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Title:
Detection of H3(+) infrared emission lines in Saturn
Authors:
Geballe, T. R.; Jagod, M.-F.; Oka, T.
Affiliation:
AA(Joint Astronomy Center, Hilo, HI), AB(Chicago Univ., IL), AC(Chicago Univ., IL)
Publication:
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 408, no. 2, p. L109-L112. (ApJL Homepage)
Publication Date:
05/1993
Category:
Lunar and Planetary Exploration; Saturn
Origin:
STI
NASA/STI Keywords:
Emission Spectra, Hydrogen, Infrared Spectra, Molecular Ions, Planetary Ionospheres, Saturn Atmosphere, Triatomic Molecules, Abundance, Morphology, Spectral Line Width
Keywords:
SATURN, EMISSIONS, HYDROGEN 3+, INFRARED, WAVELENGTHS, IONOSPHERE, POLAR REGION, COLUMN DENSITY, COMPARISON, INTENSITY, TEMPERATURE, MOLECULAR PROCESSES, EARTH-BASED OBSERVATIONS, SPECTRA, SPECTROSCOPY, MORPHOLOGY, ABUNDANCE, JUPITER, URANUS, ORIGIN, FORMATION, IONIZATION
DOI:
10.1086/186843
Bibliographic Code:
1993ApJ...408L.109G

Abstract

Three emission lines of the nu-2 fundamental vibration-rotation band of H3(+) have been detected in the ionosphere of Saturn near and at its poles. The peak observed column density of H3(+) (at the south limb) is more than two orders of magnitude lower than the column density at the south pole of Jupiter, and is less than that detected from Uranus. While the number and the S/N ratios of observed transitions are not sufficient to determine the temperature and abundance of H3(+) accurately, the observed emission intensities are consistent with a temperature of about 800 K and total column density of about 1.0 x 10 exp 11/sq cm.

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