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High-l Rydberg Lines of Fe I in the ATMOS Spectra: 4f–5g, 5g–6h …

Published online by Cambridge University Press:  03 August 2017

William G. Schoenfeld ,
Edward S. Chang  and
Murray Geller
William G. Schoenfeld
Affiliation:
Department of Physics and Astronomy, University of Massachusetts, Amherst, MA 01003, U.S.A.
Edward S. Chang
Affiliation:
Department of Physics and Astronomy, University of Massachusetts, Amherst, MA 01003, U.S.A.
Murray Geller
Affiliation:
Atmospheric and Cometary Sciences Section, Jet Propulsion Laboratory, Pasadena, CA 91109, U.S.A.

Abstract

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We have identified the Fe I 4f–5g lines at 4 μm in the ATMOS solar spectra. Using the polarization model as previously applied to silicon, we predict and identify the 5g–6h lines at 7 μm. Additional absorption features at 2.5 and 12 μm are also shown to be due to high-l Rydberg transitions in Fe I.

Keywords

atomic processesFe Iinfrared: starsline: identification
Type
Part 4: Infrared Atomic Physics and Line Formation
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 359 - 364
Copyright
Copyright © Kluwer 1994 

References

Chang, E.S.: 1984, J.Phys.B 17, L11.Google Scholar
Chang, E.S., and Noyes, R.W.: 1983, Physica Scripta 35, 792.Google Scholar
Cowan, R.D., and Andrew, K.L.: 1965, J. Opt. Soc. Am. 55, 502.Google Scholar
Edlén, B.: 1964, Encyclopedia of Physics Vol 27, Springer, Heidelberg.Google Scholar
Johansson, S., and Learner, R.C.M.: 1990, Astrophys. J. 354, 775.CrossRefGoogle Scholar
Johansson, S., Nave, G., Geller, M., Sauval, A.J., Grevesse, N.: 1993, these proceedings.Google Scholar