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Examining Spectral Variations in Localized Lunar Dark Mantle Deposits Erica R University of Nebraska - Lincoln DigitalCommons@University of Nebraska - Lincoln USGS Staff -- ubP lished Research US Geological Survey 2015 Examining spectral variations in localized lunar dark mantle deposits Erica R. Jawin European Space Research and Technology Center, Noordwijk, Netherlands, [email protected] Sebastien Besse European Space Research and Technology Center, Noordwijk, Netherlands Lisa R. Gaddis USGS Astrogeology Science Center, Flagstaff, Arizona Jessica M. Sunshine University of Maryland James W. Head Brown University See next page for additional authors Follow this and additional works at: http://digitalcommons.unl.edu/usgsstaffpub Jawin, Erica R.; Besse, Sebastien; Gaddis, Lisa R.; Sunshine, Jessica M.; Head, James W.; and Mazrouei, Sara, "Examining spectral variations in localized lunar dark mantle deposits" (2015). USGS Staff -- Published Research. 861. http://digitalcommons.unl.edu/usgsstaffpub/861 This Article is brought to you for free and open access by the US Geological Survey at DigitalCommons@University of Nebraska - Lincoln. It has been accepted for inclusion in USGS Staff -- ubP lished Research by an authorized administrator of DigitalCommons@University of Nebraska - Lincoln. Authors Erica R. Jawin, Sebastien Besse, Lisa R. Gaddis, Jessica M. Sunshine, James W. Head, and Sara Mazrouei This article is available at DigitalCommons@University of Nebraska - Lincoln: http://digitalcommons.unl.edu/usgsstaffpub/861 PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Examining spectral variations in localized lunar 10.1002/2014JE004759 dark mantle deposits Key Points: Erica R. Jawin1,2,3, Sebastien Besse1, Lisa R. Gaddis4, Jessica M. Sunshine5, James W. Head3, • Spectra were analyzed of three 1,6 localized pyroclastic dark mantle and Sara Mazrouei deposits 1 2 • Glass-bearing materials were European Space Research and Technology Center, Noordwijk, Netherlands, Department of Astronomy, Mount Holyoke 3 identified in all DMDs College, South Hadley, Massachusetts, USA, Department of Earth, Environmental, and Planetary Sciences, Brown • Two new localized DMDs were University, Providence, Rhode Island, USA, 4USGS Astrogeology Science Center, Flagstaff, Arizona, USA, 5Department of fi identi ed in Dryden T and S craters Astronomy, University of Maryland, College Park, Maryland, USA, 6Now at Department of Earth Sciences, University of Toronto, Ontario, Canada Correspondence to: E. R. Jawin, Abstract The localized lunar dark mantle deposits (DMDs) in Alphonsus, J. Herschel, and Oppenheimer [email protected] craters were analyzed using visible-near-infrared spectroscopy data from the Moon Mineralogy Mapper. Spectra of these localized DMDs were analyzed for compositional and mineralogical variations within the Citation: deposits and were compared with nearby mare basalt units. Spectra of the three localized DMDs exhibited Jawin,E.R.,S.Besse,L.R.Gaddis, mafic absorption features indicating iron-rich compositions, although the DMDs were spectrally distinct from J. M. Sunshine, J. W. Head, and nearby mare basalts. All of the DMDs contained spectral signatures of glassy materials, suggesting the S. Mazrouei (2015), Examining spectral variations in localized lunar dark mantle presence of volcanic glass in varying concentrations across the individual deposits. In addition, the albedo deposits, J. Geophys. Res. Planets, 120, and spectral signatures were variable within the Alphonsus and Oppenheimer crater DMDs, suggesting 1310–1331, doi:10.1002/2014JE004759. variable deposit thickness and/or variations in the amount of mixing with the local substrate. Two previously unidentified localized DMDs were discovered to the northeast of Oppenheimer crater. The identification of Received 13 NOV 2014 Accepted 21 JUN 2015 high concentrations of volcanic glass in multiple localized DMDs in different locations suggests that the Accepted article online 24 JUN 2015 distribution of volcanic glass across the lunar surface is much more widespread than has been previously Published online 29 JUL 2015 documented. The presence of volcanic glass implies an explosive, vulcanian eruption style for localized DMDs, as this allows volcanic glass to rapidly quench, inhibiting crystallization, compared to the larger hawaiian-style eruptions typical of regional DMD emplacement where black beads indicate a higher degree of crystallization. Improved understanding of the local and global distributions of volcanic glass in lunar DMDs will further constrain lunar degassing and compositional evolution throughout lunar volcanic history. 1. Introduction Deposits of lunar pyroclastic material, referred to as dark mantle deposits (DMDs), have been studied and mapped since the Apollo era [Wilhelms, 1968; Wilhelms and McCauley, 1971; Head, 1974; Gaddis et al., 1985, 2003; Weitz et al., 1998; Gustafson et al., 2012]. These fine-grained, low-albedo deposits are understood to be volcanic in nature [Wilson and Head, 1981]. They are characterized by unique spectral signatures [Pieters et al., 1973] and low radar returns [Gaddis et al., 1985] owing to large amounts of Fe-bearing volcanic glass and a paucity of scattering surfaces >50 cm. Morphologically, these deposits appear to mantle underlying material, smoothing and subduing small-scale topographic features [Head, 1974]. Previous studies have identified over 100 DMDs across the lunar surface (Figure 1), ranging in areal extent from <10 km2 to ~50,000 km2 [Gaddis et al., 2003; Gustafson et al., 2012]. The largest of these (>1000 km2) are known as “regional” DMDs, while the smaller (typically ~200–500 km2)aretermed“localized” DMDs [Gaddis et al., 1985]. Localized DMDs, such as those in Alphonsus crater (Figure 2), often consist of multiple local patches, which in this work are referred to as subdeposits. Additionally, regional DMDs are generally located near mare-filled basins and superimposed on highlands materials, while localized DMDs are often associated with fissures in large, Imbrian to pre-Imbrian aged floor-fractured craters [Head, 1974; Schultz, 1976; Weitz et al., 1998; Jozwiak et al., 2012]. Emplacement style is believed to vary between these two types of DMDs. Regional DMDs are understood to be the result of hawaiian-style eruptions, characterized by long-duration fire-fountaining events ©2015. American Geophysical Union. [Wilson and Head, 1981], while smaller, localized DMDs are inferred to have formed from sporadic, explosive All Rights Reserved. vulcanian-style eruptions [Head and Wilson, 1979; Hawke et al., 1989]. JAWIN ET AL. SPECTRAL VARIATIONS IN LUNAR LDMDS 1310 Journal of Geophysical Research: Planets 10.1002/2014JE004759 Figure 1. Global distribution of DMDs (white circles) [Gaddis et al., 2003; Gustafson et al., 2012] on a Wide Angle Camera global mosaic. Red stars indicate the location of localized DMDs studied here; yellow stars indicate the location of new localized DMDs identified in this work. Blue dots indicate the location of localized DMDs in Lavoisier and Walther A craters analyzed previously by Souchon et al. [2013] and Besse et al. [2014], respectively. Figure 2. Alphonsus crater. (a) Sketch map with a Kaguya TC evening mosaic as the basemap. (b) M3 1 μm albedo map. DMDs appear dark, and specific subdeposits studied here are labeled (see Table 2 for details on each subunit). (c) RGB color composite image using R: IBD 1000 nm, G: BD 1900 nm, and B: R 1580 nm. (d) RGB color composite image using R: BD 950 nm, G: BD 1050 nm, and B: BD 1250 nm. Spectra of mare basalts and crater floor used in Figure 4d are identified here. Vertical banding in Figure 2c is a residual from the photometric correction [Besse et al., 2013]. JAWIN ET AL. SPECTRAL VARIATIONS IN LUNAR LDMDS 1311 Journal of Geophysical Research: Planets 10.1002/2014JE004759 Collectively, DMDs are believed to represent the eruption of gas-rich magmas from dikes originating from deep within the Moon (>300 km depths), bringing to the surface a key suite of maficmineralswhich crystallized from primitive, unfractionated magmas [Delano and Livi, 1981]. Compositional and mineralogical analyses from remote sensing observations and laboratory measurements [Pieters et al., 1973; Adams et al., 1974; Gaddis et al., 1985, 2000, 2003; Hawke et al., 1989; Weitz et al., 1998] have found that DMDs are composed of mafic minerals enriched in iron and titanium with volatile-rich coatings. Many regional DMDs were found to contain large amounts of Fe2+-bearing volcanic glass beads, iron- and titanium-rich glass, and devitrified beads of similarly mafic composition [Pieters et al., 1973; Adams et al., 1974; Gaddis et al., 1985; Lucey et al., 1986; Weitz et al., 1998, 1999]. Iron-rich volcanic glass has also recently been clearly identified using remote sensing observations in localized DMDs [Besse et al., 2014; Horgan et al., 2014]. In addition, chromium-rich spinel has been identified in the Sinus Aestuum DMD [Sunshine et al., 2010, 2014; Yamamoto et al., 2013]. Early studies [Hawke et al., 1989] based on Earth-based telescopic data (1–5 km footprint) proposed three classes of localized DMDs whose major distinctions included the presence of mostly basaltic material, a combination of basalt and wall rock material, and a component of juvenile material including olivine and pyroxene. However, later studies [e.g., Gaddis et al., 2000] using Clementine multispectral data (100–200 m/pixel, 0.415–1.0 μm) did not identify an olivine component in any of the localized deposits studied, with the exception of J. Herschel crater. More recently, Besse
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