Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p43a1386p&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #P43A-1386
Physics
5464 Remote Sensing, 5470 Surface Materials And Properties, 6225 Mars
Scientific paper
The spatial distributions, abundances, and grain sizes of mineral phases on Mars have important petrogenetic implications for the Martian crust. One of the major science objectives of OMEGA (Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité) is to map the mineralogy of the Martian surface, in order to improve understanding of the composition of the crust and the volcanic deposits of Mars. The first global analysis of reflectance OMEGA spectra showed that low albedo regions could generally be grouped into different classes (Poulet et al., JGR 112, 2007): distinct mafic, rock-forming minerals low-calcium pyroxene (LCP), and high-calcium pyroxene (HCP) are identified in equatorial and southern low albedo regions; the regions exhibiting the strongest LCP signatures are found mainly in the ancient Noachian-aged units; olivine with high iron content and/or large grain size (>100 microns) is only detected in isolated areas, olivine (Mg- rich composition) is detected in extensive regions of the pyroxene-rich zones; extended dark regions in the northern plains exhibit shallow pyroxene absorptions. The objective of this presentation is to: 1) determine the modal mineralogy of a variety of volcanic mafic-rich regions using OMEGA data, 2) compare the modal and chemical composition with those derived from Thermal Emission Spectrometer (TES) analyses (McSween et al., JGR 108, 2003; Rogers and Christensen, JGR 112, 2007), 3) identify possible relationship with the diverse compositions of SNCs, 4) evaluate constraints on the chemistry and petrology of the volcanic deposits through time.
Aléon-Toppani A.
Bardintzeff J.
Bibring J.
Gondet Brigitte
Langevin Yves
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