Identification of a basaltic component on the Martian surface from Thermal Emission Spectrometer data

By Philip R. Christensen, J. Bandfield, Michael D. Smith, V. Hamilton, R. Clark. 2000

281 citations recorded by the source corpus.

Subfields: Artificial Intelligence, Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/5bebeac2a249780ad6ab18193d0a277eabe366bf

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Artificial Intelligence

1. V. Hamilton
2. J. Bandfield
3. H. McSween
4. Philip R. Christensen
5. W. Koeppen
6. T. Grove
7. M. Wyatt

In Astronomy and Astrophysics

1. V. Hamilton
2. H. McSween
3. W. Koeppen
4. Philip R. Christensen
5. J. Bandfield
6. T. Grove
7. M. Wyatt
8. S. Ruff

In Geophysics

1. V. Hamilton
2. J. Bandfield
3. Philip R. Christensen
4. H. McSween
5. W. Koeppen
6. T. Grove
7. M. Wyatt
8. T. Sharp

Citations in the corpus

• The case for rainfall on a warm, wet early Mars (2002, background): “If this were the case, however, the argument is that hundreds of meters of carbonates should be sequestered in the Martian regolith, and, as discussed previously, there is no spectral evidence supporting this [Blaney and McCord, 1989; Christensen et al., 2000a].”
• Constraints on the composition and petrogenesis of the Martian crust (2003, methodology): “The wave number range of 400 – 233 cm À1 was not used for deconvolutions in previous studies because mineral end-member spectra in the ASU Thermal Emission Spectroscopy library [Christensen et al., 2000c] only extended to 400 cm À1 .”
• Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, methodology): “Such modeling has been used by many investigators to study laboratory, meteorite, and TES data with relatively good results [e.g., Hamilton et al., 1997; Feely and Christensen, 1999; Bandfield et al., 2000b; Christensen et al., 2000c; Hamilton and Christensen, 2000; Wyatt et al., 2001; Johnson et ”
• Mineralogy of the Martian Surface (2014, background): “…Opportunity rover has explored in situ a hematite-enriched unit detected by TES and associated with Hesperian sedimentary units, finding Mg/Ca/Fe sulfates, hematite, silica, and some residual primary phases from basalt (Figure 5i) (Christensen et al. 2000a, Clark et al. 2005, Glotch et al. 2006).”
• Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars (2003, methodology): “…component (surface type 1), crystalline hematite, and/or a component (surface type 2) that was identified as basaltic andesite, andesite, or partially weathered basalt (Bandfield et al. 2000; Christensen et al. 2000a; Christensen et al. 2000b; Hamilton et al. 2001c; Wyatt and McSween 2002).”
• Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces (2010, methodology): “BUR-3720Aa AZ-01a KI 3115b KI 3362b KI 3372c KI 4143b KI 3373b KI 3352b KI 3354b KI 3008b WAR-FAY01c SiO2 41.95 38.47 37.40 34.91 35.17 33.36 32.83 31.33 31.06 30.11 29.27 TiO2 0.01 0.01 0.01 0.01 0.00 0.05 0.02 0.01 0.02 0.03 – FeO 8.49 9.57 29.01 34.04 38.77 48.71 50.75 56.46 60.43 64.00 67.51 MnO”
• Mineralogical constraints on the high-silica martian surface component observed by TES (2005, background): “dark-region terrain has a TES signature similar to basalt (Bandfield et al., 2000; Christensen et al., 2000; Hamilton et al., 2001), there are dark regions, typified by Acidalia Planitia (Bandfield et al.”