Other
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p11b1344g&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P11B-1344
Other
[5464] Planetary Sciences: Solid Surface Planets / Remote Sensing, [5470] Planetary Sciences: Solid Surface Planets / Surface Materials And Properties, [5480] Planetary Sciences: Solid Surface Planets / Volcanism, [6250] Planetary Sciences: Solar System Objects / Moon
Scientific paper
Clementine color (ultraviolet, visible or UVVIS) and Lunar Reconnaissance Orbiter (LRO) Wide Angle (WAC) and Narrow Angle (NAC) camera data provide the means to investigate localized lunar dark-mantle deposits (DMDs) of potential pyroclastic origin. Our goals are to (1) examine the morphology and physical characteristics of these deposits with LROC WAC and NAC data; (2) extend methods used in earlier studies of lunar DMDs with Clementine spectral reflectance (CSR) data; (3) use LRO WAC multispectral data to complement and extend the CSR data for compositional analyses; and (4) apply these results to identify the likely mode of emplacement and study the diversity of compositions among these deposits. Pyroclastic deposits have been recognized all across the Moon, identified by their low albedo, smooth texture, and mantling relationship to underlying features. Gaddis et al. (2003) presented a compositional analysis of 75 potential lunar pyroclastic deposits (LPDs) based on CSR measurements. New LRO camera (LROC) data permit more extensive analyses of such deposits than previously possible. Our study began with six sites on the southeastern limb of the Moon that contain nine of the cataloged 75 potential pyroclastic deposits: Humboldt (4 deposits), Petavius, Barnard, Abel B, Abel C, and Titius. Our analysis found that some of the DMDs exhibit qualities characteristic of fluid emplacement, such as flat surfaces, sharp margins, embaying relationships, and flow textures. We conclude that the localized DMDs are a complex class of features, many of which may have formed by a combination of effusive and pyroclastic emplacement mechanisms. We have extended this analysis to include additional localized DMDs from the catalog of 75 potential pyroclastic deposits. We have examined high resolution (up to 0.5 m/p) NAC images as they become available to assess the mode of emplacement of the deposits, locate potential volcanic vents, and assess physical characteristics of the DMDs such as thickness, roughness, and rock abundance. Within and around each DMD, the Clementine UVVIS multispectral mosaic (100 m/p, 5 bands at 415, 750, 900, 950, and 1000 nm) and LROC WAC multispectral image cubes (75 to 400 m/p, 7 bands at 320, 360, 415, 565, 605, 645, and 690 nm) have been used to extract spectral reflectance data. Spectral ratio plots were prepared to compare deposits and draw conclusions regarding compositional differences, such as mafic mineral or titanium content and distribution, both within and between DMDs. The result of the study will be an improved classification of these deposits in terms of emplacement mechanisms and composition, including identifying compositional affinities among DMDs and between DMDs and other volcanic deposits.
Bell Jon F.
Gaddis Lisa R.
Gustafson O.
Hawke Bernard Ray
LROC Science Team
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