The origin of volatile elements in the Earth–Moon system

• Published in: Proceedings of the National Academy of Sciences - PNAS Vol. 119; no. 8; pp. 1 - 5
• Main Authors: Borg, Lars E., Brennecka, Gregory A., Kruijer, Thomas S.
• Format: Journal Article
• Language: English
• Published: United States National Academy of Sciences 22.02.2022; Proceedings of the National Academy of Sciences
• Subjects: Crystallization; Depletion; Earth; GEOSCIENCES; Inner solar system; Lunar rocks; Moon; Physical Sciences; Planetary evolution; Solar system; Strontium 87; Giant Impact; Moon; Moon-forming impact; volatile elements
• ISSN: 0027-8424; 1091-6490; 1091-6490
• DOI: 10.1073/pnas.2115726119

The origin of volatile species such as water in the Earth–Moon system is a subject of intense debate but is obfuscated by the potential for volatile loss during the Giant Impact that resulted in the formation of these bodies. One way to address these topics and place constraints on the temporal evolution of volatile components in planetary bodies is by using the observed decay of 87Rb to 87Sr because Rb is a moderately volatile element, whereas Sr is much more refractory. Here, we show that lunar highland rocks that crystallized ∼4.35 billion years ago exhibit very limited ingrowth of 87Sr, indicating that prior to the Moon-forming impact, the impactor commonly referred to as “Theia” and the proto-Earth both must have already been strongly depleted in volatile elements relative to primitive meteorites. These results imply that 1) the volatile element depletion of the Moon did not arise from the Giant Impact, 2) volatile element distributions on the Moon and Earth were principally inherited from their precursors, 3) both Theia and the proto-Earth probably formed in the inner solar system, and 4) the Giant Impact occurred relatively late in solar system history.