Iron abundances on the lunar surface as measured by the Lunar Prospector gamma‐ray and neutron spectrometers

Lawrence, D. J.; Feldman, W. C.; Elphic, R. C.; Little, Robert C.; Prettyman, T. H.; Maurice, S.; Lucey, P. G.; Binder, A. B.

doi:10.1029/2001je001530

Cited by 248 publications

(312 citation statements)

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“…SPA soils exhibit a mafic character and elevated concentrations of Fe and Th are present (compared to the lunar highlands) [e.g., Pieters et al, 1997Pieters et al, , 2001Jolliff et al, 2000;Lawrence et al, 2002Lawrence et al, , 2003. Although the basin contains several mare basalt emplacements, the dominant mafic signature is nonmare and is dominated by low-Ca pyroxene (LCP) [Pieters et al, 1997].…”

Section: The South Pole-aitken Basinmentioning

confidence: 99%

Compositional heterogeneity of central peaks within the South Pole‐Aitken Basin

2013

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[1] Using high-spectral and -spatial resolution Moon Mineralogy Mapper data, we investigate compositional variations across the central peak structures of four impact craters within the South Pole-Aitken Basin (SPA). Two distinct causes of spectral diversity are observed. Spectral variations across the central peaks of Bhabha, Finsen, and Lyman are dominated by soil development, including the effects of space weathering and mixing with local materials. For these craters, the central peak structure is homogeneous in composition, although small compositional differences between the craters are observed. This group of craters is located within the estimated transient cavity of SPA, and their central uplifts exhibit similar mafic abundances. Therefore, it is plausible that they have all uplifted material associated with melts of the lower crust or upper mantle produced during the SPA impact. Compositional differences observed between the peaks of these craters reflect heterogeneities in the SPA subsurface, although the origin of this heterogeneity is uncertain. In contrast to these craters, Leeuwenhoek exhibits compositional heterogeneity across its central peak structure. The peak is areally dominated by feldspathic materials, interspersed with several smaller exposures exhibiting a mafic spectral signature. Leeuwenhoek is the largest crater included in the study and is located in a region of complex stratigraphy involving both crustal (feldspathic) and SPA (mafic melt and ejecta) materials. The compositional diversity observed in Leeuwenhoek's central peak indicates that kilometer-scale heterogeneities persist to depths of more than 10 km in this region.

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Section: The South Pole-aitken Basinmentioning

confidence: 99%

Compositional heterogeneity of central peaks within the South Pole‐Aitken Basin

2013

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“…Among these models, Lucey's model is one of the most popular, following a series of refinements [7][8][9]. Lucey's model is based on the reflectance at 0.75 μm and the ratio of the reflectances at 0.95 μm and 0.75 μm.…”

Section: Algorithm To Derive Feo Abundance 21 Clementine Uvvis Methodsmentioning

confidence: 99%

“…After obtaining data from Clementine, a series of empirical models were developed to predict the FeO content from Clementine's UVVIS images [3][4][5][6][7][8][9]. Among these models, Lucey's model is one of the most popular, following a series of refinements [7][8][9].…”

Section: Algorithm To Derive Feo Abundance 21 Clementine Uvvis Methodsmentioning

confidence: 99%

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Preliminary results of FeO mapping using Imaging Interferometer data from Chang’E-1

et al. 2011

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Information about the variability, and spatial distribution of iron abundance is important to understand lunar geological history and for future resource utilization. In this paper we present a preliminary model to produce an iron abundance map using images taken by an Imaging Interferometer on board the satellite Chang'E-1. Compared with the Clementine UVVIS images, the images from the Chang'E-1 satellite also allowed for the extraction of FeO abundance distributions on the Moon. However, the preliminary model results suggest an underestimation of ~2 wt.% for the FeO content of the mare region and an overestimation of ~3 wt.% for the highland region. Chang'E-1, Imaging Interferometer, FeO mapping, Clementine UVVIS Citation:Ling Z C, Zhang J, Liu J Z, et al. Preliminary results of FeO mapping using Imaging Interferometer data from Chang'E-1.

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“…Early results were obtained for Th and Fe, which have well resolved full energy γ-ray peaks at 2.6 million electron volts (MeV) and 7.6 MeV, respectively (22,23). Accurate determination of the other elements required the development of spectral unmixing techniques (24) (Fig.…”

Section: Examples Of Cosmochemistry Flight Instrumentsmentioning

confidence: 99%

Spacecraft instrument technology and cosmochemistry

McSween

McNutt

Prettyman

2011

Proc. Natl. Acad. Sci. U.S.A.

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Measurements by instruments on spacecraft have significantly advanced cosmochemistry. Spacecraft missions impose serious limitations on instrument volume, mass, and power, so adaptation of laboratory instruments drives technology. We describe three examples of flight instruments that collected cosmochemical data. Element analyses by Alpha Particle X-ray Spectrometers on the Mars Exploration Rovers have revealed the nature of volcanic rocks and sedimentary deposits on Mars. The Gamma Ray Spectrometer on the Lunar Prospector orbiter provided a global database of element abundances that resulted in a new understanding of the Moon's crust. The Ion and Neutral Mass Spectrometer on Cassini has analyzed the chemical compositions of the atmosphere of Titan and active plumes on Enceladus.A nalyses of extraterrestrial materials performed by instruments on spacecraft have revolutionized our understanding of planets and planetesimals, and have driven significant advances in technology. Here we focus on mobile instruments that have made cosmochemical measurements, in keeping with the theme of this issue.The adaptation of laboratory analytical instruments for flight on spacecraft missions poses many challenges. An obvious limitation for flight instruments is scale-mass and volume. Flight instruments must be crafted from light-weight materials, and miniaturization is required to fit into the confines of the spacecraft. Packing multiple instruments together can cause interferences which must be accommodated. Power limitations are often severe: instruments that use kilowatts in the laboratory might have to operate on watts in space. The storage and transmission capacities for data are limited, and onboard data compression may be required. Flight instruments must be durable to withstand the vibrations and g-forces encountered during launch and orbital insertion or landing. The instruments commonly experience extreme temperatures and irradiation by cosmic rays during long periods of interplanetary cruise. Environmental testing of flight instruments before and after they are integrated into the spacecraft system is expensive and time consuming, adding additional pressure to mission cost and schedule.During the last decade, NASA and its international partners have launched numerous spacecraft, many carrying instruments capable of performing chemical analyses. Here we provide an illustrative sampling of three successful cosmochemistry flight instruments, along with discussions of how the data that they acquired have impacted science and technology. The data from these instruments are archived in NASA's Planetary Data System (PDS, http://pds.nasa.gov/) and are available to any interested investigators. Examples of Cosmochemistry Flight Instruments Alpha Particle X-Ray Spectrometers (APXS). The Mars Exploration Rovers (MER) Spirit and Opportunity landed on Mars in 2004.Each rover carried an APXS (1), and these instruments together have analyzed hundreds of rocks and soils. The sensor head (Fig. 1), mounted on the rover arm, is brought ...

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Iron abundances on the lunar surface as measured by the Lunar Prospector gamma‐ray and neutron spectrometers

Cited by 248 publications

References 49 publications

Compositional heterogeneity of central peaks within the South Pole‐Aitken Basin

Compositional heterogeneity of central peaks within the South Pole‐Aitken Basin

Preliminary results of FeO mapping using Imaging Interferometer data from Chang’E-1

Spacecraft instrument technology and cosmochemistry

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