Timing of thermal metamorphism in CM chondrites: Implications for Ryugu and Bennu future sample return

1Elsa Amsellem,1,2Frédéric Moynier,1,3Brandon Mahan,2,4Pierre Beck
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2019.113593]
1Université de Paris, Institut de physique du globe de Paris, CNRS, F-75005 Paris, France
2Institut Universitaire de France, Paris, France
3Department of Earth and Planetary Sciences, Macquarie University, Sydney, New South Wales 2109, Australia
4Institut de Planétologie et d’Astrophysique de Grenoble, Univ. Grenoble Alpes, CNRS, CNES, 38000 Grenoble, France
Copyright Elsevier

Carbonaceous chondrites are often considered potential contributors of water and other volatiles to terrestrial planets as most of them contain significant amounts of hydrous mineral phases. As such, carbonaceous chondrites are candidate building blocks for Earth, and elucidating their thermal histories is of direct importance for understanding the volatile element history of Earth and the terrestrial planets. A significant fraction of CM type carbonaceous chondrites are thermally metamorphosed or “heated” and have lost part of their water content. The origin and the timing of such heating events are still debated, as they could have occurred either in the first Myrs of the Solar System via short-lived radioactive heating, or later by impact induced heating and/or solar radiation. Since Rb is more volatile than Sr, and some heated CM chondrites are highly depleted in Rb, a dating system based on the radioactive decay of 87Rb to 87Sr (λ87Rb = 1.393 × 10−11 yr−1) could be used to date the heating event relating to the fractionation of Rb and Sr. Here, we have leveraged the 87Rb/87Sr system to date the heating of five CM chondrites (PCA 02012, PCA 02010, PCA 91008, QUE 93005 and MIL 07675). We find that the heating events of all five meteorites occurred at least 3 Ga after the formation of the Solar System. Such timing excludes short-lived radioactive heating as the origin of thermal metamorphism in these meteorites, and relates such heating events to ages of collisional families of C-type asteroids.


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