, Imperial College of Science, Technology and Medicine, London SW7 2BZ, England
M. Geller
Affiliation:
Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, U.S.A.
A. J. Sauval
Affiliation:
Observatoire Royal de Belgique, avenue circulaire, 3, B-1180 Brussels, Belgium
N. Grevesse
Affiliation:
Institut d'Astrophysique, Université de Liège, B-4000 Cointe-Liège, Belgium

Abstract

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We present a detailed analysis of very high excitation lines (4f–5g) of Fe I which are present in the spectral region 2545–2585 cm–1 in high resolution spectra both in the laboratory and in the ATMOS solar spectra obtained from space. A value of the solar abundance of iron which agrees with the meteoritic value is derived.

Keywords

infrared: starsline: identificationSun: abundances
Type
Part 6: The Infrared Spectrum
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 543 - 548
Copyright
Copyright © Kluwer 1994 

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