Chromium isotopic insights into the origin of chondrite parent bodies and the early terrestrial volatile depletion

1KeZhu朱柯,1Frédéric Moynier,2 Martin Schiller,3ConelM. O’D. Alexander,4Jemma Davidson,4Devin L.Schrader,1,2Elishevah van Kooten,1,2Martin Bizzarro
Geochimica et Cosmochimica Acta (in Press) Link to Article []
1Université de Paris, Institut de Physique du Globe de Paris, CNRS UMR 7154, 1 rue Jussieu, Paris 75005, France
2Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Øster Voldgade 5–7, Copenhagen DK-1350, Denmark
3Earth and Planetary Laboratory, Carnegie Institution for Science, 5241 Broad Branch Road, Washington, DC 20015, USA
4Center for Meteorite Studies, School of Earth and Space Exploration, Arizona State University, 781 East Terrace Road, Tempe, AZ 85287-6004, USA
Copyright Elsevier

Chondrites are meteorites from undifferentiated parent bodies that provide fundamental information about early Solar System evolution and planet formation. The element Cr is highly suitable for deciphering both the timing of formation and the origin of planetary building blocks because it records both radiogenic contributions from 53Mn-53Cr decay and variable nucleosynthetic contributions from the stable 54Cr nuclide. Here, we report high-precision measurements of the mass-independent Cr isotope compositions (ε53Cr and ε54Cr) of chondrites (including all carbonaceous chondrites groups) and terrestrial samples using for the first time a multi-collection inductively-coupled-plasma mass-spectrometer to better understand the formation histories and genetic relationships between chondrite parent bodies. With our comprehensive dataset, the order of decreasing ε54Cr (per ten thousand deviation of the 54Cr/52Cr ratio relative to a terrestrial standard) values amongst the carbonaceous chondrites is updated to CI = CH ≥ CB ≥ CR ≥ CM ≈ CV ≈ CO ≥ CK > EC > OC. Resolvable ε54Cr (with 2SE uncertainty) differences between CV and CK chondrites rule out an origin from a common parent body or reservoir as has previously been suggested. The CM and CO chondrites share common ε54Cr characteristics, which suggests their parent bodies may have accreted their components in similar proportions. The CB and CH chondrites have low-Mn/Cr ratios and similar ε53Cr values to the CI chondrites, invalidating them as anchors for a bulk Mn-Cr isochron for carbonaceous chondrites. Bulk Earth has a ε53Cr value that is lower than any chondrite group, including enstatite chondrites. This depletion may constrain the timing of volatile loss from the Earth or its precursors to be within the first million years of Solar System formation and is incompatible with Earth’s accretion via any of the known chondrite groups as main contributors, including enstatite chondrites.


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