Spectral evidence for zeolite in the dust on Mars

By S. Ruff. 2002

170 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fe8525a4d4dfcd07a94eea187edab23baa56b6e0

How researchers see this paper

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

In Aerospace Engineering

1. V. Hamilton
2. H. McSween
3. Philip R. Christensen
4. J. Bandfield
5. J. Bibring
6. J. F. Mustard
7. Yves Langevin
8. B. Gondet

In Astronomy and Astrophysics

1. H. McSween
2. V. Hamilton
3. Philip R. Christensen
4. J. Bandfield
5. J. Bibring
6. Bethany L. Ehlmann
7. J. F. Mustard
8. Yves Langevin

Citations in the corpus

• 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): “In the TIR regime, recent works by Ruff and Christensen [2002] using TES data conclude that the bright Martian surface is dominated by plagioclase feldspar particles 100 mm in size that could have a significant zeolite component [Ruff, 2004].”
• Revised CRISM spectral parameters and summary products based on the currently detected mineral diversity on Mars (2014, background): “TES spectra indicates that zeolite may be a significant component of Mars dust [Ruff, 2004], although the exact composition of the dust remains a subject of debate.”
• Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces (2010, background): “…spectra of these mineral groups is beyond the scope of this paper, but the spectra and discussions of their variations with solid solution composition can found in the literature (Piatek, 1997; Ruff, 1998, 2004; Christensen et al., 2000c; Hamilton, 2000; Michalski et al., 2003, 2006; Lane, 2007).”
• Stability of hydrous minerals on the martian surface (2003, background): “In addition, Ruff (2002) recently co cluded that new Thermal Emission Spectrometer (TES) provide good evidence for zeolites (unspecified) in mar surface dust.”
• Mineralogical constraints on the high-silica martian surface component observed by TES (2005, background): “42, and have been proposed as a possible constituent of TES surface spectra (Ruff, 2004).”
• Identification of quartzofeldspathic materials on Mars (2004, background): “Bandfield and Smith [2003] isolated the spectral shape of high-albedo surfaces that display evidence for framework silicates such as plagioclase or zeolites and bound water [Bandfield and Smith, 2003; Ruff, 2004] as well as low concentrations of carbonates [Bandfield et al., 2003].”
• Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface (2007, methodology): “…et al., 2005; Gendrin et al., 2005; Langevin et al., 2005; Poulet et al., 2005], whereas the fundamental H2O bend near 6 mm has been observed and mapped by other workers using Mars Global Surveyor Thermal Emission Spectrometer (TES) data [Bandfield and Smith, 2003; Ruff, 2004; Kuzmin et al., 2004].”
• Mineralogy of the Martian Surface (2014, background): “The dusty surfaces of Mars are hydrated in both VNIR and TIR data, and some features suggest the presence of a hydrated silicate such as a zeolite (Ruff 2004).”