Microstructural Investigations of the Cosmochemical Histories of Presolar Grains

Details Microstructural Investigations of the Cosmochemical Histories of Presolar Grains Microstructural Investigations of the Cosmochemical Histories of Presolar Grains

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..341..645s&link_type=abstract

Chondrites and the Protoplanetary Disk, ASP Conference Series, Vol. 341, Proceedings of a workshop held 8-11 November 2004 in Ka

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Presolar grains are the remnants of the dusty materials from which our solar system formed. These grains, which escaped heavy processing in the early solar nebula and retain isotopic signatures of presolar stellar origins, are trace constituents of meteorites and interplanetary dust particles. The compositions and microstructures of the grains are a record of circumstellar dust condensation processes, overprinted with a record of processing events that occurred in the interstellar medium, solar nebula, meteorite parent body or host interplanetary dust particle, and laboratory. Possible alteration processes include: radiation damage, heating, shock, oxidation, aqueous alteration, and acid etching. The probability of a given grain retaining a signature of one or more processing events depends on the properties of the phase. Among the known presolar phases, silicates are the most readily altered, and diamond and Al2O3 the least. Recent advances in laboratory instrumentation permit the analysis of distinct processing signatures in individual presolar grains, in order to complement astrophysical observations and theoretical models of cosmic dust processing.

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