Lunar red spots: Possible pre-mare materials
References (21)
- et al.
Mare Humorum: an integrated study of spectral reflectivity
Icarus
(1973) - et al.
Geologic map of the near side of the moon
U.S. Geol. Survey Map 1–703
(1971) Lunar color boundaries and their relationship to topographic features
The Moon
(1972)Color differences on the lunar surface
- et al.
Lunar spectral types
J. Geophys. Res.
(1972) - et al.
Remote sensing of lunar surface mineralogy implications from visible and near infrared reflectivity of Apollo 11 samples
- et al.
Electronic spectra of pyroxenes and the interpretation of telescopic spectral reflectivity curves on the moon
The distribution and ages of regional units in the lunar maria
- et al.
Technique for rapid determination of relative ages of lunar areas using orbital photography
J. Geophys. Res.
(1972) - et al.
Origin of the lunar regolith at Tranquility Base
Cited by (41)
Geology of Mairan middle dome: Its implication to silicic volcanism on the Moon
2018, Planetary and Space ScienceCitation Excerpt :The focus of this study is MMD, the largest of four small domes (Fig. 2). Mairan middle dome is a lunar “red spot” characterized by relatively high albedo, strong absorption in the UV, and is thought to be a volcanic construct produced by non-mare volcanism connected with KREEP basalts or even more evolved highlands composition, such as dacite or rhyolite (Malin, 1974; Wood and Head, 1975; Head and McCord, 1978). These volcanic centers appear to be petrologic anomalies on the Moon that represent strong geochemical departures from primordial compositions, and are indicators of magma processing.
Hansteen Mons: An LROC geological perspective
2017, IcarusThe Lassell massif-A silicic lunar volcano
2016, IcarusCitation Excerpt :Nevertheless, both telescopic and orbital observations of morphologically and compositionally distinct constructs, including the nearside lunar red spots (regions of strong ultraviolet (UV) absorption), have supported non-mare, Si-rich volcanic interpretations (e.g., Whitaker, 1972a; Malin, 1974; Wood and Head, 1975; Head and McCord, 1978; Müller et al., 1986; Chevrel et al., 1999; Hawke et al., 2001, 2003; Hagerty et al., 2006; Glotch et al., 2010; Wagner et al., 2010; Glotch et al., 2011; Jolliff et al., 2011; Kusuma et al., 2012; Lawrence et al., 2014; Wilson et al., 2015). The lunar red spots (first identified based on a spectral contrast between the UV and visible) include Hansteen Alpha, Herigonius ε and π, the Gruithuisen domes, Montes Riphaeus, portions of Aristarchus crater and its plateau, and the Lassell massif (Whitaker, 1972b; Malin, 1974; Wood and Head, 1975; Bruno et al., 1991; Hawke et al., 2001). Many red spots, including the Lassell massif, correlate with anomalously high Th signatures in Lunar Prospector Gamma-Ray Spectrometer (LP GRS) data, consistent with evolved magma sources (Hawke et al., 2001; Lawrence et al., 2003; Hagerty et al., 2006).
The lunar Gruithuisen silicic extrusive domes: Topographic configuration, morphology, ages, and internal structure
2016, IcarusCitation Excerpt :Both types of flows occur at different elevations indicating that their sources exist at different levels within the Gruithuisen-Gamma dome. The Gruithuisen domes form three unusually high (1.4–1.7 km) topographic features that are associated with one of the lunar red spot complexes (Whitaker, 1972; Malin, 1974). The general shape of the domes and their specific spectral characteristics have been interpreted as evidence of formation by eruptions of high-viscosity, silica-rich lavas (Wood and Head, 1975; Head et al., 1978; Head and McCord, 1978; Wilson and Head, 2003).
Contribution No. 2386, Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena 91109.