Young asteroid families as the primary source of meteorites

M. Brož (), P. Vernazza, M. Marsset, F. E. DeMeo, R. P. Binzel, D. Vokrouhlický and D. Nesvorný
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M. Brož: Institute of Astronomy
P. Vernazza: Institut Origines
M. Marsset: European Southern Observatory (ESO)
F. E. DeMeo: MIT
R. P. Binzel: MIT
D. Vokrouhlický: Institute of Astronomy
D. Nesvorný: Southwest Research Institute

Nature, 2024, vol. 634, issue 8034, 566-571

Abstract: Abstract Understanding the origin of bright shooting stars and their meteorite samples is among the most ancient of astronomy-related questions, which at larger scales has human consequences1–3. As of today, only approximately 6% of meteorite falls have been firmly linked to their sources (Moon, Mars or asteroid (4) Vesta4–6). Here we show that approximately 70% of meteorites originate from three recent break-ups of D > 30 km asteroids that occurred 5.8, 7.6 and less than about 40 Myr ago. These break-ups, including the well-known Karin family7, took place in the prominent yet old Koronis and Massalia families and are at the origin of the dominance of H and L ordinary chondrites among meteorite falls. These young families are distinguished among all main belt asteroids by having a uniquely high abundance of small fragments. Their size–frequency distribution remained steep for a few tens of millions of years, exceeding temporarily the production of metre-sized fragments by the largest old asteroid families (for example, Flora and Vesta). Supporting evidence includes the existence of associated dust bands8–10, the cosmic-ray exposure ages of H-chondrite meteorites11,12 and the distribution of the pre-atmospheric orbits of meteorites13–15.

Date: 2024
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DOI: 10.1038/s41586-024-08006-7

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