The Hf-W Isotopic System and the Origin of the Earth and Moon

Details The Hf-W Isotopic System and the Origin of the Earth and Moon The Hf-W Isotopic System and the Origin of the Earth and Moon

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005areps..33..531j&link_type=abstract

Annual Review of Earth and Planetary Sciences, vol. 33, p.531-570

Computer Science

56

Scientific paper

The Earth has a radiogenic W-isotopic composition compared to chondrites, demonstrating that it formed while 182Hf (half-life 9 Myr) was extant in Earth and decaying to 182W. This implies that Earth underwent early and rapid accretion and core formation, with most of the accumulation occurring in ~10 Myr, and concluding approximately ~30 Myr after the origin of the Solar System. The Hf-W data for lunar samples can be reconciled with a major Moon-forming impact that terminated the terrestrial accretion process ~30 Myr after the origin of the Solar System. The suggestion that the proto-Earth to impactor mass ratio was 7:3 and occurred during accretion is inconsistent with the W isotope data. The W isotope data is satisfactorily modeled with a Mars-sized impactor on proto-Earth (proto-Earth to impactor ratio of 9:1) to form the Moon at ~30 Myr.

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