The global distribution of pure anorthosite on the Moon

Ohtake, M.; Matsunaga, Tsuneo; Haruyama, Junichi; Yokota, Yasuhiro; Morota, Tomokatsu; Honda, Chikatoshi; Ogawa, Y.; Torii, M.; Miyamoto, H.; Arai, Tomoko; Hirata, Naru; Iwasaki, Akira; Nakamura, Ryosuke; Hiroi, T.; Sugihara, Takamitsu; Takeda, Hiroshi; Otake, Hisashi; Pieters, C. M.; Saiki, Kazuto; Kitazato, K.; Abe, Masanao; Asada, Naoki; Demura, H.; Yamaguchi, Yasushi; Sasaki, Sho; Kodama, Shinsuke; Terazono, Junya; Shirao, Motomaro; Yamaji, Atsushi; Minami, Shigeyuki; Akiyama, Hiroaki; Josset, Jean-Luc

doi:10.1038/nature08317

Cited by 287 publications

(273 citation statements)

References 24 publications

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“…KAGUYA MI showed evidence of anorthosite in SPA 8) . But spectral data of central peaks of craters inside SPA show ultramafic assemblage dominated by magnesium rich orthopyroxene, suggesting the presence impact melt sheet 9) .…”

Section: South Pole Aitken Basinmentioning

confidence: 96%

Structure of the South Pole-Aitken Basin from KAGUYA Selenodesy Data

Sasaki

Ishihara

Goossens

et al. 2012

AEROSPACE TECHNOLOGY JAPAN

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The South Pole-Aitken basin (SPA) is the largest (2500km in diameter), deepest and presumably oldest impact basin in the solar system. SPA was characterized by an ellipse with axes 2400 by 2050 km, but more precise topography and gravity data are necessary to discuss the structure of large basin like SPA. We use localized representation of gravity potential where Slepian functions were used to estimate the gravity field over certain areas of the Moon and a spherical cap area with a radius of 40 degree from the SPA center. The direction of an ellipse denoting the depression is found to be similar to the previous result. The region with the thinnest crust is offset southward from the center of SPA. We analyzed interior structure of small basins in and around SPA. We interpret that a positive gravity anomaly corresponds to a Moho uplift. Just around the rim of SPA, a distinct Moho uplift beneath Schrödinger corresponds to the presence of olivine and obscure circular structure Amundsen-Ganswindt has a significant Moho uplift, suggesting a buried impact structure.

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Section: South Pole Aitken Basinmentioning

confidence: 96%

Structure of the South Pole-Aitken Basin from KAGUYA Selenodesy Data

Sasaki

Ishihara

Goossens

et al. 2012

AEROSPACE TECHNOLOGY JAPAN

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“…However, a more solid interpretation of the causes for the nearside-farside dichotomy in mare volcanism requires a clearer understanding of the ages, volumes, compositions of mare basalts, and relation to crustal structure. Such clarification will be possible with SELENE multispectral Ohtake et al, 2009), topography (Araki et al, 2009), and gravity (Namiki et al, 2009) data sets.…”

Section: Comparison With the Spa Basin And The Nearsidementioning

confidence: 99%

Timing and duration of mare volcanism in the central region of the northern farside of the Moon

et al. 2011

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Age determinations of lunar mare basalts are essential for understanding the thermal evolution of the Moon. In this study, we performed new crater size-frequency measurements in mare deposits in the central region of the northern farside, consisting of Lacus Luxuriae, Buys-Ballot, Campbell, and Kohlschütter, using high-resolution images obtained by SELENE (Kaguya) Terrain Camera. The estimated model ages of the mare deposits range from 2.7 to 3.5 Ga. On the basis of model ages for all investigated mare deposits in the central part of the northern farside, considering the results of previous studies, we concluded that mare volcanism in this region began at least as early as 3.9 Ga and continued until ∼2.6 Ga. From a comparison of model ages in the region and the South Pole-Aitken basin, we found that mare volcanism in these regions ended at the same time, suggesting that the South Pole-Aitken basin formation impact had a minor effect on mare volcanism in the region.

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“…The Apollo sample collection contains several large, nearly monomineralic plagioclase rocks (e.g. Warren 1990), and outcrops of 'pure' anorthosite have also been identified from Earth-based and spacecraft observations Ohtake et al 2009). However, its perceived importance to lunar crustal formation has been challenged by Lucey et al (2006) because, although ferroan anorthosite is the most common pristine rock type at the Apollo 16 site, it is uncommon or rare at other sites.…”

Section: Igneous Geochemistrymentioning

confidence: 99%

Volcanism and tectonism across the inner solar system: an overview

Platz

Byrne

Massironi

et al. 2014

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Volcanism and tectonism are the dominant endogenic means by which planetary surfaces change. This book, in general, and this overview, in particular, aim to encompass the broad range in character of volcanism, tectonism, faulting and associated interactions observed on planetary bodies across the inner solar system -a region that includes Mercury, Venus, Earth, the Moon, Mars and asteroids. The diversity and breadth of landforms produced by volcanic and tectonic processes are enormous, and vary across the inventory of inner solar system bodies. As a result, the selection of prevailing landforms and their underlying formational processes that are described and highlighted in this review are but a primer to the expansive field of planetary volcanism and tectonism. In addition to this extended introductory contribution, this Special Publication features 21 dedicated research articles about volcanic and tectonic processes manifest across the inner solar system. Those articles are summarized at the end of this review.

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The global distribution of pure anorthosite on the Moon

Cited by 287 publications

References 24 publications

Structure of the South Pole-Aitken Basin from KAGUYA Selenodesy Data

Structure of the South Pole-Aitken Basin from KAGUYA Selenodesy Data

Timing and duration of mare volcanism in the central region of the northern farside of the Moon

Volcanism and tectonism across the inner solar system: an overview

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