2004
DOI: 10.1016/j.icarus.2003.10.020
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Properties of the Hermean regolith: V. New optical reflectance spectra, comparison with lunar anorthosites, and mineralogical modelling

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Cited by 75 publications
(70 citation statements)
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References 64 publications
(158 reference statements)
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“…Although we have only limited information on the abundance of FeO in Mercury's crust, information on the abundances of other key elements (e.g., Ca, Si, Mg, K, Ti) that are concentrated in planetary crusts during differentiation is even more restricted. Ti may be particularly informative, since, like FeO, it appears to be low in abundance in Mercury surface silicates (Warell and Blewett, 2004), but it couples with iron in a variety of Fe-Ti-oxides in crustal rocks on other bodies.…”
Section: Introductionmentioning
confidence: 99%
“…Although we have only limited information on the abundance of FeO in Mercury's crust, information on the abundances of other key elements (e.g., Ca, Si, Mg, K, Ti) that are concentrated in planetary crusts during differentiation is even more restricted. Ti may be particularly informative, since, like FeO, it appears to be low in abundance in Mercury surface silicates (Warell and Blewett, 2004), but it couples with iron in a variety of Fe-Ti-oxides in crustal rocks on other bodies.…”
Section: Introductionmentioning
confidence: 99%
“…The particle-size range in the sample with finer particle sizes corresponds closely to the particle-size distribution in hermean regolith which have a median at ∼30 μm (Warell and Blewett 2004), even though the chemical composition of the hermean regolith is unlikely to be close to olivine basalt. The sample material with larger particle sizes has also been used in a study 10…”
Section: Sample Materialsmentioning
confidence: 66%
“…The key morphologic properties used to identify flood lavas on the Moon (other than albedo) are embayment relationships and ponding in topographic lows (usually basins; see arrows on both images). For the Moon, classic flow features such as flow fronts and vents are not visible at a scale of 1 km, except in some cases under low-Sun illumination (see Milkovich et al 2002, and references therein) ences , although a generally anorthositic crust is favored (Blewett et al 2002;Warell and Blewett 2004). From the data currently available it is not possible to identify basaltic material or of any other rock type; however, the Mariner 10-derived spectral parameters, stratigraphic relations, and morphology are interpreted by numerous workers to be consistent with volcanically emplaced materials (e.g., Spudis and Guest 1988;.…”
Section: Chemistry and Mineralogymentioning
confidence: 99%