The Massalia asteroid family as the origin of ordinary L chondrites

M. Marsset (), P. Vernazza, M. Brož, C. A. Thomas, F. E. DeMeo, B. Burt, R. P. Binzel, V. Reddy, A. McGraw, C. Avdellidou, B. Carry, S. Slivan and D. Polishook
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M. Marsset: European Southern Observatory (ESO)
P. Vernazza: Aix Marseille Université, CNRS, CNES, LAM, Institut Origines
M. Brož: Charles University, Faculty of Mathematics and Physics, Institute of Astronomy
C. A. Thomas: Northern Arizona University
F. E. DeMeo: Massachusetts Institute of Technology
B. Burt: Lowell Observatory
R. P. Binzel: Massachusetts Institute of Technology
V. Reddy: University of Arizona
A. McGraw: University of Arizona
C. Avdellidou: Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange
B. Carry: Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange
S. Slivan: Massachusetts Institute of Technology
D. Polishook: Weizmann Institute of Science

Nature, 2024, vol. 634, issue 8034, 561-565

Abstract: Abstract Studies of micrometeorites in mid-Ordovician limestones and impact craters on Earth indicate that our planet witnessed a massive infall of ordinary L chondrite material about 466 million years ago1–3 that may have been at the origin of an Ordovician ice age and major turnover in biodiversity4. The breakup of a large asteroid in the main belt is the likely cause of this massive infall. Currently, material originating from this breakup still dominates meteorite falls (>20% of all falls)5. Here we provide spectroscopic observations and dynamical evidence that the Massalia collisional family is the only plausible source of this catastrophic event and the most abundant class of meteorites falling on Earth today. This family of asteroids is suitably located in the inner belt, at low-inclination orbits, which corresponds to the observed distribution of L-chondrite-like near-Earth objects and interplanetary dust concentrated at 1.4° (refs. 6,7).

Date: 2024
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DOI: 10.1038/s41586-024-08007-6

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