Terrestrial Chemical Alteration of Hot Desert Meteorites

Details Terrestrial Chemical Alteration of Hot Desert Meteorites Terrestrial Chemical Alteration of Hot Desert Meteorites

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p51a..01c&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #P51A-01

Mathematics

Logic

1065 Trace Elements (3670), 3662 Meteorites, 3670 Minor And Trace Element Composition, 4885 Weathering, 6225 Mars

Scientific paper

Large numbers of meteorites have recently been recovered from terrestrial hot deserts. They include objects whose study holds the promise of significantly increasing our knowledge of the origin and petrogenesis of rare groups of meteorites (e.g., martian and lunar rocks, ureilites, etc). However, these meteorites have typically been exposed to harsh desert conditions for more than 10,000 yr since their fall on earth. A number of alterations have been described, including mineralogical and chemical changes (e.g., Crozaz and Wadhwa, 2001, and references therein). Through weathering, Fe-bearing minerals are progressively altered into clays and iron oxides and hydroxides, which often fill cracks and mineral fractures, together with terrestrial quartz and carbonates. In addition, for whole rock samples, elevated Ba, Sr, and U seem to be the telltale signs of terrestrial contamination (e.g., Barrat et al., 1999). In our work, we use the rare earth elements (REE) as monitors of terrestrial alteration. These elements are important because they are commonly used to decipher the petrogenesis and chronology of meteorites. We have made in-situ concentration measurements, by secondary ion mass spectrometry (SIMS), of individual grains in shergottites (assumed to have formed on Mars), lunar, and angritic meteorites. Terrestrial contamination, in the form of LREE enrichment and Ce anomalies, is encountered in the olivine and pyroxene, the two minerals with the lowest REE concentrations, of all objects analyzed. However, the contamination is highly heterogeneous, affecting some grains and not others of a given phase. Therefore, provided one uses a measurement technique such as SIMS to obtain data on individual grains and to identify the unaltered ones, it is still possible to obtain geochemical information about the origins of hot desert meteorites. On the other hand, great caution must be exercised if one uses data for whole rocks or mineral separates. The U-Pb, Rb-Sr and Sm-Nd systematics are likely to be affected by terrestrial contamination even in samples with a fresh appearance. Leachates are particularly suspicious (Crozaz and Wadhwa, 2001; Dreibus et al., 2001). In the case of shergottites which have proven difficult to date (Nyquist et al., 2001), this is a complicating and especially unfortunate factor. References: Barrat et al. (1999) MAPS 34, 91-97. Crozaz G. and Wadhwa M. (2001) GCA 65, 971-978. Dreibus et al. (2001) MAPS, in press. Nyquist et al. (2001) Space Sci. Rev., in press.

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