Early Moon formation inferred from hafnium–tungsten systematics

  title={Early Moon formation inferred from hafnium–tungsten systematics},
  author={Maxwell M. Thiemens and Peter Sprung and Ra{\'u}l O. C. Fonseca and Felipe Padilha Leitzke and Carsten M{\"u}nker},
  journal={Nature Geoscience},
The date of the Moon-forming impact places an important constraint on Earth’s origin. Lunar age estimates range from about 30 Myr to 200 Myr after Solar System formation. Central to this age debate is the greater abundance of 182W inferred for the silicate Moon than for the bulk silicate Earth. This compositional difference has been explained as a vestige of less late accretion to the Moon than to the Earth after core formation. Here we present high-precision trace element composition data from… 

Isotopic evidence for the formation of the Moon in a canonical giant impact

It is shown that the vanadium isotopic composition of the Moon is offset from that of the bulk silicate Earth by 0.04 parts per thousand towards the chondritic value, which implies that the impactor and proto-Earth mainly accreted from a common isotopic reservoir in the inner solar system.

Evidence for Transient Atmospheres during Eruptive Outgassing on the Moon

Events following the giant impact formation of the Moon are thought to have led to volatile depletion and concurrent mass-dependent fractionation of the isotopes of moderately volatile elements

Geochemical Constraints on the Origin of the Moon and Preservation of Ancient Terrestrial Heterogeneities

The Moon forming giant impact marks the end of the main stage of Earth’s accretion and sets the stage for the subsequent evolution of our planet. The giant impact theory has been the accepted model

Common feedstocks of late accretion for the terrestrial planets

Abundances of the highly siderophile elements (HSEs) in silicate portions of Earth and the Moon provide constraints on the impact flux to both bodies, but only since ~100 Myr after the beginning of

Formation of Venus, Earth and Mars: Constrained by Isotopes

Here we discuss the current state of knowledge of terrestrial planet formation from the aspects of different planet formation models and isotopic data from Hf-W, U-Pb, lithophile-siderophile

A Review of the Lunar 182Hf-182W Isotope System Research

In recent years, the extinct nuclide 182Hf-182W system has been developed as an essential tool to date and trace the lunar origin and evolution. Despite a series of achievements, controversies and



Tungsten isotopic evidence for disproportional late accretion to the Earth and Moon

Characterization of the hafnium–tungsten systematics of the lunar mantle will enable better constraints on the timescale and processes involved in the currently accepted giant-impact theory for the formation and evolution of the Moon, and for testing the late-accretion hypothesis.

Early formation of the Moon 4.51 billion years ago

Data on lunar zircons indicate differentiation of the lunar crust by 4.51 billion years, indicating the formation of the Moon within the first ~60 million years after the birth of the solar system.

Lunar tungsten isotopic evidence for the late veneer

Data independently show that HSE abundances in the bulk silicate Earth were established after the giant impact and core formation, as predicted by the late veneer hypothesis and constitutes a challenge to current models of lunar origin.

Highly siderophile elements in Earth’s mantle as a clock for the Moon-forming impact

A large number of N-body simulations are used to demonstrate a relationship between the time of the last giant impact on an Earth-like planet and the amount of mass subsequently added during the era known as Late Accretion, and the concentration of highly siderophile elements in Earth’s mantle constrains the mass of chondritic material added to Earth during LateAccretion.

Geochemical arguments for an Earth-like Moon-forming impactor

An inversion method is presented to calculate the Hf/W ratios and ϵ182W values of the proto-Earth and impactor mantles for a given Moon-forming impact scenario.

The tungsten isotopic composition of the Earth’s mantle before the terminal bombardment

It is speculated that the decrease in mantle 182W/184W occurs during the Archean eon (about four to three billion years ago), potentially on the same timescale as a notable decrease in 142Nd/144Nd (refs 3 and 6).