Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-11-28T21:39:31.399Z Has data issue: false hasContentIssue false
  • English
  • Français

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

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.

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