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This study analyzed highly siderophile element (HSE) and Os isotope data in lunar mare basalts. Results indicate a homogeneous lunar interior with low HSE abundances, consistent with late accretion before crust formation.

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Area of Science:

  • Geochemistry
  • Isotope Geochemistry
  • Planetary Science

Background:

  • Lunar mare basalts provide insights into the Moon's mantle composition and evolution.
  • Highly siderophile elements (HSEs) are crucial tracers of planetary formation and differentiation processes.
  • Osmium (Os) isotopes offer a sensitive tool for tracking mantle evolution and accretion history.

Purpose of the Study:

  • To determine the abundance and isotopic composition of HSEs in various lunar mare basalts.
  • To constrain the origin and evolution of the lunar mantle.
  • To investigate the nature and timing of late accretion on the Moon.

Main Methods:

  • Analysis of coupled 187Os/188Os and HSE abundance data.
  • Samples include Apollo mare basalts (12, 15, 17) and lunar meteorites (LAP 04841, MIL 05035).
  • Modeling of partial melting and fractional crystallization processes.

Main Results:

  • Most magnesian samples show chondrite-relative HSE abundances and chondritic initial 187Os/188Os.
  • Mare basalts exhibit consistently low HSE abundances (~2x10^-5 to 2x10^-7 chondritic abundance).
  • Apollo 12 basalts yield a Re-Os age of 3.0 ±0.6 Ga with an initial 187Os/188Os of 0.109 ±0.008.

Conclusions:

  • Lunar mare basalt compositions suggest partial melting of metal-free sources with low HSE concentrations.
  • Homogeneous HSE abundances across different lunar sites indicate a well-mixed lunar interior.
  • Low HSE abundances and chondritic Re/Os ratios support ~0.02% late accretion prior to lunar crust formation.