Bright and dark regions on Mars: Particle size and mineralogical characteristics based on thermal emission spectrometer data

By S. Ruff, Philip R. Christensen. 2002

421 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b8b7b65c829b9a536d255bd0ab77e338a069eee1

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. W. Koeppen
5. J. Bandfield
6. J. Bibring
7. Hugh H. Kieffer
8. J. F. Mustard

In Astronomy and Astrophysics

1. V. Hamilton
2. Philip R. Christensen
3. H. McSween
4. J. Bandfield
5. W. Koeppen
6. James W. Head III
7. J. Bibring
8. Ralph E. Milliken

Citations in the corpus

• The rayed crater Zunil and interpretations of small impact craters on Mars (2005, background): “All six of the other rayed craters are also l cated over regions of Mars with moderate thermal ine but a bright albedo, along the margins of the regions of h dust-cover index(Ruff and Christensen, 2002) and low thermal inertia, so perhaps this type of surface is needed to f and/or preserve the rays.”
• Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface (2007, methodology): “, thermal inertia derived using TES data) [Christensen, 1986; Christensen and Moore, 1992; Mellon et al., 2000; Ruff and Christensen, 2002; Putzig et al., 2005].”
• Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, methodology): “region of TES data because it is relatively free of features associated with suspended dust and atmospheric CO2 gas, and it serves as a spectral window through which surface emissivity features are observed, even in data that are not atmospherically corrected [ Ruff and Christensen, 2002; Bandfield”
• 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, background): “The major trends are the same than those of the visible albedo map or bolometric albedo [Mellon et al., 2000; Ruff and Christensen, 2002].”
• Physical properties of the Mars Exploration Rover landing sites as inferred from Mini‐TES–derived thermal inertia (2006, background): “al., 2006] greater than � 60 mm [e.g., Ruff and Christensen, 2002 ].”
• 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): “Ratios (or differences) of two spectra contain contributions from both spectra and the ratio spectrum should be interpreted with caution (Ruff and Christensen 2002).”
• Dust devils on Earth and Mars (2006, methodology): “Dust devil diameter frequency distributions from six studies: (a) Sinclair [1969], Avra Valley, (b) Sinclair [1969], Tucson, (c) Sinclair [1965], (d) Carroll and Ryan [1970], (e) Snow and McClelland [1990], AOC 1985 census, and (f) Snow and McClelland [1990], AOC 1987 census. N is the total number o”
• Selection of the Mars Science Laboratory Landing Site (2012, methodology): “The amount of dust cover at the landing sites was also evaluated using the TES dust cover index (16 pixels per degree), which includes a more explicit measure of the particle size and the amount of dust coating the surface (Ruff and Christensen 2002).”
• OSIRIS-REx: Sample Return from Asteroid (101955) Bennu (2017, background): “The heritage for the dust cover index is a product first published by Ruff and Christensen (2002).”
• The current martian cratering rate (2010, background): “This idea was first presented (and rejected) by Shoemaker (1965), but has been championed by subsequent workers (e.g., Wilhelms et al., 1987; Xiao and Strom, 2012).”
• 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).”
• Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces (2010, background): “…sort of analysis can be enhanced and/or enabled by the use of data manipulations that isolate spectral components of interest, such as carefully constructed spectral subtractions or ratios (e.g., Ruff and Christensen, 2002; Hamilton et al., 2003; Hoefen et al., 2003; Koeppen and Hamilton, 2008).”
• Selection of the InSight Landing Site (2017, background): “97 (Ruff and Christensen 2002) and landing sites that are no dustier than this (i.”
• High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications (2006, background): “The dust cover index (DCI; 0.93–0.94) also indicates that a surface layer of fine, unconsolidated material is present [ Ruff and Christensen, 2002 ].”