Detection of H3(+) from Uranus

Details Detection of H3(+) from Uranus Detection of H3(+) from Uranus

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...405..761t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 405, no. 2, p. 761-766.

Astronomy and Astrophysics

Astronomy

64

Abundance, Emission Spectra, Energy Transfer, Hydrogen Ions, Infrared Astronomy, Uranus (Planet), Infrared Telescopes, Jupiter (Planet), Molecular Ions, Neptune (Planet), Saturn (Planet), Triatomic Molecules, Voyager 2 Spacecraft, Uranus, Infrared, Emissions, Jupiter, Spectrometry, Magnetosphere, Auroras, Telescope Methods, Earth-Based Observations, Description, Analysis, Comparisons, Gas Planets, Energy, Tritium, Wavelengths, Ions, Ionosphere, Composition, Neptune, Spectra, Temperature

Scientific paper

The detection of H3(+) in Uranus is reported. Using the CGS4 spectrometer on the UKIRT telescope, we clearly detected 11 emission features of the H3(+) fundamental vibration-rotation band between 3.89 and 4.09 microns. These features are composed primarily of lines from the Q-branch; the strongest of them is the Q(3) blend at 3.985 microns. Analysis of these features indicates a rotational temperature of 740 +/- 25 K, an ortho-H3(+) fraction of 0.51 +/- 0.03, and a disk-averaged H3(+) column abundance of 6.5 x 10 exp 10 (+/- 10 percent) molecules/sq cm. Comparison is made with Jupiter, Saturn, and Neptune. A detection of the H2 1-0 S(1) line in Uranus and an upper limit to H3(+) emission from Neptune also are reported. The rate of energy deposition into Uranus appears to be significantly higher than the rate reported during the Voyager 2 flyby in January of 1986.

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