Planetary bodies acquire their primary compositions from that of their smaller, precursor planetesimals.  While much is hypothesized about how these planetesimals evolved both physically and chemically in the early solar system, there are wide gaps in our understanding of how their compositions were modified, and ultimately set, prior to incorporation into the final planetary body.  Meteorites provide invaluable information about primary processes such as accretion, melting and crystallization and secondary processes such as shock modification and metasomatism.   The Eucrite meteorites, part of the larger HED group assumed to have originated on asteroid 4Vesta, record evidence of one such secondary, metasomatic event.<br/>Eucrites are basaltic rocks, consisting primarily of pyroxene and plagioclase with minor silica/sulfides and are sub-divided into three groups based on their geochemistry.  Unequilibrated eucrites preserve evidence of a metasomatic event in which pyroxene is observed to breakdown into silica and troilite.  Pyroxene, however, does not contain meaningful amounts of sulfur to form even trace amounts of Troilite.  In this work, we present a series of exploratory experiments to understand the interactions of sulfur and pyroxene at conditions appropriate for late-stage metasomatism on the eucrite parent body.  Constraints on the reaction, to include phases and compositions required as well as boundary conditions such temperature, will be presented along with implications for the compositions of planetary bodies assembled from planetesimals experiencing metasomatism.<br/>

Late-stage sulfur driven metasomatism: Pyroxene to troilite on planetesimals in the early solar system

Macromolecular Chemistry: The Second Century

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ACS Spring 2020 National Meeting & Expo

The official archive and repository for all ACS Meetings & Expositions abstracts and select posters or presentations.