Using Fe and Mg in Olivine as an Indicator of Asteroidal Hydrothermal Alteration

Details Using Fe and Mg in Olivine as an Indicator of Asteroidal Hydrothermal Alteration Using Fe and Mg in Olivine as an Indicator of Asteroidal Hydrothermal Alteration

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9001s&link_type=abstract

American Astronomical Society Meeting 210, #90.01; Bulletin of the American Astronomical Society, Vol. 39, p.203

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Amoeboid Olivine Aggregates (AOAs) found in CO3 meteorites are sensitive indicators of parent body alteration. Because chondritic meteorites are considered to be some of the most primordial material of the early solar system, studying these features reveals information about the hydrothermal alteration undergone after the time of their formation. As water encounters the AOAs, the Mg-rich olivine, forsterite (Mg2SiO4), is replaced with Fe-rich olivine, creating fayalite (Fe2SiO4). The calculation of the Fe/Mg ratio of the, along with a visual examination of the ferroan veins and diffusive halos in these features, allows for a classification of the petrologic subtype (3.0-3.8) of the meteorite. By using a scanning electron microscope for meteorite mapping, feature identification, and element mapping, as well as an electron microprobe for accurate elemental abundance calculation, we were able to accomplish this classification. In this work we present the subtype classification of six previously unclassified meteorites (ALH83108, A-882094, MET00694, MET00711, MET00747, QUE97416, and Y-82094) along with the analysis of two previously studied meteorites as standards (Lance and ALH77003). We found that on the basis of the distribution of the mol% Fe/(Mg+Fe) that Y-82094 is a CO3.3, QUE97416 is a CO3.5, ALH83108, MET00694, MET00711 and MET00747 are CO3.8, and that A-882094 is probably a breccia since the AOAs show different levels of alteration ranging from CO3.4 to CO3.6.

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