THE Hf-W ISOTOPIC SYSTEM AND THE ORIGIN OF THE EARTH AND MOON
Abstract
▪ Abstract The Earth has a radiogenic W-isotopic composition compared to chondrites, demonstrating that it formed while 182 Hf (half-life 9 Myr) was extant in Earth and decaying to 182 W. 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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The formation of Earth commenced no earlier than 10 million years after the formation of the Solar System.
“Thus, the formation of Earth commenced no earlier than 10 million years after the formation of the Solar System (Kleine et al., 2004; Jacobsen, 2005; Touboul et al., 2007).”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Jacobsen, 2005
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60Fe–60Ni chronology of core formation in Mars
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Early magnetic field and magmatic activity on Mars from magma ocean cumulate overturn
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Magma Oceans and Primordial Mantle Differentiation
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Lu–Hf zircon evidence for rapid lunar differentiation
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Comparative Climatology of Terrestrial Planets
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Terrestrial planet formation constrained by Mars and the structure of the asteroid belt
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Shock Events in the Solar System: The Message from Minerals in Terrestrial Planets and Asteroids
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Chemical fingerprints of formation in rocky super-Earths’ data
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High precision tungsten isotope measurement by thermal ionization mass spectrometry
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Self-citationA tale of planet formation: from dust to planets
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Tungsten isotopic evolution during late-stage accretion: Constraints on Earth–Moon equilibration
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Nebular atmosphere to magma ocean: A model for volatile capture during Earth accretion
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Core Formation and Mantle Differentiation on Mars
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Fast accretion of the Earth with a late Moon-forming giant impact
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Chronometry of Meteorites and the Formation of the Earth and Moon
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The Earth’s missing lead may not be in the core
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Dating the First Stage of Planet Formation
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Magma Ocean, Water, and the Early Atmosphere of Venus
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Did the terrestrial planets of the solar system form by pebble accretion?
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- Authors
- Jacobsen, S. B.
- Affiliations
- Harvard University (US)
- Corresponding author
- Jacobsen, Stein B.
- ORCID
- Jacobsen, Stein B.
- Venue
- Annual Review of Earth and Planetary Sciences
- Publisher
- Annual Reviews
- Published
- 2005-05-31
- Volume
- 33
- Issue
- 1
- Pages
- 531-570
- ISSN
- 0084-6597 (ISSN-L)
- 1545-4495
- OpenAlex
- W2133510984
- Cited by
- 234
- References
- 81
- Citations by year
- 2026: 5 · 2025: 7 · 2024: 14 · 2023: 9 · 2022: 4 · 2021: 11 · 2020: 12 · 2019: 7 · 2018: 9 · 2017: 5 · 2016: 7 · 2015: 14 · 2014: 15 · 2013: 14 · 2012: 10
- FWCI
- 2.00
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Annual Review of Earth and Planetary Sciences (publishedVersion)
- Funders
- National Aeronautics and Space Administration
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Earth and Planetary Sciences › Geophysics › Geological and Geochemical Analysis
- Physical Sciences › Earth and Planetary Sciences › Paleontology › Paleontology and Stratigraphy of Fossils
- Keywords
- tungsten isotopes, Hf isotopes, Earth formation, Moon formation, giant impact hypothesis, core formation, radiogenic isotopes, chondrites, Moon-forming impact
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