Monodeuterated methane in the outer solar system. IV - Its detection and abundance on Neptune

Details Monodeuterated methane in the outer solar system. IV - Its detection and abundance on Neptune Monodeuterated methane in the outer solar system. IV - Its detection and abundance on Neptune

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...355..661d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 355, June 1, 1990, p. 661-666.

Physics

Optics

28

Abundance, Methane, Neptune Atmosphere, Solar System, Astronomical Spectroscopy, Cassegrain Optics, Fourier Transformation, Uranus (Planet), Neptune, Methane, Abundance, Spectra, Earth-Based Observations, Gases, Spectroscopy, Comaparisons, Deuterium, Hydrogen, Isotopic Ratios, Ice, Infrared, Wavelengths, Outer Planets, Atmosphere, Icy Bodies, Volatiles, Condensates, Enrichment

Scientific paper

The 3nu2 band of CH3D was detected in the spectrum of Neptune near 1.6 micron recorded at a spectral resolution of 4/cm with the Cassegrain Fourier Transportation Spectrometer at the 3.6 m Canada-France-Hawaii Telescope CFHT) on Mauna Kea. The analysis of this spectrum, using spectral synthesis techniques, yielded a CH3D/CH4 ratio of about 0.0006, which corresponds to a global D/H ratio for Neptune of about 0.00012, if CH3D is in isotopic fractionation equilibrium with HD. This value is about an order of magnitude larger than an earlier estimate by Orton et al. (1987) based on deconvolution measurements of unresolved molecular emission in the 8-10-micron region. Comparison of this new determination with previous studies of CH3D in the outer solar system shows that, as in the case of Uranus, the D/H on Neptune is strongly enhanced over that found on Jupiter and Saturn and is comparable to the D/H in methane on Titan and in terrestrial methane and water.

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