¹Katsuhito Ohtsuka et al. (>10)
Planetary ans Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2020.104940]
¹Tokyo Meteor Network, 1–27–5 Daisawa, Setagaya-ku, Tokyo, 155–0032, Japan

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¹J.Gattacceca,²L.Bonal,¹C.Sonzogni,¹J.Longerey
Earth and Planetary Science 547, 116467 Link to Article [https://doi.org/10.1016/j.epsl.2020.116467]
¹CNRS, Aix Marseille Univ, IRD, INRAE, CEREGE, Aix-en-Provence, France
²Institut de Planétologie et d’Astrophysique de Grenoble, Université Grenoble Alpes, CNRS CNES, 38000 Grenoble, France
Copyright Elsevier

CV chondrites are one of the most studied group of carbonaceous chondrites. Based on a number of mineralogical features, they have been divided into three sub-groups: CVOxA, CVOxB, and CVRed. These sub-groups are classically interpreted as coming from a single parent body, with a common protolith affected by significant parent body fluid-assisted metasomatism occurring at different temperatures and/or redox conditions. In this work, we studied a set of 53 CV chondrites. We classified them into the three sub-groups, measured their apparent chondrule sizes and their matrix modal abundance. We measured the triple oxygen isotopic composition for 17 of them. The distributions of chondrule size and matrix abundances in CVOxA and CVOxB cannot be statistically distinguished. Conversely, CVRed and CVOx have distinct distributions. These two robust and simple petrographic indicators combined with the previous knowledge of the peak metamorphic temperatures experienced by these meteorites show that CVOx and CVRed originate from two distinct parent bodies. On the other hand, CVOxA and CVOxB likely originate from the same parent body, with CVOxA representing deeper, more metamorphosed levels. For clarification of the chondrite classification scheme, in which one group should ultimately represent a single parent body, we propose to divide the CV group into two proper groups (and not subgroups as in the current scheme), keeping the names CVRed and CVOx. These two groups can be readily separated by estimating the average nickel content of their sulfides.

¹Romain Tartèse,^2,3Mahesh Anand,⁴Jérôme Gattacceca,¹Katherine H. Joy,²James I. Mortimer,¹John F. Pernet-Fisher,³Sara Russell,⁵Joshua F. Snape,⁶Benjamin P. Weiss
Space Science Reviews 215, 54 Link to Article [DOI
https://doi.org/10.1007/s11214-019-0622-x]
¹Department of Earth and Environmental Sciences, The University of Manchester, Manchester, M13 9PL, UK
²Planetary and Space Sciences, School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
³Department of Earth Sciences, The Natural History Museum, Cromwell Road, London, SW7 5BD, UK
⁴CNRS, Aix-Marseille Univ, IRD, Coll France, INRA, CEREGE, Aix-en-Provence, France
⁵Faculty of Sciences, Department of Earth Sciences, Vrije Universiteit, Amsterdam, The Netherlands
⁶Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA

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¹Zita Martins,²Queenie Hoi Shan Chan,³Lydie Bonal,⁴Ashley King,⁵Hikaru Yabuta
Space Science Reviews 216, 54 Link to Article [DOI
https://doi.org/10.1007/s11214-020-00679-6]
¹Centro de Química Estrutural, Departamento de Engenharia Química, Instituto Superior Técnico, Universidade de Lisboa, Avenida Rovisco Pais 1, 1049-001, Lisboa, Portugal
²Planetary and Space Sciences, School of Physical Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
³Institut de Planétologie et d’Astrophysique de Grenoble, Univ. Grenoble Alpes, CNRS, CNES, 38000, Grenoble, France
⁴The Natural History Museum, Cromwell Road, London, SW7 5BD, UK
⁵Department of Earth and Planetary Systems Science, Hiroshima University, 1-3-1 Kagamiyama, Hiroshima, 739-8526, Japan

We currently do not have a copyright agreement with this publisher and cannot display the abstract here