A thermal emission spectral library of rock-forming minerals

By Philip R. Christensen, J. Bandfield, V. Hamilton, D. A. Howard, M. Lane, J. Piatek, S. Ruff, W. Stefanov. 2000

406 citations recorded by the source corpus.

Subfields: Artificial Intelligence, Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/d1dbb3de856dfd8bcbf8b9d7fbcbe79c6ec0d2a1

How researchers see this paper

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

In Artificial Intelligence

In Astronomy and Astrophysics

In Geophysics

Citations in the corpus

The Compositional Structure of the Asteroid Belt (2015, background): “Minerals can be identified by emission features (e.g., Christensen et al., 2000) with silicates being the most common and easiest to identify (e.g., Beichman et al., 2005, Lisse et al., 2012, Ballering et al., 2014).”
Miniature thermal emission spectrometer for the Mars Exploration Rover (2002, methodology): “[15] The primary silicate minerals associated with igneous rocks are the most abundant mineral class found on Mars [Christensen et al., 2000b; Bandfield et al., 2000; Christensen et al., 2001a; Bandfield, 2002], and the ability to distinguish and quantify volcanic minerals, such as feldspars,…”
Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces (2010, methodology): “BUR-3720Aa AZ-01a KI 3115b KI 3362b KI 3372c KI 4143b KI 3373b KI 3352b KI 3354b KI 3008b WAR-FAY01c SiO2 41.95 38.47 37.40 34.91 35.17 33.36 32.83 31.33 31.06 30.11 29.27 TiO2 0.01 0.01 0.01 0.01 0.00 0.05 0.02 0.01 0.02 0.03 – FeO 8.49 9.57 29.01 34.04 38.77 48.71 50.75 56.46 60.43 64.00 67.51 MnO”
The ASTER spectral library version 2.0 (2009, background): “More recently, complimentary spectral libraries have been made available from other collections, for example: http://speclib.asu. edu (Christensen et al., 2000), http://pds.geosciences.wustl.edu/ missions/mro/spectral_library.htm and http://speclab.cr.usgs.gov (Clark et al., 2007).”
Constraints on the composition and petrogenesis of the Martian crust (2003, methodology): “The wave number range of 400 – 233 cm À1 was not used for deconvolutions in previous studies because mineral end-member spectra in the ASU Thermal Emission Spectroscopy library [Christensen et al., 2000c] only extended to 400 cm À1 .”
Global mapping of Martian hematite mineral deposits: Remnants of water‐driven processes on early Mars (2001, methodology): “Atmosphere-removed TES spectra from the initial hematite discovery site in Sinus Meridiani [Christensen et al., 2000c] (Figure 1) show that the surface is composed primarily of basaltic material [Christensen et al., 2000b; Bandfield et al., 2000a] that has absorptions from 1250 to 680 cm 1 and 500…”
Global mineral distributions on Mars (2002, methodology): “Spectroscopic evidence indicates that these materials were most likely formed from precipitation from aqueous fluids, and morphologic features such as layered, friable units of these localities suggest a sedimentary environment [Christensen et al., 2000a, 2001b].”
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].”
Europa’s Surface Composition (2009, background): “While large spectral databases exist for many materials (Clark et al., 1993, 2003, 2007; Henning et al., 1999; Christensen et al., 2000) and applications to Mars have prompted spectroscopic studies of sulfate minerals (Cloutis et al., 2006), many measurements do not encompass Europa’s entire solar…”
Derivation of an urban materials spectral library through emittance and reflectance spectroscopy (2014, positive): “…temperature T relative to that emitted by a perfect blackbody at the same kinetic temprature L k : Hence, measurements of the sample’s thermal emitted radiance spectra can be used to derive spectral emissivity information (e.g. Ruff et al., 1997; Christensen et al., 2000; Kerekes et al., 2008).”
Absorption and reflection infrared spectra of MgO and other diatomic compounds (2003, methodology): “For very large samples, the colder outside layers absorb the essentially blackbody emissions from the interior, producing spectra in emission that look like absorption [cf. emission spectra of Christensen et al. (2000) to those of Bates (1978)].”