Possible mantle origin of olivine around lunar impact basins detected by SELENE

Yamamoto, Sakae; Nakamura, Ryosuke; Matsunaga, Tsuneo; Ogawa, Y.; Ishihara, Yoshiaki; Morota, Tomokatsu; Hirata, Naru; Ohtake, M.; Hiroi, T.; Yokota, Yasuhiro; Haruyama, Junichi

doi:10.1038/ngeo897

Cited by 189 publications

(207 citation statements)

References 25 publications

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“…The fact that troctolite-rich materials are only exposed in crater central peaks suggests that they occur dominantly as intrusive igneous deposits in the lunar crust. Dunite and olivine-rich rocks are also excavated from the crust (Pieters, 1982;Tompkins and Pieters, 1999) and possibly from the mantle during impact basin events (Yamamoto et al, 2010).…”

Section: Discussionmentioning

confidence: 99%

Lunar cryptomaria: Mineralogy and composition of ancient volcanic deposits

Whitten

Head

2015

Planetary and Space Science

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Section: Discussionmentioning

confidence: 99%

Lunar cryptomaria: Mineralogy and composition of ancient volcanic deposits

Whitten

Head

2015

Planetary and Space Science

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“…Taking into account lateral variations in crustal density as implied by remote sensing data, Wieczorek et al [30] varied the mantle density in order to find a global crustal thickness model that fit the recent seismic constraints and that possessed minimum crustal thicknesses close to zero. The thinnest crust was found to occur beneath the Crisium and Moscoviense impact basins, precisely where remote sensing data suggest that the mantle may have been excavated [31]. When using the seismic crustal thickness constraints of 30 and 38 km at the Apollo 12 and 14 landing sites with 12% porosity in the crust, the average crustal thickness was found to be 34 and 43 km, respectively.…”

Section: Thickness Of the Crustmentioning

confidence: 99%

Lunar bulk chemical composition: a post-Gravity Recovery and Interior Laboratory reassessment

Taylor

Wieczorek

2014

Phil. Trans. R. Soc. A.

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New estimates of the thickness of the lunar highlands crust based on data from the Gravity Recovery and Interior Laboratory mission, allow us to reassess the abundances of refractory elements in the Moon. Previous estimates of the Moon fall into two distinct groups: earthlike and a 50% enrichment in the Moon compared with the Earth. Revised crustal thicknesses and compositional information from remote sensing and lunar samples indicate that the crust contributes 1.13–1.85 wt% Al 2 O 3 to the bulk Moon abundance. Mare basalt Al 2 O 3 concentrations (8–10 wt%) and Al 2 O 3 partitioning behaviour between melt and pyroxene during partial melting indicate mantle Al 2 O 3 concentration in the range 1.3–3.1 wt%, depending on the relative amounts of pyroxene and olivine. Using crustal and mantle mass fractions, we show that that the Moon and the Earth most likely have the same (within 20%) concentrations of refractory elements. This allows us to use correlations between pairs of refractory and volatile elements to confirm that lunar abundances of moderately volatile elements such as K, Rb and Cs are depleted by 75% in the Moon compared with the Earth and that highly volatile elements, such as Tl and Cd, are depleted by 99%. The earthlike refractory abundances and depleted volatile abundances are strong constraints on lunar formation processes.

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“…feldspathic and lack obvious signatures of lunar mantle material [Pieters et al, 2009;Yamamoto et al, 2010] as well as by geophysical modelling [Wieczorek and Phillips, 1999;Hikida and Wieczorek, 2007]. If the Cordillera ring radius approximates the radius of the excavation, this would imply an excavation volume of 17.0 × 10 6 km 3 , substantially greater than the ∼2.9 × 10 6 km 3 of ejecta observed within one basin diameter of the Cordillera ring.…”

Section: Ejecta Volumes and Comparisons To Estimated Transient Rim Crmentioning

confidence: 99%

Thickness of proximal ejecta from the Orientale Basin from Lunar Orbiter Laser Altimeter (LOLA) data: Implications for multi-ring basin formation

Fassett

Head

Smith

et al. 2011

Geophys. Res. Lett.

112

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Quantifying the ejecta distribution around large lunar basins is important to understanding the origin of basin rings, the volume of the transient cavity, the depth of sampling, and the nature of the basin formation processes. We have used newly obtained altimetry data of the Moon from the Lunar Orbiter Laser Altimeter (LOLA) instrument to estimate the thickness of ejecta in the region surrounding the Orientale impact basin, the youngest and best preserved large basin on the Moon. Our measurements yield ejecta thicknesses of ∼2900 m near the Cordillera Mountains, the topographic rim of Orientale, decaying to ∼1 km in thickness at a range of 215 km. These measurements imply a volume of ejecta in the region from the Cordillera ring to a radial range of one basin diameter of ∼2.9 × 106 km3 and permit the derivation of an ejecta‐thickness decay model, which can be compared with estimates for the volume of excavation and the size of the transient cavity. These data are consistent with the Outer Rook Mountains as the approximate location of the transient cavity's rim crest and suggest a volume of ∼4.8 × 106 km3 for the total amount of basin ejecta exterior to this location.

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Possible mantle origin of olivine around lunar impact basins detected by SELENE

Cited by 189 publications

References 25 publications

Lunar cryptomaria: Mineralogy and composition of ancient volcanic deposits

Lunar cryptomaria: Mineralogy and composition of ancient volcanic deposits

Lunar bulk chemical composition: a post-Gravity Recovery and Interior Laboratory reassessment

Thickness of proximal ejecta from the Orientale Basin from Lunar Orbiter Laser Altimeter (LOLA) data: Implications for multi-ring basin formation

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