Evidence for extensive, olivine-rich bedrock on Mars

By V. Hamilton, Philip R. Christensen. 2005

203 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fb0a81939569489ba69090d862648226b07aa694

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In Aerospace Engineering

In Astronomy and Astrophysics

Citations in the corpus

The Sedimentary Rock Record of Mars: Distribution, Origins, and Global Stratigraphy (2012, background): “Rover measurements have shown that the major constituents of this material are consistent with pulverized, unaltered basalt (Goetz 2005, Hamilton and Christensen 2005).”
Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces (2010, background): “, 2003), laterally extensive lava flows (Hamilton and Christensen, 2005) or an impact melt sheet (Mustard et al.”
CRISM multispectral summary products: Parameterizing mineral diversity on Mars from reflectance (2007, background): “As discussed by Bibring et al. [2005, 2006] and Mustard et al. [2005], highlighted areas are seen mainly in association with volcanic rocks in and around Syrtis Major as reported in the past [Hoefen et al., 2003; Hamilton and Christensen, 2005], as well as in crater floors and rims.”
Compact Reconnaissance Imaging Spectrometer for Mars investigation and data set from the Mars Reconnaissance Orbiter's primary science phase (2009, background): “…Hesperian-aged layered deposits in Meridiani Planum and Valles Marineris [Christensen et al., 2001a], and furthermore revealed extensive outcrops of olivine that would easily have weathered in the presence of liquid water [Hoefen et al., 2003; Hamilton and Christensen, 2005; Edwards et al., 2008].”
Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO) (2007, methodology): “OMEGA, TES, and THEMIS data covering regions with spectral heterogeneity [Mustard et al., 2005; Hamilton and Christensen, 2005] together provide the first insights into the temporal evolution of Martian magma source regions, described above.”
Mineralogy of the Martian Surface (2014, background): “These circumferential deposits have been proposed to represent igneous intrusions (Hoefen et al. 2003); upper-mantle-sourced cumulates that settled from impact melt (Mustard et al. 2007, 2009); or fluid, komatiitic-type lavas (Hamilton & Christensen 2005, Tornabene et al. 2008).”
Global investigation of olivine on Mars: Insights into crust and mantle compositions (2013, background): “…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 al., 2007; Koeppen and Hamilton, 2008; Edwards et al., 2008; Salvatore et al., 2010;…”
High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications (2006, background): “High thermal inertia surfaces corresponding to exposed bedrock have been identified with THEMIS data, and these surfaces are found to range in size and to be exposed in a variety of geologic settings, such as crater interiors, channel walls, chaotic terrain, and the Martian plains [e.g., Rogers et a”
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): “5.5.1. Mg-Rich Olivine [33] All previously identified olivine regions are detected using the forsterite spectral parameter and include Nili Fossae, Terra Meridiani, Syrtis Major and Ganges Chasma [Bandfield, 2002; Christensen et al., 2003; Hoefen et al., 2003; Hamilton and Christensen, 2005; Musta”