Origin of water in the terrestrial planets

@article{Drake2005OriginOW,
  title={Origin of water in the terrestrial planets},
  author={Michael J. Drake},
  journal={Meteoritics \& Planetary Science},
  year={2005},
  volume={40}
}
  • M. Drake
  • Published 1 April 2005
  • Physics, Geology
  • Meteoritics & Planetary Science
Abstract— I examine the origin of water in the terrestrial planets. Late‐stage delivery of water from asteroidal and cometary sources appears to be ruled out by isotopic and molecular ratio considerations, unless either comets and asteroids currently sampled spectroscopically and by meteorites are unlike those falling to Earth 4.5 Ga ago, or our measurements are not representative of those bodies. However, the terrestrial planets were bathed in a gas of H, He, and O. The dominant gas phase… 

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References

SHOWING 1-10 OF 61 REFERENCES

Source regions and timescales for the delivery of water to the Earth

Abstract— In the primordial solar system, the most plausible sources of the water accreted by the Earth were in the outer asteroid belt, in the giant planet regions, and in the Kuiper Belt. We

Core Formation in Earth's Moon, Mars, and Vesta

Stimulated by new experimental results on metal/silicate partitioning of elements at elevated temperatures and pressures, we have revisited the question of core formation in Earth's Moon, Mars, and

Determining the composition of the Earth

Material from the Earth, Mars, comets and various meteorites have Mg/Si and Al/Si ratios, oxygen-isotope ratios, osmium-isOTope ratios and D/H, Ar/H2O and Kr/Xe ratios such that no primitive material similar to the Earth's mantle is currently represented in the authors' meteorite collections.

Identification of molecular-cloud material in interplanetary dust particles

It is shown that H and N isotopic anomalies among fragile ‘cluster’ IDPs are far larger, more common, and less equilibrated than those previously observed in other IDPs or meteorites, suggesting that molecular-cloud material has survived intact.

Origin of the Moon in a giant impact near the end of the Earth's formation

This work reports a class of impacts that yield an iron-poor Moon, as well as the current masses and angular momentum of the Earth–Moon system, and suggests that the Moon formed near the very end of Earth's accumulation.

Oxygen Isotopes and the Moon-Forming Giant Impact

The three oxygen isotopes (Δ17O), 16O,17O, and 18O provide no evidence that isotopic heterogeneity on the Moon was created by lunar impacts, and are consistent with the Giant Impact model.

Radial Migration of Phyllosilicates in the Solar Nebula

It has long been recognized that the high temperatures of the inner solar nebula (within approx. 3 AU) would not have allowed water to be incorporated into solids. However, the presence of water on

Water on Mars: Clues from Deuterium/Hydrogen and Water Contents of Hydrous Phases in SNC Meteorites

Inon microprobe studies of hydrous amphibole, biotite, and apatite in SNC meteorites indicate high deuterium/hydrogen (D/H) ratios relative to terrestrial values, providing evidence for a D-enriched martian crustal water reservoir.

Evolution of Oxygen Isotopic Composition in the Inner Solar Nebula

Changes in the chemical and isotopic composition of the solar nebula with time are reflected in the properties of different constituents that are preserved in chondritic meteorites. CR-group
...