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Isotopes01:12

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Elements have a set number of protons that determines their atomic number (Z). For example, all atoms with eight protons are oxygen; however, the number of neutrons can vary for atoms of the same element. The sum of the number of protons and the number of neutrons is the mass number (A). Atoms with the same atomic number but different mass numbers are called isotopes. Elements can have multiple isotopes, for example, carbon-12, carbon-13, and carbon-14.
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Tungsten Isotopes in Planets.

Thorsten Kleine1, Richard J Walker2

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Summary
This summary is machine-generated.

The Hf-W isotope system reveals early Solar System processes. Planetary accretion and differentiation occurred rapidly, within millions of years after the Solar System

Keywords:
core formationhafnium-tungsten isotopeslate accretionmodel ages

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Area of Science:

  • Cosmochemistry and Geochemistry
  • Isotope Geochemistry
  • Planetary Science

Background:

  • The Hafnium-Tungsten (Hf-W) isotope system is a valuable tool for studying early Solar System history.
  • Tungsten (W) is siderophile, while Hafnium (Hf) is lithophile, making the Hf-W system ideal for dating planetary accretion and differentiation.
  • Short-lived isotopes like Aluminum-26 (26Al) played a significant role in fueling early planetary melting and differentiation.

Purpose of the Study:

  • To utilize the Hf-W isotope system as a chronometer for planetary formation processes.
  • To constrain the timescales of accretion and core formation for various Solar System bodies, including Earth and Mars.
  • To investigate the implications of W isotopic compositions for models of lunar formation and early Earth history.

Main Methods:

  • Analysis of Tungsten (W) isotopic compositions in meteorite samples.
  • Application of the Hf-W isotope chronometer to date geological events.
  • Comparison of isotopic data with existing models of planetary formation and differentiation.

Main Results:

  • Meteorite data indicate that some differentiated bodies accreted within 1 million years of Solar System formation.
  • Planetary melting and differentiation, powered by 26Al decay, occurred within 1-3 million years for these bodies.
  • Timescales for accretion and core formation increase with planetary mass: ~10 million years for Mars and >34 million years for Earth.
  • Nearly identical 182W compositions in the lunar and terrestrial mantles challenge current lunar formation models.
  • Terrestrial samples older than 4 billion years show minimal 182W variations, preserving evidence of Earth's earliest history.

Conclusions:

  • The Hf-W isotope system provides crucial insights into the rapid early evolution of the Solar System.
  • The study refines timescales for planetary accretion and differentiation, highlighting the role of short-lived radionuclides.
  • Discrepancies in W isotopes between Earth and the Moon necessitate revisions to lunar formation theories, while early Earth's isotopic record remains remarkably preserved.