^1,2,3Benjamin E. Cohen,^1,4Darren F. Mark,⁵William S. Cassata,³Lara M. Kalnins,²Martin R. Lee,^2,6Caroline L. Smith,^7,8David L. Shuster
Earth and Planetary Science Letters 621, 118373 Open Access Link to Article [https://doi.org/10.1016/j.epsl.2023.118373]
¹Scottish Universities Environmental Research Centre (SUERC), East Kilbride, UK
²School of Geographical and Earth Sciences, University of Glasgow, UK
³School of GeoSciences, University of Edinburgh, UK
⁴Department of Earth and Environmental Sciences, University of St Andrews, UK
⁵Lawrence Livermore National Laboratory, CA, USA
⁶Department of Earth Sciences, The Natural History Museum, London, UK
⁷Department of Earth and Planetary Science, University of California, Berkeley, CA, USA
⁸Berkeley Geochronology Center, Berkeley, CA, USA
Copyright Elsevier

The shergottites are the most abundant and diverse group of Martian meteorites and provide unique insights into the mafic volcanic and igneous history of Mars. Their ages, however, remain a source of debate. Different radioisotopic chronometers, including 40Ar/39Ar, have yielded discordant ages, leading to conflicting interpretations on whether the shergottites originate from young (mostly <700 Ma) or ancient (>4,000 Ma) Martian volcanoes. To address this issue, we have undertaken an 40Ar/39Ar investigation of seven shergottite meteorites utilizing an innovative approach to correcting data for cosmogenic isotope production and resolution of initial trapped components which, crucially, do not require assumptions concerning the sample’s geologic context. Our data yield statistically robust 40Ar/39Ar isochron ages ranging from 161 ± 9 Ma to 540 ± 63 Ma (2σ), synchronous with the U-Pb, Rb-Sr, and Sm-Nd ages for the respective meteorites. These data indicate that, despite experiencing shock metamorphism, the shergottites were sourced from the youngest volcanoes on Mars.