Abstract
The original hydrogen isotope (D/H) ratios of different planetary bodies may indicate where each body formed in the Solar System. However, geological and atmospheric processes can alter these ratios through time. Over the past few decades, D/H ratios in meteorites from Vesta and Mars, as well as from S- and C-type asteroids, have been measured. The aim of this article is to bring together all previously published data from these bodies, as well as the Earth, in order to determine the original D/H ratio for each of these inner Solar System planetary bodies. Once all secondary processes have been stripped away, the inner Solar System appears to be relatively homogeneous in terms of water D/H, with the original water D/H ratios of Vesta, Mars, the Earth, and S- and C-type asteroids all falling between δD values of −100‰ and −590‰. This homogeneity is in accord with the ‘Grand tack’ model of Solar System formation, where giant planet migration causes the S- and C-type asteroids to be mixed within 1 AU to eventually form the terrestrial planets.This article is part of the themed issue ‘The origin, history and role of water in the evolution of the inner Solar System’.
Highlights
One contribution of 9 to a Theo Murphy meeting issue ‘The origin, history and role of water in the evolution of the inner Solar System’
Once all secondary processes have been stripped away, the inner Solar System appears to be relatively homogeneous in terms of water D/H, with the original water D/H ratios of Vesta, Mars, the Earth, and S- and C-type asteroids all falling between δD values of −100‰ and −590‰
This homogeneity is in accord with the ‘Grand tack’ model of Solar System formation, where giant planet migration causes the S- and C-type asteroids to be mixed within 1 AU to eventually form the terrestrial planets
Summary
If meteorite alteration mineral D/H ratios are plotted in conjunction with current atmospheric measurements, as well as in situ lithological measurements from the Curiosity rover [94], a picture of atmospheric loss over time is produced (figure 2) These data suggest a linear increase in the atmospheric D/H ratio with time, and an origin of approximately 0‰. Hydrogen implantation from the surrounding atmosphere was reported during these experiments, which would exaggerate the D/H increase under Martian atmospheric conditions This trend of dehydration with a strong D/H increase is visible in chassignite amphibole, with amphibole in the highly shocked chassignite NWA 2737 showing much higher D/H ratios and lower water contents than that in Chassigny (figure 3c [95]). MI glass in the enriched shergottites GRV 020090 and LAR 06319
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