Global mineral distributions on Mars

By J. Bandfield. 2002

396 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/15e79a1a2137926340d7842fff228e7b3f90356a

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Citations in the corpus

Distribution, morphology, and origins of Martian pit crater chains (2004, background): “(e.g., carbonates) in the quantities called for by their model has not been found to date [ Bandfield, 2002 ].”
Global investigation of olivine on Mars: Insights into crust and mantle compositions (2013, background): “…identified large olivine regions including Nili Fossae, Terra Tyrrhena, Chryse Planitia, Argyre basin, Valles Marineris are visible [e.g., Bandfield, 2002; Christensen et al., 2003; Hoefen et al., 2003; McSween et al., 2006; Hamilton and Christensen, 2005; Mustard et al., 2005; Poulet et…”
Ripple migration and dune activity on Mars: Evidence for dynamic wind processes (2010, background): “These dunes consist of low albedo sand that, like dark sand elsewhere on Mars, is likely basaltic in origin [Bandfield, 2002; Tirsch et al., 2008].”
Martian surface mineralogy from Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité on board the Mars Express spacecraft (OMEGA/MEx): Global mineral maps (2007, methodology): “This map is consistent with the TES global pyroxene map [Bandfield, 2002] and with the map derived from OMEGA observations analyzed with the Modified Gaussian Model [Bibring et al., 2006].”
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 crust mi”
Constraints on the composition and petrogenesis of the Martian crust (2003, background): “…[e.g., Christensen et al., 2000b] , orthopyroxene [e.g., Hamilton et al., 2003; Bandfield, 2002] , and olivine [e.g., Clark et al., 1982; Hamilton et al., 2003; Bandfield, 2002] have also been identified in regional and local occurrences where surface type 1 compositions dominate surface units.”
Searching for the source regions of martian meteorites using MGS TES: Integrating martian meteorites into the global distribution of igneous materials on Mars (2003, background): “Concentrations of 0.10 are the minimum detection limit previously identified for martian data (Bandfield et al. 2000; Christensen et al. 2000b; Bandfield 2002).”
Equatorial and midlatitude distribution of chlorine measured by Mars Odyssey GRS (2007, background): “Previous remote sensing attempts to measure Clbearing materials on a global scale using infrared spectroscopy from orbit have proved inconclusive [e.g., Bandfield, 2002; Lane and Christensen, 1998].”
Concentration of H, Si, Cl, K, Fe, and Th in the low- and mid-latitude regions of Mars (2007, background): “This enhancement corresponds closely to the surface type-2 region of Bandfield et al. [2000]. This region has been suggested to be”
High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications (2006, methodology): “This effect is not significant as changes in the 684emissivity from 1.0 to 0.96, which is typical for Mars at 68512.57 mm (band 9) [e.g., Bandfield, 2002], only changes the 686surface kinetic temperature 1.2 K, which translates to a 687!”
Detection and discrimination of sulfate minerals using reflectance spectroscopy (2006, background): “Bandfield (2002) tentatively identified a few areas in Acidalia that may contain sulfate minerals (type unknown but probably a Ca-sulfate) just above the detection limit (∼10”
Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, methodology): “[48] We included TES data that exhibited a larger range of water ice opacities ( Bandfield [2002] (<0.10).”
Mineralogical constraints on the high-silica martian surface component observed by TES (2005, background): “While there is some evidence that the Acidalia Planitia-type spectra may include a sulfate component (Bandfield, 2002), sulfates should produce an absorption centered near 1150 cm−1.”
Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces (2010, methodology): “This model represents a case similar to two previously published studies where no intermediate olivines were available (Hamilton et al., 1997; Bandfield, 2002).”
Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO) (2007, methodology): “While TES data have yielded some evidence for sulfates and sheet silicates, such identifications are close to the detection limits of the instruments [e.g., Bandfield, 2002].”
The Thermal Emission Imaging System (THEMIS) for the Mars 2001 Odyssey Mission (2004, methodology): “…martian surface at wavelengths from 6 to 50 micrometers, providing an initial global reconnaissance of mineralogy and thermophysical properties (Christensen et al., 2000b, d, 2001a; Bandfield et al., 2000a; Bandfield, 2002; Ruff and Christensen, 2002; Jakosky et al., 2000; Mellon et al., 2000).”