Microtextures in the Chelyabinsk impact breccia reveal the history of Phosphorus‐Olivine‐Assemblages in chondrites

1Craig R. Walton,2Ioannis Baziotis,3Ana Černok,4Ludovic Ferrière,5Paul D. Asimow,1,6Oliver Shorttle,3,7Mahesh Anand
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13648]
1Department of Earth Sciences, University of Cambridge, Downing Street, Cambridge, CB2 3EQ UK
2Department of Natural Resources Management and Agricultural Engineering, Agricultural University of Athens, IeraOdos 75, 11855 Athens, Greece
3Department of Physical Sciences, Open University, Walton Hall, Milton Keynes, MK7 6AA UK
4Natural History Museum, Burgring 7, A‐1010 Vienna, Austria
5Division of Geological and Planetary Sciences, California Institute of Technology, 1200 E California Blvd, Pasadena, California, 91125 USA
6Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 OHA UK
7Department of Earth Sciences, The Natural History Museum, London, SW7 5BD UK
Published by arrangement with John Wiley & Sons

The geochemistry and textures of phosphate minerals can provide insights into the geological histories of parental asteroids, but the processes governing their formation and deformation remain poorly constrained. We assessed phosphorus‐bearing minerals in the three lithologies (light, dark, and melt) of the Chelyabinsk (LL5) ordinary chondrite using scanning electron microscope, electron microprobe, cathodoluminescence, and electron backscatter diffraction techniques. The majority of studied phosphate grains appear intergrown with olivine. However, microtextures of phosphates (apatite [Ca5(PO4)3(OH,Cl,F)] and merrillite [Ca9NaMg(PO4)7]) are extremely variable within and between the differently shocked lithologies investigated. We observe continuously strained as well as recrystallized strain‐free merrillite populations. Grains with strain‐free subdomains are present only in the more intensely shocked dark lithology, indicating that phosphate growth predates the development of primary shock‐metamorphic features. Complete melting of portions of the meteorite is recorded by the shock‐melt lithology, which contains a population of phosphorus‐rich olivine grains. The response of phosphorus‐bearing minerals to shock is therefore hugely variable throughout this monomict impact breccia. We propose a paragenetic history for P‐bearing phases in Chelyabinsk involving initial phosphate growth via P‐rich olivine replacement, followed by phosphate deformation during an early impact event. This event was also responsible for the local development of shock melt that lacks phosphate grains and instead contains P‐enriched olivine. We generalize our findings to propose a new classification scheme for Phosphorus‐Olivine‐Assemblages (Type I–III POAs). We highlight how POAs can be used to trace radiogenic metamorphism and shock metamorphic events that together span the entire geological history of chondritic asteroids.


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