Mineralogy of young lunar mare basalts: Assessment of temporal and spatial heterogeneity using M3 data from Chandrayaan-1

Varatharajan, Indhu; Srivastava, Neeraj; Murty, S. V. S.

doi:10.1016/j.icarus.2014.03.045

Cited by 34 publications

(17 citation statements)

References 48 publications

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“…The olivine abundances in the other maria are slightly lower (5%-6%) and show variations between 4% and 4.5% in the highlands. Several of the areas in Oceanus Procellarum indicated as olivine-rich in our map have also been found to have a high olivine content in (Varatharajan et al, 2014, Staid et al, 2016. The high-olivine basalts of western Oceanus Procellarum and western Mare Imbrium have also been mapped by (Lucey, 2004), however, with olivine abundances of 40%-50%.…”

Section: Resultssupporting

confidence: 57%

Spectral Unmixing Based Construction of Lunar Mineral Abundance Maps

Bernhardt

Grumpe

Wöhler

2017

Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci.

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ABSTRACT:In this study we apply a nonlinear spectral unmixing algorithm to a nearly global lunar spectral reflectance mosaic derived from hyperspectral image data acquired by the Moon Mineralogy Mapper (M 3 ) instrument. Corrections for topographic effects and for thermal emission were performed. A set of 19 laboratory-based reflectance spectra of lunar samples published by the Lunar Soil Characterization Consortium (LSCC) were used as a catalog of potential endmember spectra. For a given spectrum, the multi-population population-based incremental learning (MPBIL) algorithm was used to determine the subset of endmembers actually contained in it. However, as the MPBIL algorithm is computationally expensive, it cannot be applied to all pixels of the reflectance mosaic. Hence, the reflectance mosaic was clustered into a set of 64 prototype spectra, and the MPBIL algorithm was applied to each prototype spectrum. Each pixel of the mosaic was assigned to the most similar prototype, and the set of endmembers previously determined for that prototype was used for pixel-wise nonlinear spectral unmixing using the Hapke model, implemented as linear unmixing of the singlescattering albedo spectrum. This procedure yields maps of the fractional abundances of the 19 endmembers. Based on the known modal abundances of a variety of mineral species in the LSCC samples, a conversion from endmember abundances to mineral abundances was performed. We present maps of the fractional abundances of plagioclase, pyroxene and olivine and compare our results with previously published lunar mineral abundance maps.

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Section: Resultssupporting

confidence: 57%

Spectral Unmixing Based Construction of Lunar Mineral Abundance Maps

Bernhardt

Grumpe

Wöhler

2017

Int. Arch. Photogramm. Remote Sens. Spatial Inf. Sci.

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“…We find that the spectra from CE3-0005 and CE3-0008 sites have wide and strong 1 μm absorption bands but shallow 2 μm band depths ( Fig. 3a,b ), thus they should have a higher 1–2μm band area ratio (BAR), which implies the presence of a significant amount of olivine in the soils of these two sites 15 21 22 23 . The absorption components of all four continuum-removed spectra ( Fig.…”

Section: Resultsmentioning

confidence: 93%

Correlated compositional and mineralogical investigations at the Chang′e-3 landing site

et al. 2015

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The chemical compositions of relatively young mare lava flows have implications for the late volcanism on the Moon. Here we report the composition of soil along the rim of a 450-m diameter fresh crater at the Chang′e-3 (CE-3) landing site, investigated by the Yutu rover with in situ APXS (Active Particle-induced X-ray Spectrometer) and VNIS (Visible and Near-infrared Imaging Spectrometer) measurements. Results indicate that this region's composition differs from other mare sample-return sites and is a new type of mare basalt not previously sampled, but consistent with remote sensing. The CE-3 regolith derived from olivine-normative basaltic rocks with high FeO/(FeO+MgO). Deconvolution of the VNIS data indicates abundant high-Ca ferropyroxene (augite and pigeonite) plus Fe-rich olivine. We infer from the regolith composition that the basaltic source rocks formed during late-stage magma-ocean differentiation when dense ferropyroxene-ilmenite cumulates sank and mixed with deeper, relatively ferroan olivine and orthopyroxene in a hybridized mantle source.

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“…The spectral features of mare basalts were preferentially extracted from fresh craters to avoid the detrimental effects of space weathering [ Kramer , ; Kaur et al ., ], which lowers albedo, weakens band absorption, and reddens the spectral slope of lunar minerals [ McCord and Adams , ; Pieters et al ., ]. Previously, researchers have extracted spectra from small, fresh craters with diameters of about 1 km [ Kaur et al ., ; Varatharajan et al ., ] to analyze their compositions. However, as mentioned above, the thickness of the late stage basalt flows was estimated to be less than 60 m [ Hiesinger et al ., , ].…”

Section: Methodsmentioning

confidence: 99%

Mineralogical variation of the late stage mare basalts

Zhang

Bugiolacchi

et al. 2016

JGR Planets

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The last major phases of lunar volcanism occurred mainly in Oceanus Procellarum and Mare Imbrium and produced spectrally unique medium‐ and high‐titanium basalts. The composition and distribution of these basalts provide a record of the late stage thermal evolution of the Moon. To study the spectral and mineralogical variations of the late stage mare basalts, 31 distinct units were mapped employing a range of remote sensing data. Their inferred mineralogical characteristics were studied by analyzing the spectral features of small, fresh craters derived from the Moon Mineralogy Mapper (M3) data. The strongest olivine spectral signatures were found around Lichtenberg crater, while the units with the lowest olivine/pyroxene ratio occurred mainly in the southern Kepler crater and some local areas. In Oceanus Procellarum, the olivine/pyroxene ratio decreases progressively from the Lichtenberg crater to the southern units. The northern and southern units within Mare Imbrium have higher olivine/pyroxene ratios than the central ones. The inferred abundance of olivine appears to vary stratigraphically, with the younger flows being more olivine rich. However, the stratigraphically younger units around Euler crater in Mare Imbrium, which present as dark red hues in the integrated band depth image of M3, were found to have lower olivine/pyroxene ratios than the units around Lichtenberg crater (shown as light red hues) in Oceanus Procellarum. It could be interpreted that the late stage mare basalts around Lichtenberg crater originated from a more olivine‐rich source than those around Euler crater.

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Mineralogy of young lunar mare basalts: Assessment of temporal and spatial heterogeneity using M3 data from Chandrayaan-1

Cited by 34 publications

References 48 publications

Spectral Unmixing Based Construction of Lunar Mineral Abundance Maps

Spectral Unmixing Based Construction of Lunar Mineral Abundance Maps

Correlated compositional and mineralogical investigations at the Chang′e-3 landing site

Mineralogical variation of the late stage mare basalts

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