Maria Schönbächler, Mattias Ek, Manuela A Fehr, Katarzyna M Liszewska, Lara A E Meyer, Miriam Rüfenacht, James M J Ball, Paul Frossard, Jan Render, Quinn R Shollenberger, Greg A Brennecka, Thomas S Kruijer, Josh Wimpenny, Martin Bizzarro, Jessica J Barnes, Ann N Nguyen
Analyses of returned samples from asteroids Bennu and Ryugu reveal notable similarities in chemical and isotopic compositions to Ivuna-type (CI) carbonaceous chondrites, prompting reassessment of their origin. We present nucleosynthetic iron (Fe), titanium (Ti), and chromium (Cr) isotope data for Bennu. Minor Cr isotope variations among aliquots likely reflect parent body aqueous alteration, whereas Fe and Ti isotope data are homogeneous and indistinguishable from those of Ryugu and CI chondrites at bulk (>20 milligrams) scale. These results demonstrate that CI-like bodies accreted from a common dust reservoir with affinities to both inner (noncarbonaceous) and outer (carbonaceous) Solar System materials. Combined isotopic, petrographic, and chemical evidence suggests formation near the water ice line inside proto-Jupiter's orbit, where Jupiter's growth restricted the inward drift of larger particles, whereas efficient mixing of fine-grained dust produced bodies with near-solar compositions.