The D/H ratio and the evolution of water in the terrestrial planets.
The presence of liquid water at the surface of the Earth has played a major role in the biological evolution of the Earth. None of the other terrestrial planets--Mercury, Venus and Mars--has liquid water at its surface. However, it has been suggested, since the early seventies, from both geological and atmospheric arguments that, although Venus and Mars are presently devoid of liquid water, their surfaces could have been partially or completely covered by water at some time of their evolution. There are many possible diagnostics of the long-term evolution of the planets, either from the present characteristics of their surfaces or from their present atmospheric compositions. Among them, the present value of the D/H ratio is of particular interest, although its significance in terms of long term evolution has been challenged by some authors. Recent progress has been made in this field. We now have evidence for higher D/H ratios on Mars and Venus than on Earth, with an enrichment factor of the order of 5 on Mars, and about 100 on Venus. Any scenario for the evolution of these planets must take this into The most recent models on the evolution of Mars and Venus are reviewed in light of these new measurements.
de Bergh
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Observatoire de Paris, Departement de Recherche Spatiale, Meudon, France.
D001272:Atmosphere / Q000032:analysis / Q000737:chemistry; D003903:Deuterium / Q000032:analysis*; D018534:Earth, Planet; D019419:Evolution, Planetary; D005118:Extraterrestrial Environment; D006859:Hydrogen / Q000032:analysis*; D018535:Mars; D013057:Spectrum Analysis; D018536:Venus; D014867:Water / Q000737:chemistry*
D014867:Water; D006859:Hydrogen; D003903:Deuterium