The composition of asteroid 2 Pallas and its relation to primitive meteorites
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Cited by (38)
Low-temperature specific heat capacity measurements and application to Mars thermal modeling
2019, IcarusCitation Excerpt :Knowledge of the specific heat capacity (the adjective “specific” means “per unit of mass”) and its temperature dependence in the 130–320 K range relevant for Mars are relatively limited for many geological materials (Touloukian et al., 1970; Gottschalk, 1997; Waples and Waples, 2004). With the exception of basalt and a few minerals noted below, most published specific heat measurements of volcanic and igneous rocks were performed at or above room temperature (Buettner, 1963; Winter and Saari, 1969; Waples and Waples, 2004), despite the diversity of materials identified on planetary bodies (e.g. quartz-bearing granitoids (Bandfield et al., 2004), dacite (Christensen et al., 2005; Koeppen and Hamilton, 2008), amorphous silica (Squyres et al., 2008), as well as many phases related to aqueous environments, various glasses (Morris et al., 2006), and other primitive materials identified on asteroids (Larson et al., 1983; Licandro et al., 2007). Extrapolation of these specific heat capacity measurements to lower temperatures is not a satisfactory option because the Debye temperature of most materials is usually unknown.
Bidirectional reflectance spectroscopy of carbonaceous chondrites: Implications for water quantification and primary composition
2016, IcarusCitation Excerpt :Major spectroscopic surveys are limited to the VNIR and typically lack the 3-μm feature, which is the most diagnostic for –OH/H2O bearing phases (water–ice, hydrated hydroxylated minerals, alcohol function). Such “water” related absorptions have been observed on asteroidal surfaces (Lebofsky et al., 1981; Larson et al., 1983; Jones et al., 1990; Rivkin et al., 2002), but observations in this region are usually limited to large objects and the effort of building a taxonomy based on this spectral range is ongoing (Takir and Emery, 2012). At present, most observations at 3-μm have been interpreted by the presence of –OH bearing mineral phase, and a few of them by the presence of water ice (mostly outer main belt objects, Campins et al., 2010; Rivkin and Emery, 2010; Takir and Emery, 2012; see also Beck et al. (2011) for an alternative – goethite).
Thermal infrared observations and thermophysical characterization of OSIRIS-REx target asteroid (101955) Bennu
2014, IcarusCitation Excerpt :The B-class includes many intriguing objects such as (2) Pallas, the second largest asteroid, (24) Themis, the largest member of the Themis family, and (3200) Phaethon, the parent of the Gemenid meteor shower (e.g., de León et al., 2010). Spectroscopy of B-class objects suggests surface constituents are anhydrous silicates, hydrated silicates (phyllosilicates), organic polymers, magnetite, and sulfides (Larson et al., 1983; Clark et al., 2010; Ziffer et al., 2011; de León et al., 2012), and those in the outer Main Belt may support H2O ice (Rivkin and Emery, 2010; Campins et al., 2010a). Dynamically and spectrally, Bennu itself is likely related to a population of B-type asteroids in the inner belt (e.g., Campins et al., 2010b; Walsh et al., 2013).
Asteroids
2013, Treatise on Geochemistry: Second EditionWater, heat, bombardment: The evolution and current state of (2) Pallas
2012, IcarusCitation Excerpt :Several other lines of evidence exist for a water-rich past, and possibly present, for Pallas. Its near-IR spectrum possesses a ∼3-μm absorption feature that is indicative of hydration, requiring that its surface minerals were processed in the presence of liquid water (Lebofsky, 1979; Larson et al., 1979, 1983). Pallas’s surface shows evidence for albedo variation in the UV that is consistent with gradients in either thermal processing or water content of its surface materials (Schmidt et al., 2009).
Spectral reflectance properties of carbonaceous chondrites: 1. CI chondrites
2011, IcarusCitation Excerpt :While tentative links between other CCs and various taxonomic classes of asteroids have been made (e.g., Burbine et al., 1992; Burbine, 1998; Carvano et al., 2003), attempts to match CIs to dark asteroids often fail, usually on the basis of presence/absence of absorption bands, wavelength position of the UV–visible reflectance downturn, and overall spectral slopes (e.g., Gaffey and McCord, 1977; Hiroi et al., 1993; Kelley et al., 2007). While possible links between some C-/B-class asteroids and CIs have been advanced, it appears that modifications to CI mineralogy must be invoked to match CIs to members of other asteroid taxonomic classes (Larson et al., 1983; Gaffey et al., 1993). An absorption complex in the 0.95–1.2-μm region, attributable to Fe2+-bearing phyllosilicates ± magnetite, present in some of the CI spectra, suggests that it may be fruitful to search for similar features in asteroid spectra.
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National Research Council Associate.