Constraining The Surface Mineralogy of Mars: Infrared (2.5 to 14 micron) Reflectance Microspectroscopy Of Meteoritic Minerals In Thin Section.

Details Constraining The Surface Mineralogy of Mars: Infrared (2.5 to 14 micron) Reflectance Microspectroscopy Of Meteoritic Minerals In Thin Section. Constraining The Surface Mineralogy of Mars: Infrared (2.5 to 14 micron) Reflectance Microspectroscopy Of Meteoritic Minerals In Thin Section.

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p23c0073h&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P23C-0073

Computer Science

Databases

5460 Physical Properties Of Materials, 5464 Remote Sensing, 5470 Surface Materials And Properties, 6094 Instruments And Techniques, 6225 Mars

Scientific paper

The surface mineralogy of Mars is constrained using spectral and chemical data gathered by spacecraft in orbit around and landers roving on the planet. One of the most common techniques for determining lithologies is using thermal emission spectroscopy. Virtually the entire surface of Mars has been mapped using either the TES [1] or THEMIS [2] instruments. These complex spectral data can be deconvolved [3] into their constituents using a spectral database [e.g., 4] of terrestrial minerals, thus giving a good understanding of the surface composition of Mars, which in turn allows interpretation of its history. The spectral database in use is extensive and contains over 200 different phases. Most spectral data are acquired using systems that observe spots ranging from 1mm to several cm. The use of microspectroscopy is limited to a few studies [e.g. 5]. This method allows expansion of spectral databases to include exotic and fine-grained minerals that are present in meteorite thin sections that would be hard to physically separate. Preliminary spectral measurements on thin sections [6, 7] have been carried out using an infrared microscope attached to a benchtop FT-IR. Using a similar system, we have measured the mineral constituents of Nakhla and Murchison. Augite in Nakhla exhibits zoning in Fe content. We tested the robustness of our method by measuring more than 100 augite cores and rims in a single thin section of Nakhla. There are two distinct spectral shapes, although they do not seem to correlate with cores and rims. Future work will also include measurement of spectra of pigeonite in shergottites as well as other pyroxenes from eucrites and diogenites. [1] Christensen et al. (2001) JGR, 106, 23823-23871. [2] Christensen P.R. et al., (2004) Space Sci. Rev., 110, 85-130. [3] Ramsey M. and Christensen P.R. (1998) JGR, 103, 577-596. [4] Christensen et al., JGR, 105, 9735-9739, 2000. [5] Klima R.L. and C.M. Pieters (2006) JGR 111, E01005. [6] Morlok A. et al. (2006) MAPS 41, 773-784. [7] Palomba et al (2006) Icarus 182, 68-79.

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