Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p51f..02b&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P51F-02
Physics
[3620] Mineralogy And Petrology / Mineral And Crystal Chemistry, [5464] Planetary Sciences: Solid Surface Planets / Remote Sensing, [5470] Planetary Sciences: Solid Surface Planets / Surface Materials And Properties, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
Great advances have been achieved recently in our understanding of the surface of Mars at global scales from orbital missions and at local scales from landed missions. This presentation seeks to provide links between the chemistry and mineralogy observed by landed missions with remote detections of minerals from orbit. Spectral data from CRISM, OMEGA and TES characterize a mostly basaltic planet with some outcrops of hematite, clays, sulfates and carbonates at the surface. Recent alteration of these rocks to form soils has likely been dominated by physical processes; however, martian soils probably also contain relicts of early alteration involving aqueous processes. Clays, hydroxides, sulfates, carbonates and perchlorates are examples of surface components that may have formed early in the planet’s history in the presence of liquid water. Some of these minerals have not been detected in the soil, but all have likely contributed to the current soil composition. The grain size, shape, chemistry, mineralogy, and magnetic properties of Martian soils are similar to altered volcanic ash found at many analog sites on Earth. Reflectance and emission spectra of some of these analog soils are consistent with the basic soil spectral properties observed from orbit. The cemented soil units observed by rovers may have formed through interaction of the soil grains with salts, clays, and hydroxides. Lab experiments have shown that cementing of analog grains darkens the VN reflectance, which could explain the low reflectance of Martian soils compared to analog sites. Reflectance spectra of an analog soil mixture containing altered ash and sulfate are shown in Figure 1. A pellet was made by adding water and allowing the sample to dry in air. Finally, the pellet was crushed and ground again to <125 µm. Both the dried pellet spectrum and the crushed pellet spectrum are darker than the original spectrum of the same composition. Erosion and weathering are likely the dominant processes forming the soils on Mars. However, reaction of surface grains with sulfates and perchlorates probably also influenced the soil grains. The perchlorates found by Phoenix are a strong oxidant. Consideration is being given to the interactions of perchlorates with minerals identified in surface rocks (pyroxene, olivine, feldspar, phyllosilicate, iron oxides, sulfate, silica, carbonate) and how perchlorates might be contributing to soil formation from these minerals and what their spectral properties might be.
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