Remote sensing studies of the terrain northwest of Humorum Basin

Hawke, B. R.; Peterson, C. A.; Lucey, P. G.; Taylor, G. J.; Blewett, D. T.; Campbell, B. A.; Coombs, C. R.; Spudis, P. D.

doi:10.1029/92gl02921

Cited by 36 publications

(49 citation statements)

References 9 publications

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“…Initially analyses were carried out for 25 regions previously recognized as cryptomaria (Fig. 4, Table 1) Spudis, 1979, 1983;Hawke and Spudis, 1980;Hawke and Bell, 1981;Bell and Hawke, 1984;Hawke et al, 1985Hawke et al, , 1993Hawke et al, , 2002Hawke et al, , 2005Hawke et al, , 2013Head et al, 1993;Blewett et al, 1995;Mustard and Head, 1996;Antonenko, 1999a,b;Giguere et al, 2003;Campbell and Hawke, 2005;Lawrence et al, 2008). Of these 25 proposed locations, only 20 were confirmed in this study (see Section 4.1.…”

Section: Methodsmentioning

confidence: 90%

Lunar cryptomaria: Physical characteristics, distribution, and implications for ancient volcanism

Whitten

Head

2015

Icarus

110

147

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Section: Methodsmentioning

confidence: 90%

Lunar cryptomaria: Physical characteristics, distribution, and implications for ancient volcanism

Whitten

Head

2015

Icarus

110

147

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“…Anorthosites-Anorthosites (labeled "A" in our classification scheme) have no detectable mafic minerals and are comparable to those traditionally identified as anorthosites in NIR spectra (Hawke et al, 1992bPieters et al, 1996a). Because reflectance spectra are sensitive to very small amounts of mafic minerals in an anorthositic rock, "A" rocks are believed to contain 4 0 % mafic minerals (Pieters, 1986).…”

Section: Central Peaks Lithologiesmentioning

confidence: 96%

Mineralogy of the lunar crust: Results from Clementine

Tompkins

Pieters

1999

Meteorit & Planetary Scien

290

313

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Abstract-The central peaks of 109 impact craters across the Moon are examined with Clementine ultraviolet-visible (UVVIS) camera multispectral data. The craters range in diameter from 40 to 180 km and are believed to have exhumed material from 5-30 km beneath the surface to form the peaks, including both upper and lower crustal rocks depending on whether craters have impacted into highlands or basins. Representative five-color spectra from spectrally and spatially distinct areas within the peaks are classified using spectral parameters, including "key ratio" (which is related to mafic mineral abundance) and "spectral curvature" (linked to absorption band shape, which distinguishes between low-and high-Ca pyroxene and olivine). The spectral parameters are correlated to mineralogical abundances, related in turn to highland plutonic rock compositions. The derived rock compositions for the various central peaks are presented in a global map. From these results, it is evident that the lunar crust is compositionally diverse, both globally and at local 100 m scales found within individual sets of central peaks. Although the central peaks compositions imply a crust that is generally consistent with previous models of crustal structure, they also indicate a more anorthositic crust than generally assumed, with a bulk plagioclase content of -8 1%, evolving from "pure" anorthosite near the surface towards more mafic, low-Ca pyroxene-rich compositions with depth (comparable to anorthositic norite). Evidence for mafic plutons occurs in both highlands and basins and represent all mafic highland rock types. However, the lower crust is more compositionally diverse than the highlands, with both a greater range of rock types and more diversity within individual sets of central peaks.

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“…These zones correspond, in part, to small fresh craters for which spectral reflectance data from Earth-based telescopes show no mafic absorption [Hawke et al, 1991[Hawke et al, , 1993. Hawke and coworkers interpreted the spectra to indicate the presence of pure anorthosite deposits.…”

Section: Geologic Settingmentioning

confidence: 99%

Compositional studies of the Orientale, Humorum, Nectaris, and Crisium lunar basins

Bussey¹,

Spudis²

2000

J. Geophys. Res.

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Abstract. We have used full-resolution (250 m/pixel) Clementine images to map the compositions of ejecta from four multiring basins on the Moon: Orientale, Humorurn, Nectaris, and Crisium. All basins have relatively feldspathic ejecta, with iron contents ranging from 2 to 6 wt % Fee. Some basins show remarkably homogeneous ejecta blankets (Orientale), while others display distinct compositional zoning within exterior sectors of the basin (Crisium); in some cases this zoning correlates with morphologically observed ejecta facies (Nectaris). The iron-poor composition of most basin ejecta indicates that the crust of the Moon at these locations is feldspathic down to depths of at least several tens of kilometers, the likely sampling depth of basin-forming impacts. The inner rings of all four basins display massifs and small crater floors of nearly pure anorthosite (Fee < 1 wt %), virtually the only such occurrences of this rock type on the Moon. Because basin rings are structurally emplaced topographic elements derived from depths of at least 10-20 km into the Moon, we postulate that basin inner rings are sampling a unique stratigraphic level in the Moon and at these depths, the primordial, pristine anorthositic crust of the Moon is largely preserved. Below this zone of anorthosite is the more mafic region of the lower crust, probably having "highland basalt" composition (Fee -10 wt %, A12e 3 -18-22 wt %). The petrologic nature of lower crustal levels remains uncertain but must at least in part include members of the mafic highland suite, such as norites and troctolites. IntroductionThe formation of impact basins has had a profound effect in shaping the Moon. These impacts excavated vast amounts of material and redistributed it across the lunar surface. We are using basins as probes to build up a three-dimensional picture of the crust. By studying the variations in composition of basin ejecta deposits, we have the opportunity to look "into" the crust of the Moon to learn about its makeup and origin. In this paper we discuss the results of a study of several nearside impact basins using the Clementine multispectral data set. The Clementine mission has given us complete coverage of the Moon, allowing all exposed basin ejecta to be characterized. Moreover, the newly developed techniques

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Remote sensing studies of the terrain northwest of Humorum Basin

Cited by 36 publications

References 9 publications

Lunar cryptomaria: Physical characteristics, distribution, and implications for ancient volcanism

Lunar cryptomaria: Physical characteristics, distribution, and implications for ancient volcanism

Mineralogy of the lunar crust: Results from Clementine

Compositional studies of the Orientale, Humorum, Nectaris, and Crisium lunar basins

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