Spectroscopic observations of the planets

Details Spectroscopic observations of the planets Spectroscopic observations of the planets

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986plas.rept...51o&link_type=abstract

In NASA, Washington Reports of Planetary Astronomy, 1985 p 51-52 (SEE N87-12407 03-89)

Astronomy and Astrophysics

Astronomy

Planetary Atmospheres, Planetary Composition, Planetary Structure, Satellite Atmospheres, Deuterium Compounds, Jupiter (Planet), Methane, Saturn (Planet), Titan, Ultraviolet Spectra, Uranus (Planet)

Scientific paper

The first phase of a program to determine D/H in the atmospheres of all of the major planets and Titan was completed. D/H on Titan and Uranus is significantly higher than on Jupiter and Saturn. Titan has the highest value, consistent with the possibility for hydrogen escape. These measurements were all made in terms of CH3D/CH4. They suggest that at least two reservoirs for deuterium exist in the outer solar system - a large one in hydrogen and a much smaller one in hydrogen-containing compounds that have not isotopically equilibrated with the hydrogen. This result also demonstrates that a large fraction of the carbon in the outer solar nebula was in the form of methane and it supports the nucleation model for the formation of the outer planets. Other studies included an investigation of the phosphine abundance over the Great Red Spot (GRS) of Jupiter, pre-Voyager determination of the amount of acetylene on Uranus, and the carbon isotope ratio in Halley's Comet. UV spectra of the GRS obtained with the IUE show no evidence of the enhancement of phosphine that would be expected if the red color of this object is caused by P4.

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