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The dissipation of the solar nebula constrained by impacts and core cooling in planetesimals

Publikation: Bidrag til tidsskrift/Konferencebidrag i tidsskrift /Bidrag til avis › Tidsskriftartikel › Forskning › peer review

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  • Alison C. Hunt, ETH Zürich
    • ,
  • Karen J. Theis, Manchester University
    • ,
  • Mark Rehkämper, Imperial College London
    • ,
  • Gretchen K. Benedix, Curtin University of Technology, Western Australian Museum
    • ,
  • Rasmus Andreasen
  • Maria Schönbächler, ETH Zürich

Rapid cooling of planetesimal cores has been inferred for several iron meteorite parent bodies on the basis of metallographic cooling rates, and linked to the loss of their insulating mantles during impacts. However, the timing of these disruptive events is poorly constrained. Here, we used the short-lived 107Pd–107Ag decay system to date rapid core cooling by determining Pd–Ag ages for iron meteorites. We show that closure times for the iron meteorites equate to cooling in the time frame ~7.8–11.7 Myr after calcium–aluminium-rich inclusion formation, and that they indicate that an energetic inner Solar System persisted at this time. This probably results from the dissipation of gas in the protoplanetary disk, after which the damping effect of gas drag ceases. An early giant planet instability between 5 and 14 Myr after calcium–aluminium-rich inclusion formation could have reinforced this effect. This correlates well with the timing of impacts recorded by the Pd–Ag system for iron meteorites.

OriginalsprogEngelsk
TidsskriftNature Astronomy
Vol/bind6
Nummer7
Sider (fra-til)812-818
Antal sider7
DOI
StatusUdgivet - jul. 2022

Bibliografisk note

Funding Information:
This work was supported by the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007–2013/ERC grant agreement 279779, M.S.). We gratefully acknowledge funding from STFC (ST/F002157/1 and ST/J001260/1, M.R.; ST/J001643/1, M.S.) and funding from the Swiss National Science Foundation (project 200020_179129, M.S.). A.C.H. wishes to thank M. Ek and M. Fehr for laboratory assistance at ETH Zürich during this study. M.S. would like to thank R. Carlson and M. Horan (DTM, Carnegie Institution) for their support and the opportunity to analyse Ag isotopes in May 2006. We also thank C. Smith and D. Cassey (Natural History Museum, London) and J. Hoskin (Smithsonian Institution National Museum of Natural History) for the loan of samples used in this work.

Publisher Copyright:
© 2022, The Author(s), under exclusive licence to Springer Nature Limited.

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