Magnesium isotope evidence that accretional vapour loss shapes planetary compositions

Remco C. Hin*, Christopher D. Coath, Philip J. Carter, Francis Nimmo, Yi-Jen Lai, Philip A. E. Pogge von Strandmann, Matthias Willbold, Zoë M. Leinhardt, Michael J. Walter, Tim Elliott

*Corresponding author for this work

Research output: Contribution to journalLetterpeer-review

137 Citations (Scopus)


It has long been recognized that Earth and other differentiated planetary bodies are chemically fractionated compared to primitive, chondritic meteorites and, by inference, the primordial disk from which they formed. However, it is not known whether the notable volatile depletions of planetary bodies are a consequence of accretion(1) or inherited from prior nebular fractionation(2). The isotopic compositions of the main constituents of planetary bodies can contribute to this debate(3-6). Here we develop an analytical approach that corrects a major cause of measurement inaccuracy inherent in conventional methods, and show that all differentiated bodies have isotopically heavier magnesium compositions than chondritic meteorites. We argue that possible magnesium isotope fractionation during condensation of the solar nebula, core formation and silicate differentiation cannot explain these observations. However, isotopic fractionation between liquid and vapour, followed by vapour escape during accretionary growth of planetesimals, generates appropriate residual compositions. Our modelling implies that the isotopic compositions of magnesium, silicon and iron, and the relative abundances of the major elements of Earth and other planetary bodies, are a natural consequence of substantial (about 40 per cent by mass) vapour loss from growing planetesimals by this mechanism.

Original languageEnglish
Pages (from-to)511-515
Number of pages17
Publication statusPublished - 28 Sept 2017
Externally publishedYes


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