Letter

A Martian origin for the Mars Trojan asteroids

  • Nature Astronomy 1, Article number: 0179 (2017)
  • doi:10.1038/s41550-017-0179
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Abstract

Seven of the nine known Mars Trojan asteroids belong to an orbital cluster1,2 named after its largest member, (5261) Eureka. Eureka is probably the progenitor of the whole cluster, which formed at least 1 Gyr ago3. It has been suggested3 that the thermal YORP (Yarkovsky–O'Keefe–Radzievskii–Paddack) effect spun up Eureka, resulting in fragments being ejected by the rotational-fission mechanism. Eureka’s spectrum exhibits a broad and deep absorption band around 1 μm, indicating an olivine-rich composition4. Here we show evidence that the Trojan Eureka cluster progenitor could have originated as impact debris excavated from the Martian mantle. We present new near-infrared observations of two Trojans ((311999) 2007 NS2 and (385250) 2001 DH47) and find that both exhibit an olivine-rich reflectance spectrum similar to Eureka’s. These measurements confirm that the progenitor of the cluster has an achondritic composition4. Olivine-rich reflectance spectra are rare amongst asteroids5 but are seen around the largest basins on Mars6. They are also consistent with some Martian meteorites (for example, Chassigny7) and with the material comprising much of the Martian mantle8,9. Using numerical simulations, we show that the Mars Trojans are more likely to be impact ejecta from Mars than captured olivine-rich asteroids transported from the main belt. This result directly links specific asteroids to debris from the forming planets.

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Acknowledgements

We thank F. DeMeo and B. Burt for their help with spectral analysis of olivine asteroids, and J. Mustard for providing CRISM reflectance spectra of Mars. D.P. is grateful to the Ministry of Science, Technology and Space of the Israeli government for their Ramon fellowship for post-docs. S.A.J. and A.M. were supported by the European Research Council Advanced Grant ‘ACCRETE’ (contract number 290568). O.A. acknowledges support from the Helen Kimmel Center for Planetary Science, the Minerva Center for Life Under Extreme Planetary Conditions and the I-CORE Program of the Planning and Budgeting Committee of the Council for Higher Education and the Israeli Science Foundation (Center No. 1829/12). Observations for this study were performed in Hawaii. We are most fortunate to have had the opportunity to conduct observations from the Mauna Kea Observatory, and we thank the NASA Infrared Telescope Facility staff for their continuous help.

Author information

Affiliations

  1. Department of Earth and Planetary Sciences, Weizmann Institute of Science, Rehovot 7610001, Israel.

    • D. Polishook
    •  & O. Aharonson
  2. Bayerisches Geoinstitut, Universtat Bayreuth, 95440 Bayreuth, Germany.

    • S. A. Jacobson
  3. Laboratoire Lagrange, Observatoire de la Cote d'Azur, 06304 Nice, France.

    • S. A. Jacobson
    •  & A. Morbidelli

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Contributions

D.P. and S.A.J. led the project and wrote the manuscript. D.P. ran the observations, reduction and analysis of the spectral data. S.A.J. wrote the dynamical simulations and analysed their results. All authors participated in the interpretation of the results.

Competing interests

The authors declare no competing financial interests.

Corresponding author

Correspondence to D. Polishook.

Supplementary information

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  1. 1.

    Supplementary Information

    Supplementary Table 1 and Supplementary References