Oxygen Isotopes and the Moon-Forming Giant Impact

Author:

Wiechert U.1,Halliday A. N.1,Lee D.-C.1,Snyder G. A.2,Taylor L. A.2,Rumble D.3

Affiliation:

1. Institute for Isotope Geology and Mineral Resources, Department of Earth Sciences, ETH Zentrum, Sonneggstrasse 5, 8092 Zürich, Switzerland.

2. Planetary Geosciences Institute, Department of Geological Sciences, University of Tennessee, Knoxville, TN 37996–1410, USA.

3. Geophysical Laboratory, Carnegie Institution of Washington, 5251 Broad Branch Road, Washington, DC 20015, USA.

Abstract

We have determined the abundances of 16 O, 17 O, and 18 O in 31 lunar samples from Apollo missions 11, 12, 15, 16, and 17 using a high-precision laser fluorination technique. All oxygen isotope compositions plot within ±0.016 per mil (2 standard deviations) on a single mass-dependent fractionation line that is identical to the terrestrial fractionation line within uncertainties. This observation is consistent with the Giant Impact model, provided that the proto-Earth and the smaller impactor planet (named Theia) formed from an identical mix of components. The similarity between the proto-Earth and Theia is consistent with formation at about the same heliocentric distance. The three oxygen isotopes (Δ 17 O) provide no evidence that isotopic heterogeneity on the Moon was created by lunar impacts.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference26 articles.

1. The origin of the moon and the single impact hypothesis IV

2. Cameron A. G. W., Canup R. M., Lunar Planet Sci XXIX, 1062 (1998);

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

4. A. N. Halliday Earth Planet. Sci. Lett. 176 17 (2000a).

5. Clayton R. N., Mayeda T. K., Proc Lunar Sci Conf XI, 1761 (1975).

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