¹Ségolène Rabin, ¹Steven Goderis, ¹Lisa Krämer-Ruggiu, ¹Pim Kaskes, ²Jan Smit, ³Kasper Hobin, ³Frank Vanhaecke, ^1,4Philippe Claeys
Earth and Planetary Science Letters 674, 119721 Link to Article [https://doi.org/10.1016/j.epsl.2025.119721]
¹Archaeology, Environmental Changes, and Geo-Chemistry, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium
²Geology and Geochemsitry, Vrije Universiteit Amsterdam, de Boelelaan 1085, 1081HV Amsterdam, Netherlands
³Atomic & Mass Spectrometry – A&MS research unit, Ghent University, Department of Chemistry, Campus Sterre, Krijgslaan 281 – S12, 9000 Gent, Belgium
⁴Earth, Ocean and Atmospheric Sciences, University of British Columbia, Vancouver, V6T1Z4 BC, Canada
Copyright Elsevier

Stable Fe isotopic variations recorded in impact spherules provide insights in the evolution of the impact plume generated by a hypervelocity impact. This study reports the first high-precision Fe isotope ratio of both proximal and distal impact spherules, originating from the Chicxulub impact. A total of 47 impact spherules, formed as the result of melting and condensation, are investigated from different localities at different distances and directions from the source crater. The major challenge of studying 66 million years old impact spherules lies in the extensive alteration and diagenesis processes that could affect their original Fe signatures. Proximal and distal impact spherules show a comparable mean δ56Fe value of -0.036 ± 0.28 ‰ (n = 40). This Fe isotope signature, identical to the mean value for the Earth crust, shows that Fe did not significantly fractionate in the plume generated by the Chicxulub impact event. Only a few impact spherules display light isotopic composition, with δ56Fe values down to -3.01 ± 0.07 ‰, due to their high degree of alteration. The lack of Fe fractionation in the Chicxulub impact spherules likely reflects the thermal conditions within the impact generated plume. The rate of temperature change in the Chicxulub impact plume is assumed to be slower than the evaporation and condensation timescales (seconds-minutes), allowing the temperature to remain above 1300 K for a sufficient period to enable re-equilibration of the Fe isotopic system.

¹Yingnan Zhang, ¹Mi Zhou, ¹Liping Qin, ¹Bing Yang, ¹Haolan Tang, ²Thomas Smith, ²Huaiyu He
Earth and Planetary Science Letters 674, 119738 Link to Article [https://doi.org/10.1016/j.epsl.2025.119738]
¹National Key Laboratory of Deep Space Exploration/State Key Laboratory of Lithospheric and Environmental Coevolution, University of Science and Technology of China, Hefei 230026, China
²State Key Laboratory of Lithospheric and Environmental Coevolution, Institute of Geology and Geophysics, Chinese Academy of Sciences, 19 Beitucheng Western Road, Box 9825, Beijing 100029, China
Copyright Elsevier

The fingerprints of ancient stars are preserved in the isotopic anomalies of meteorites, revealing how the Solar System’s building blocks formed and evolved. Potassium, a moderately volatile element, exhibits isotopic anomalies that can serve as tracers of volatile inventories in meteorites and terrestrial planets. We measured the K isotopic compositions in a range of meteorites. After correcting for cosmic-ray effects, all meteorites show ε40K values that are the same as or slightly higher than Earth’s. The lack of correlation with other neutron-rich isotopes, but a clear link to 30Si and 43Ca, points to stellar burning as the main source of 40K. Large 40K enrichments in CI chondrites and Tagish Lake indicate the addition of 40K-rich material, while other subgroups of carbonaceous chondrites show evidence of various degrees of mixing with this component. These patterns suggest inward migration of CI-like volatile-rich carriers in the protoplanetary disk. The uniform enrichment in meteorites implies that Earth’s slightly lower ε40K required a missing, 40K-depleted building block, likely from early-formed planetesimals that had avoided this late addition of CI-like material.