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High-n Hydrogen Lines in Solar Infrared Spectra from Balloon-borne, Mauna Kea, and ATMOS Observations

Published online by Cambridge University Press:  03 August 2017

R. T. Boreiko ,
T. A. Clark ,
D. A. Naylor  and
J. R. Busler
R. T. Boreiko
Affiliation:
Center for Astrophysics and Space Astronomy, University of Colorado, Campus Box 389, Boulder, CO 80309, U.S.A.
T. A. Clark
Affiliation:
Physics Department, University of Calgary, Calgary, Alberta T2N 1N4 Canada
D. A. Naylor
Affiliation:
Department of Physics, University of Lethbridge, Lethbridge, Alberta T1K 3M4, Canada
J. R. Busler
Affiliation:
Physics Department, University of Calgary, Calgary, Alberta T2N 1N4 Canada

Abstract

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This paper reports the observation of high-n lines in emission from n = 12-11, 13-12, 14-13 and 16-15 Rydberg transitions in H, Mg and Si in solar far IR spectra taken from balloon altitudes, in which the H I line intensities are found to exceed those from the heavier elements. Tentative identification is also made of the n = 8-7 hydrogen line in emission on 20 μm spectra taken from Mauna Kea. The characteristics of the hydrogen lines are compared with lower-n transitions seen in the Space Shuttle ATMOS spectra, in which Brackett, Pfund and n = 6 lines with Δn = 1, 2, 3 and 4 are seen as broad absorption features, while the n = 7-6 line shows a small emission peak within a broader absorption line and the n = 9-7, and possibly the 11-8, transitions appear as weak emission lines. These results indicate that the transformation from absorption to emission occurs at longer wavelengths for hydrogen lines than for those of heavier elements.

Keywords

H Iinfrared: starsline: formationline: identificationSun: atmosphere
Type
Part 4: Infrared Atomic Physics and Line Formation
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 365 - 370
Copyright
Copyright © Kluwer 1994 

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