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Journal Article

Petrogenesis of Erg Chech 002 Achondrite and Implications for an Altered Magma Ocean

Authors

Jin,  Ziliang
External Organizations;
GFZ SIMS Publications, Deutsches GeoForschungsZentrum;

Zhang,  Yishen
External Organizations;
GFZ SIMS Publications, Deutsches GeoForschungsZentrum;

Bose,  Maitrayee
External Organizations;
GFZ SIMS Publications, Deutsches GeoForschungsZentrum;

/persons/resource/sglynn

Glynn,  S.
0 Pre-GFZ, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum;
GFZ SIMS Publications, Deutsches GeoForschungsZentrum;

/persons/resource/couffig

Couffignal,  F.
3.1 Inorganic and Isotope Geochemistry, 3.0 Geochemistry, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum;
GFZ SIMS Publications, Deutsches GeoForschungsZentrum;

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5025460.pdf
(Publisher version), 2MB

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Citation

Jin, Z., Zhang, Y., Bose, M., Glynn, S., Couffignal, F. (2024): Petrogenesis of Erg Chech 002 Achondrite and Implications for an Altered Magma Ocean. - The Astrophysical Journal, 965, 1, 24.
https://doi.org/10.3847/1538-4357/ad2ea7


Cite as: https://gfzpublic.gfz-potsdam.de/pubman/item/item_5025460
Abstract
This study conducts mineralogical and chemical investigations on the oldest achondrite, Erg Chech 002 (∼4565 million yr old). This meteorite exhibits a disequilibrium igneous texture characterized by high-Mg-number (atomic Mg/(Mg + Fe2+)) orthopyroxene xenocrysts (Mg number = 60–80) embedded in an andesitic groundmass. Our research reveals that these xenocrysts were early formed crystals, loosely accumulated or scattered in the short-period magma ocean on the parent body. Subsequently, these crystals underwent agitation due to the influx of external materials. The assimilation of these materials enriched the 16O component of the magma ocean and induced a relatively reduced state. Furthermore, this process significantly cooled the magma ocean and inhibited the evaporation of alkali elements, leading to elevated concentrations of Na and K within the meteorite. Our findings suggest that the introduced materials are probably sourced from the reservoirs of CR clan meteorites, indicating extensive transport and mixing of materials within the early solar system.