Mathematics – Logic
Scientific paper
Mar 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27..925m&link_type=abstract
Lunar and Planetary Science, volume 27, page 925
Mathematics
Logic
1
Composition, Mars, Spectroscopy, Syrtis Major, Valles Marineris
Scientific paper
The high spatial resolution, spectral coverage, and high signal to noise of the ISM data have permitted the determination of a mineralogic basis for the spectral properties of weakly altered regions of Mars. Through the use of the Modified Gaussian Model (MGM), it was demonstrated that weakly altered mafic materials are dominated by two-pyroxene basalts, analogous to the basaltic SNC meteorites. In addition, differences in spectral properties between Eos Chasma and Nili Patera were best modelled as a change in relative modal abundance of low (LCP) and high (HCP) calcium pyroxene, with Nili Patera enriched in high-calcium pyroxene relative to Eos Chasma. There is a great deal of diversity within other spectra of weakly altered crust identified thus far, and some of this diversity is due to mixing with dust and alteration products, and some to mineralogic variations. We have examined the mineralogic basis for this diversity to determine how regionally extensive these mineralogic differences are, the degree of homogeneity of surface compositions, and if other compositional units can be identified. For all areas examined, the weakly altered materials on Mars are best modelled as two-pyroxene basalts enriched in HCP. Syrtis Major, a low relief, Early Hesperian, shield volcano, has a homogeneous composition with the highest relative abundance of HCP. Ophir Planum, a region of ridged, volcanic(?) plains, is also enriched in HCP, but has ~12% less than Syrtis, while the floor of Valles Marineris is the ~20%-25% less HCP than Syrtis. These differences can be interpreted to indicate a change in source mantle composition from relatively fertile (Syrtis Major, Ophir Planum) to depleted (Valles Marineris), which would be consistent with the relative ages and environments of formation.
Mustard John F.
Sunshine Jessica M.
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