Lunar cryptomaria: Mineralogy and composition of ancient volcanic deposits

Whitten, J. L.; Head, J. W.

doi:10.1016/j.pss.2014.11.027

Cited by 44 publications

(66 citation statements)

References 66 publications

(112 reference statements)

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“…of the M 3 data used for checking each potential cryptomare DHC are shown in Table 3. Moreover, the DHC with the ID 18 in this work was also identified as a cryptomare DHC in Whitten and Head (2015b). Hawke et al (2005) suggested 25 DHCs with the percentage of mare basalt varying from 49.3% to 81.7%.…”

Section: Journal Of Geophysical Research: Planetssupporting

confidence: 52%

“…The three mare basalt splits B1a, B1b, and B6 of the lunar meteorite Northeast Africa (NEA) 001 have the FeO contents 16.54, 12.21, and 13.64 wt%, respectively (Snape et al, 2011). The other method employed the diagnostic spectra of high-Ca pyroxene (e.g., Kaur et al, 2013;Whitten & Head, 2015b) or used both the high-Ca pyroxene and the high FeO abundances as the criteria of mare basalts (e.g., Giguere et al, 2006;Hawke et al, 2015). With regard to the magnesian suite, the gabbronorite 67667,3 has a FeO concentration of 17.1 wt% (Warren & Wasson, 1979;Wieczorek et al, 2006).…”

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confidence: 99%

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Lunar Cryptomare: New Insights Into the Balmer‐Kapteyn Region

Wang

Qiu

2018

JGR Planets

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Cryptomaria record the early mare volcanisms and put important constraints on the lunar thermal and volcanic history and on the early partial melting of the mantle. This work focuses on the representative cryptomare region of Balmer‐Kapteyn and employs multisource exploration data including Lunar Reconnaissance Orbiter Camera Wide Angle Camera, Lunar Reconnaissance Orbiter Camera Narrow Angle Camera, Lunar Orbiter Laser Altimeter Digital Elevation Model (DEM), GLD 100, Chang'E‐1 Interference Imaging Spectrometer, Moon Mineralogy Mapper, Clementine, and Lunar Prospector Gamma‐Ray and Neutron Spectrometers data to provide new insights into the distribution, geometry, buried depth, space weathering, chemical compositions, lithology, and mineralogy of the cryptomare in the Balmer‐Kapteyn region. Some viewpoints are primarily as follows. (1) Cryptomare may widely occur in the Balmer‐Kapteyn region with various small and separate exposure areas. The lithology in this region has an obvious north‐south dichotomy. Alkali suite may dominate the northern region, responsible for the local Th enhancement, whereas ferroan anorthosite suite and magnesian suite may spread over the southern part. Cryptomare may occur in both the north and the south, with most exposures within the craters dominated by alkali suite or ferroan anorthosite suite. (2) The buried depths of the cryptomare may fall into the range from at least ~33 m to at least ~1,849 m. Thus, the buried thickness may be more than ~1.8 km. (3) The buried mare basalts in this region are member of the high‐alumina type and a previously unsampled new type of high‐alumina mare basalts may be revealed. (4) At least two periods of mare volcanisms or at least an intrusion of basaltic lava may have happened in this region. The erupted or intruded mare basalts in the later period are more abundant in Al but relatively poor in Fe, Ti, Ca, and Mg, and some of them were buried or intruded much shallowly (~33 m) under the surface ejecta.

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Section: Journal Of Geophysical Research: Planetssupporting

confidence: 52%

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confidence: 99%

Lunar Cryptomare: New Insights Into the Balmer‐Kapteyn Region

Wang

Qiu

2018

JGR Planets

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“…Sometimes, the strength and position of the absorption spectra near 2800 nm region may be due to illumination and thermal conditions. Recent studies confirm that the strength of the OH/H 2 O feature does not vary in different date M 3 images and under sun illumination condition of spectra (e.g., Cheek et al, 2011;Chauhan and Kaur, 2014) with no significant shift in absorption band (Whitten and Head, 2015). Olivine rich area is located in the southern edge of the inner ring of the basin.…”

Section: Moscoviense Basin -(Sample Site 3)mentioning

confidence: 79%

“…1), respectively. The coverage of the M 3 level-2 data for the sample sites are restricted to the single optical period, as there is no significant absorption band shift in different optical period images due to sensor thermal effect (Whitten and Head, 2015). The RELAB lab spectra (Fig.…”

Section: Data Acquisitionmentioning

confidence: 99%

Lunar surface mineralogy using hyperspectral data: Implications for primordial crust in the Earth–Moon system

Sivakumar

Neelakantan

Santosh

2017

Geoscience Frontiers

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a b s t r a c t Mineralogy of the Lunar surface provides important clues for understanding the composition and evolution of the primordial crust in the EartheMoon system. The primary rock forming minerals on the Moon such as pyroxene, olivine and plagioclase are potential tools to evaluate the Lunar Magma Ocean (LMO) hypothesis. Here we use the data from Moon Mineralogy Mapper (M 3 ) onboard the Chandrayaan-1 project of India, which provides Visible e Near Infra Red (NIR) spectral data (hyperspectral data) of the Lunar surface to gain insights on the surface mineralogy. Band shaping and spectral profiling methods are used for identifying minerals in four sites: Moscoviense Basin, Orientale Basin, Apollo Basin and Wegener Crater e highland. The common presence of plagioclase is in conformity with the anorthositic composition of the Lunar crust. Pyroxenes, olivine and Fe-Mg-spinel from the sample sites indicate the presence of gabbroic and basaltic components. The compositional difference in pyroxenes suggests magmatic differentiation on the Lunar surface. Olivine contains OH/H 2 O band, indicating hydrous phase in the primordial magmas. Ó 2016, China University of Geosciences (Beijing) and Peking University. Production and hosting by Elsevier B.V. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/ licenses/by-nc-nd/4.0/).

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“…The global means of the kriged RBA/ D c and ϕ c are the same as those of original crater data, while the standard deviations decrease to 0.14 mGal/km and 4%, as the kriging processes have removed the spatially random signals. In the highlands, the southern part of South Pole‐Aitken (SP‐A) is associated with the largest negative RBA/ D c of −0.44 ± 0.10 mGal/km and the lowest ϕ c of 4 ± 3% (all errors are the standard errors of the kriged values), suggesting that the local craters probe the impact melt sheet (Hurwitz & Kring, ; Vaughan et al, ) underlying a relatively thin porous top layer (Besserer et al, ), although we cannot exclude the effects of impact‐induced porosity decrease and postimpact magmatism (Shearer et al, ; Whitten & Head, ). The north‐south asymmetry of the SP‐A basin might be due to enhanced impact melting in the southern half of the basin caused by an oblique impact from north to south with its first contact near the Ingenii basin (Garrick‐Bethell & Zuber, ; Petro, ; Schultz & Crawford, ).…”

Section: Resultsmentioning

confidence: 99%

Constraints on Lunar Crustal Porosity From the Gravitational Signature of Impact Craters

et al. 2018

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Based on Gravity Recovery and Interior Laboratory (GRAIL) observations and the Lunar Orbiter Laser Altimeter (LOLA) crater database, we constrain the spatial variations in the Moon's crustal porosity (ϕc) to a depth of several kilometers using the gravity anomalies of 4,864 midsized craters (those with a diameter of 20–100 km). For each crater, we estimated the local ϕc by quantifying the gravitational effects of impact‐induced porosity change and postimpact breccia infill. The crustal porosity model was uniquely determined assuming a global mean ϕc of 12%, although a trade‐off exists between the porosity of postimpact breccia infill and the (preimpact) crustal porosity that results in zero net porosity change underlying the crater floor. At this crustal porosity the effects of impact bulking and compaction compensate each other to yield zero crater residual Bouguer anomaly (RBA), when the effect of postimpact infill is excluded. For lower crustal porosities, bulking dominates to produce a negative RBA; for higher crustal porosities, compaction dominates to produce a positive RBA. Spatial kriging and statistical tests suggest lower‐than‐average ϕc in the western nearside maria and southern South Pole‐Aitken (SP‐A) basin, in contrast to higher‐than‐average values in the southwestern periphery of the nearside maria. Most of the large impact basins, presumably formed before the majority of the midsized craters we analyzed, show reduced porosities relative to their immediate surroundings.

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Lunar cryptomaria: Mineralogy and composition of ancient volcanic deposits

Cited by 44 publications

References 66 publications

Lunar Cryptomare: New Insights Into the Balmer‐Kapteyn Region

Lunar Cryptomare: New Insights Into the Balmer‐Kapteyn Region

Lunar surface mineralogy using hyperspectral data: Implications for primordial crust in the Earth–Moon system

Constraints on Lunar Crustal Porosity From the Gravitational Signature of Impact Craters

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