Mathematics – Logic
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p23c0070w&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #P23C-0070
Mathematics
Logic
5410 Composition (1060, 3672), 5464 Remote Sensing, 6225 Mars
Scientific paper
Bounce Rock was found by the MER Opportunity rover and is interpreted as an anomalous distal impact ejecta deposited on the windblown sands of the Meridiani plains [Squyres et al., Science, 2004]. X-Ray, Moessbauer, and thermal infrared (TIR) spectra of Bounce Rock are distinct from any measured at either Rover landing site and are best matched by various basaltic shergottites such as Shergotty and Zagami. Recent work on the TIR spectra of experimentally shocked plagioclases and basalts [Johnson et al., JGR, 2002; 2006] and shocked terrestrial basalt [Wright et al., LPSC, 2006] suggest that the Mini-TES spectrum of Bounce Rock appears to be an unshocked version of Zagami or perhaps Shergotty. Spectral observations of unshocked martian lithologies similar in composition to martian meteorites are important for constraining the extent of SNC-like lithologies in orbital data as all meteorite samples display some degree of shock effect and may not be representative of the bulk of martian surface compositions. The Mini-TES spectrum of Bounce Rock thus represents a rare unshocked pigeonite-augite-plagioclase basalt spectrum that would never be available in meteorite collections or spectral libraries. This fact and the difficulties of both producing an artificial pigeonite spectrum and finding pigeonite-rich regions on Mars make the Bounce Rock spectrum an excellent end-member in the search for potential shergottite source regions with global TIR data. Previous work locating Thermal Emission Spectrometer (TES) pixels high in olivine, orthopyroxene [Hamilton et al., MaPS, 2003], and quartzofeldspathic minerals [Bandfield et al., JGR, 2004] have shown the utility of using lithologic end-members rather than large mineral spectral libraries. However, minerals with higher polymerization than feldspar such as olivines and pyroxenes do not show changes in TIR spectra at the shock level all shergottites have been subjected to [Johnson et al., JGR, 2002]. In this work, global TES data were binned to 4 pixels per degree. End-members include six atmospheric end-members, Surface Type 1 (plagioclase-rich basalt), Surface Type 2 (andesite or weathered basalt), hematite, dust, and Bounce Rock. Distributions of the surface end-members are normalized to 100%. Global maps of the distributions of ST1, ST2, dust, and hematite agree with previous work [Bandfield et al., Science, 2000; McSween et al., JGR, 2003; Christensen et al., JGR, 2000]. The global distribution of pixels high in the Bounce Rock end-member were further limited to ensure high thermal inertia, no dust, and concentrations of 25% or more. Visual inspection shows these TES spectra resemble the Mini-TES spectrum of Bounce Rock. Detailed analyses of these sites using individual TES pixels (rather than binned data), THEMIS spectral data, and other orbital data will be shown.
Christensen Per Rex
Wright Shawn P.
Wyatt Michael Bruce
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