A Global View of Martian Surface Compositions from MGS-TES

By J. Bandfield, V. Hamilton, Philip R. Christensen. 2000

654 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/38a36740425dea3f17cee7b693e46fe39373f46e

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Citations in the corpus

Determination of molar absorptivities for infrared absorption bands of H2O in andesitic glasses (2002, neutral): “Andesites are one of the most common magma types on Earth, and may be widespread on Mars (Gill 1981; Grove and Kinzler 1986; Wilson 1989; McSween and Murchie 1999; Bandfield et al. 2000).”
Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, methodology): “For example, the surface type 1 spectral shape derived by Bandfield et al. [2000b] , which likely contains 5–10% olivine [Rogers and Christensen, 2007], produces olivine index values >1.0, but Bandfield et al. [2000b] , whereas the silica/ phyllosilicate map correlates with both surface type 1 and”
Revised CRISM spectral parameters and summary products based on the currently detected mineral diversity on Mars (2014, background): “Plagioclase Plagioclase is the most abundant mineral exposed on the surface of Mars [Bandfield et al., 2000; Bandfield, 2002] and also provides information about the magmatic evolution of the crust.”
Interannual variability in TES atmospheric observations of Mars during 1999–2003 (2004, methodology): “Using the “type 2” (andesitic-basalt) surface emissivity shape from Bandfield et al. (2000b) instead of our assumed “type 1” (basalt) shape results in systematic errors of about 0.005 in dust optical depth and about 0.003 in water ice optical depth.”
Mineralogical constraints on the high-silica martian surface component observed by TES (2005, methodology): “, 2001), there are dark regions, typified by Acidalia Planitia (Bandfield et al., 2000), that are not spectrally similar to fresh basaltic rock.”
Identification of quartzofeldspathic materials on Mars (2004, methodology): “[19] The deconvolution surface-atmosphere separation also provides areal mineral and spectral unit abundances that can be used for compositional analysis [Smith et al., 2000; Bandfield et al., 2000a; Bandfield, 2002; Hamilton et al., 2003].”
Crustal structure of Mars from gravity and topography (2004, background): “However the Thermal Emission Spectrometer data [ Bandfield et al. , 2000; Bandfield , 2002] suggest a more basaltic composition for dark regions in the south and a more silicic northern composition (but see also Wyatt and McSween [2002]), raising the possibility that, if anything, the southern…”
Selection of the Mars Science Laboratory Landing Site (2012, background): “The observed spectral identification of phyllosilicates at the sites is consistent with the lack of dust, as dusty regions do not show mineral identifications in thermal and infrared spectral data (Bandfield et al. 2000; Bibring et al. 2006; Mustard et al. 2008).”
Possible formation of ancient crust on Mars through magma ocean processes (2005, methodology): “Data from the Thermal Emission Spectrometer (TES) aboard the Mars Global Surveyor [Bandfield et al., 2000] has shown that the major element compositions of the southern highlands and the northern lowlands are significantly different.”
Bright and dark regions on Mars: Particle size and mineralogical characteristics based on thermal emission spectrometer data (2002, background): “To date, surface studies using TES spectra have focused on dark regions, where basalt, basaltic andesite, and hematiterich materials have been identified [Bandfield et al., 2000a; Christensen et al., 2000a, 2000b].”
The Syrtis Major volcanic province, Mars: Synthesis from Mars Global Surveyor data (2004, methodology): “In addition, we used TES data on the composition of the Syrtis Major basalts [e.g., Bandfield et al., 2000; Christensen et al., 2001], as well as THEMIS IR images [e.g., Christensen et al., 1999], and Viking image mosaics at $230 m spatial resolution (Mars Digital Image Model MDIM).”
Global mineral distributions on Mars (2002, methodology): “Global mapping revealed two major distinct spectral units within Martian low-albedo regions [Bandfield et al., 2000a].”
Mineralogy of the Martian Surface (2014, background): “…do not possess the distinctive spectral properties imparted by pyroxene in the Si-O stretch (10 μm; 1,000 cm−1) and at lower wavenumbers but rather have a sharper Si-O absorption characteristic of high-silica phases (Figure 1) (Bandfield et al. 2000, Wyatt & McSween 2002, Kraft et al. 2003).”
Impact‐induced hydrothermal activity on early Mars (2005, methodology): “The liquidus and solidus temperatures of 1280 C and 1070 C, respectively, were chosen on the basis of those of gabbro [Ernst, 1976], a coarse-grained equivalent of basalt, because the surface ofMars appears to be dominated by basaltic lithologies [Bandfield et al., 2000].”
Constraints on the composition and petrogenesis of the Martian crust (2003, methodology): “9 -8 sedimentary minerals [Bandfield et al., 2000; Hamilton et al., 2001; Wyatt and McSween, 2002].”