Mathematics – Logic
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p51b1423s&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P51B-1423
Mathematics
Logic
[5499] Planetary Sciences: Solid Surface Planets / General Or Miscellaneous
Scientific paper
The geology and surface mineralogy of Mars is characterised using remote sensing techniques such as thermal emission spectroscopy (TES) from instruments on a number of spacecraft currently orbiting Mars or gathered from roving missions on the Martian surface. However, the study of Martian meteorites is also important in efforts to further understand the geological history of Mars or to interpret mission data as they are believed to be the only available samples that give us direct clues as to Martian igneous processes [1]. We have recently demonstrated that the spectra of Martian-specific minerals can be determined using micro-spectroscopy [2] and that these spectra can be reliably obtained from thin sections of Martian meteorites [3]. Accurate modal mineralogy of these meteorites is also important [4]. In this study we are using a variety of techniques to build upon previous studies of these particular samples in order to fully characterise the nature of the 2 common pyroxenes found in Martian Shergottites; pigeonite and augite [5], [6]. Previous studies have shown that the Shergottite meteorites are dominated by pyroxene (pigeonite and augite in varying quantities) [4], [5], commonly but not always olivine, plagioclase or maskelynite/glass and also hydrous minerals, which separate the Martian meteorites from other achondrites [7]. Our microprobe study of meteorites Zagami, EETA79001, SAU005 and DAG476 in thin-section at the Natural History Museum, London shows a chemical variability within both the pigeonite and augite composition across individual grains in all thin sections; variation within either Mg or Ca concentration varies from core to rim within the grains. This variation can also be seen in modal mineralogy maps using SEM-derived element maps and the Photoshop® technique previously described [4], and in new micro-spectroscopy data, particularly within the Zagami meteorite. New mineral spectra have been gathered from the Shergottite thin-sections by means of FT-IR analyses in efforts to further constrain Martian-specific minerals such as pigeonite in the meteorites, and will be added to the current spectral database. References: [1] McSween, H.Y. Jnr (1994) Meteoritics and Planetary Science 29, 757-779 [2] Benedix G. and Hamilton V. (2007) Abstract #1805 Lunar and Planetary Science Conference XXXVIII [3] Benedix G.K. and Hamilton V.E. (2009) Abstract #5082 Meteoritics and Planetary Science Annual Meeting 44 [4] Stephen, N.R. et al. (2010) Abstract #2367 Lunar and Planetary Science Conference XLI [5] Stolper E. and McSween, H.Y. Jnr (1979) Geochemica et Cosomochimica Acta, 43, 1475-1498 [6] McCoy, T. et al. (1992) Geochemica et Cosomochimica Acta 56, 3571-3582 [7] Mikouchi, T. and Miyamoto, M. (1999) Meteoritics and Planetary Science, 35, 155-159
Benedix Gretchen K.
Bland Phil
Hamilton Victoria E.
Stephen N.
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