Abstract

The formation of a primordial crust is a critical step in the evolution of terrestrial planets but the timing of this process is poorly understood. The mineral zircon is a powerful tool for constraining crust formation because it can be accurately dated with the uranium-to-lead (U–Pb) isotopic decay system and is resistant to subsequent alteration. Moreover, given the high concentration of hafnium in zircon, the lutetium-to-hafnium (176Lu–176Hf) isotopic decay system can be used to determine the nature and formation timescale of its source reservoir1,2,3. Ancient igneous zircons with crystallization ages of around 4,430 million years (Myr) have been reported in Martian meteorites that are believed to represent regolith breccias from the southern highlands of Mars4,5. These zircons are present in evolved lithologies interpreted to reflect re-melted primary Martian crust4, thereby potentially providing insight into early crustal evolution on Mars. Here, we report concomitant high-precision U–Pb ages and Hf-isotope compositions of ancient zircons from the NWA 7034 Martian regolith breccia. Seven zircons with mostly concordant U–Pb ages define 207Pb/206Pb dates ranging from 4,476.3 ± 0.9 Myr ago to 4,429.7 ± 1.0 Myr ago, including the oldest directly dated material from Mars. All zircons record unradiogenic initial Hf-isotope compositions inherited from an enriched, andesitic-like crust extracted from a primitive mantle no later than 4,547 Myr ago. Thus, a primordial crust existed on Mars by this time and survived for around 100 Myr before it was reworked, possibly by impacts4,5, to produce magmas from which the zircons crystallized. Given that formation of a stable primordial crust is the end product of planetary differentiation, our data require that the accretion, core formation and magma ocean crystallization on Mars were completed less than 20 Myr after the formation of the Solar System. These timescales support models that suggest extremely rapid magma ocean crystallization leading to a gravitationally unstable stratified mantle, which subsequently overturns, resulting in decompression melting of rising cumulates and production of a primordial basaltic to andesitic crust6,7.

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Acknowledgements

Financial support for this project was provided by the Danish National Research Foundation (DNRF97) and the European Research Council (ERC Consolidator Grant Agreement 616027, STARDUST2ASTEROIDS) to M.B. We thank J. Frydenvang and K. Kinch for discussions.

Reviewer information

Nature thanks A. Brandon and L. Elkins-Tanton for their contribution to the peer review of this work.

Author information

Author notes

  1. These authors contributed equally: Laura C. Bouvier, Maria M. Costa.

Affiliations

  1. Centre for Star and Planet Formation and Natural History Museum of Denmark, University of Copenhagen, Copenhagen, Denmark

    • Laura C. Bouvier
    • , Maria M. Costa
    • , James N. Connelly
    • , Ninna K. Jensen
    •  & Martin Bizzarro
  2. Quadlab and Natural History Museum of Denmark, University of Copenhagen, Copenhagen, Denmark

    • Daniel Wielandt
    •  & Michael Storey
  3. Department of Applied Geology, Curtin University, Perth, Western Australia, Australia

    • Alexander A. Nemchin
  4. Swedish Museum of Natural History, Stockholm, Sweden

    • Martin J. Whitehouse
    • , Joshua F. Snape
    •  & Jeremy J. Bellucci
  5. Institut de Physique du Globe de Paris, Université Paris Diderot, Sorbonne Paris Cité, Paris, France

    • Frédéric Moynier
  6. Laboratoire Géosciences Océan (UMR CNRS 6538), Université de Bretagne Occidentale et Institut Universitaire Européen de la Mer, Plouzané, France

    • Arnaud Agranier
    •  & Bleuenn Gueguen
  7. Institute of Geochemistry and Petrology, ETH, Zurich, Switzerland

    • Maria Schönbächler

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Contributions

M.B. designed and led the research project. M.M.C. and J.N.C. identified and separated the zircons and performed analytical work related to the U–Pb isotope systematics of the zircons. L.C.B., J.N.C. and M.B. performed analytical work related to the 176Lu–176Hf systematics of the zircons. N.K.J., D.W., M.S., M.J.W., J.F.S., J.J.B., A.A.N., F.M., A.A. and B.G. assisted in sample preparation and zircon identification. All authors participated in the interpretation of the data. The manuscript was written by L.C.B., M.M.C., J.N.C. and M.B.

Competing interests

The authors declare no competing interests.

Corresponding author

Correspondence to Martin Bizzarro.

Extended data figures and tables

  1. Extended Data Fig. 1 Photomicrographs of the NWA 7034 zircons analysed in this study taken under natural light.

    Given the small size and limited number of zircons recovered from the crushing process, we considered it to be preferable not to conduct additional imaging (using cathodoluminescence) because this necessitates extra manipulation of the individual grains, thereby increasing the risk of losing zircons. The fact that the zircons have mostly concordant U–Pb ages confirms their simple igneous history and, therefore, additional imaging to investigate potential zoning is not required here.

Supplementary information

  1. Supplementary Table 1

    U-Pb isotope data for NWA 7034 zircons.

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https://doi.org/10.1038/s41586-018-0222-z

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