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Early planetesimal melting from an age of 4.5662 Gyr for differentiated meteorites

Naturevolume 436, pages1127–1131 (2005)Cite this article

Abstract

Long- and short-lived radioactive isotopes and their daughter products in meteorites are chronometers that can test models for Solar System formation1,2. Differentiated meteorites come from parent bodies that were once molten and separated into metal cores and silicate mantles. Mineral ages for these meteorites, however, are typically younger than age constraints for planetesimal differentiation3,4,5. Such young ages indicate that the energy required to melt their parent bodies could not have come from the most likely heat source6—radioactive decay of short-lived nuclides (26Al and60Fe) injected from a nearby supernova—because these would have largely decayed by the time of melting. Here we report an age of 4.5662 ± 0.0001 billion years (based on Pb–Pb dating) for basaltic angrites, which is only 1 Myr younger than the currently accepted minimum age of the Solar System7 and corresponds to a time when26Al and60Fe decay could have triggered planetesimal melting. Small26Mg excesses in bulk angrite samples confirm that26Al decay contributed to the melting of their parent body. These results indicate that the accretion of differentiated planetesimals pre-dated that of undifferentiated planetesimals, and reveals the minimum Solar System age to be 4.5695 ± 0.0002 billion years.

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Figure 1:Pb–Pb age and isotope data for angrites.
Figure 2:Timing of angrite magmatism and parent body (APB) accretion compared with upper age limits for accretion of chondrite parent bodies.

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Acknowledgements

Financial support for this project was provided by the Danish Lithosphere Centre (funded by the Danish National Science Foundation). L. Labenne is thanked for his efforts in finding SAH99555 and providing our angrite samples. C. Stirling provided us with a pre-print of her U isotope study of meteorites. NASA supplied the Martian meteorite EETA79001. V. Fernandes provided us with lunar meteorite NWA032. Y. Amelin is thanked for his feedback on an earlier version of this paper.

Author information

Authors and Affiliations

  1. School of Earth Sciences, Victoria University of Wellington, PO Box 600, Wellington, New Zealand

    Joel Baker

  2. Geological Institute, Øster Voldgade 10, DK-1350, Denmark

    Martin Bizzarro & Nadine Wittig

  3. Geological Museum, Øster Voldgade 5–7, DK-1350, Denmark

    Martin Bizzarro, Nadine Wittig & Henning Haack

  4. Department of Geological Sciences, The University of Texas at Austin, 1 University Station C1100, Texas, 78712-02, Austin, USA

    James Connelly

Authors
  1. Joel Baker
  2. Martin Bizzarro
  3. Nadine Wittig
  4. James Connelly
  5. Henning Haack

Corresponding author

Correspondence toJoel Baker.

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Reprints and permissions information is available atnpg.nature.com/reprintsandpermissions. The authors declare no competing financial interests.

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Supplementary Methods

Description of analytical methods for Pb and Mg isotopic analysis. (DOC 32 kb)

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Baker, J., Bizzarro, M., Wittig, N.et al. Early planetesimal melting from an age of 4.5662 Gyr for differentiated meteorites.Nature436, 1127–1131 (2005). https://doi.org/10.1038/nature03882

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Editorial Summary

Angrites: early arrivals

The latest ultra-precise measurement techniques have been used to obtain lead isotope ages for two examples of a rare type of meteorite, called basaltic angrites. These ‘differentiated’ meteorites are from parent bodies that were once molten and had solidified as a metal core and silicate mantle. Their absolute age is about 4.6 billion years, only a million years younger than the currently accepted minimum age of the Solar System. An excess of magnesium-26 in the angrite samples suggests that aluminium-26 decay triggered melting of the planetesimal that was the parent body.

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