Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...406..285m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 406, no. 1, p. 285-297.
Astronomy and Astrophysics
Astrophysics
52
Atmospheric Chemistry, Carbon Monoxide, Hydrocyanic Acid, Neptune Atmosphere, Uranus Atmosphere, Line Spectra, Millimeter Waves, Radio Telescopes, Planets, Neptune, Uranus, Carbon Monoxide, Wavelengths, Atmsophere, Chemistry, Hydrogen Cyanide, Emissions, Earth-Based Observations, Stratosphere, Troposphere, Abundance, Origin, Source, Convection, Nitrogen, Ammonia, Raditive Transfer, Opacity, Temperature, Spectra, Distribution, Frequencies, Comparison, Model, Thermochemistry, Triton, Satellites
Scientific paper
Observations are presented which show that CO is present in both the troposphere and stratosphere of Neptune, whereas is confined to the Neptune stratosphere with a mean mole fraction in the 0.003-30 mbar pressure level range of 1.0 x 10 exp -9. CO is present in both the stratosphere and in the troposphere with a uniformly mixed model fraction of 1.2 x 10 exp -6. Upper limits of 1.0 x 10 exp -10 and 3.0 x 10 exp -8 mole fractions are derived for HCN and CO respectively on Uranus. The origin of these species in the atmosphere of Neptune and their nondetection in that of Uranus are discussed in detail. It is concluded that the most plausible scenario involves upward convection of CO and N2 from Neptune's deep interior and a failure of chemical equilibrium at deep atmospheric levels, allowing excess CO and presumably N2 to reach the upper atmosphere. Nondetection in Uranus may be explained by the lack of a significant internal heat source in the planet and consequent suppression of vertical convection.
Atreya Sushil K.
Deane J. R.
Gautier Daniel
Marten André
Matthews Henry E.
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