Preliminary results of TiO2 mapping using Imaging Interferometer data from Chang’E-1

Ling, Zongcheng; Jiang, Zhang; Liu, Jianzhong; Zhang, Wenxi; Zhang, GuangLiang; Liu, Bin; Ren, Xin; Mu, Lingli; Liu, Jing; Li, Chunlai

doi:10.1007/s11434-011-4550-8

Cited by 19 publications

(6 citation statements)

References 28 publications

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“…From the above discussion, a couple of significant points can be summarized. First, there is a strong correlation between the average atomic number and the concentration of iron in maria regions, which is confirmed by gamma‐ray spectra (Feldman et al, 2002; Lawrence et al, 2002), neutron spectra (Elphic et al, 2002, 1998, 2000), and multispectral analysis (Ling ZC et al, 2011; Yan BX et al, 2012). Second, there some high Z A value spots surrounding the maria and scattered throughout the Moon.…”

Section: Average Atomic Number Of Rock and Soil On Lunar Surfacementioning

confidence: 79%

Mapping of the lunar surface by average atomic number based on positron annihilation radiation from Chang’e-1

Zhao

Zhang

et al. 2018

Earth and Planetary Physics

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A map of the average atomic number of lunar rock and soil can be used to differentiate lithology and soil type on the lunar surface. This paper establishes a linear relationship between the average atomic number of lunar rock or soil and the flux of position annihilation radiation (0.512‐MeV gamma‐ray) from the lunar surface. The relationship is confirmed by Monte Carlo simulation with data from lunar rock or soil samples collected by Luna (Russia) and Apollo (USA) missions. A map of the average atomic number of the lunar rock and soil on the lunar surface has been derived from the Gamma‐Ray Spectrometer data collected by Chang’e‐1, an unmanned Chinese lunar‐orbiting spacecraft. In the map, the higher average atomic numbers (ZA > 12.5), which are related to different types of basalt, are in the maria region; the highest ZA (13.2) readings are associated with Sinus Aestuum. The middle ZA (~12.1) regions, in the shape of irregular oval rings, are in West Oceanus Procellarum and Mare Frigoris, which seems to be consistent with the distribution of potassium, rare earth elements, and phosphorus as a unique feature on the lunar surface. The lower average atomic numbers (ZA < 11.5) are found to be correlated with the anorthosite on the far side of the Moon.

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Section: Average Atomic Number Of Rock and Soil On Lunar Surfacementioning

confidence: 79%

Mapping of the lunar surface by average atomic number based on positron annihilation radiation from Chang’e-1

Zhao

Zhang

et al. 2018

Earth and Planetary Physics

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“…Mapping the quantity of ilmenite (FeTiO 3 ) in lunar mare basalts and soils is an essential component of lunar exploratory geological researches and prospective resource usage sources for lunar oxygen (Allen et al 1994;Ling et al 2011). The TiO 2 content distribution of mare deposits is consistent with their source regions (mare cumulates), the cumulate from the LMO coupled with dynamic sinking and dense mixing of Ti-rich, Ferich late-stage cumulates finally rising as Mg-rich early cumulates or undifferentiated rock (Dowty 1975;Herbert 1980;Ryder 1991;Hess & Parmentier 1995;Giguere et al 2000).…”

Section: Tio 2 Mappingmentioning

confidence: 99%

“…Charette et al (1974) created the first Ti elemental concentration map from mature mare soils by correlating the UV/VIS spectral ratio, and this approach was then used and refined by others (Blewett et al 1997;Lucey et al 1998Lucey et al , 2000aLucey et al , 2000b. The TiO 2 content of the Mare Moscoviense basin was mapped in this work utilizing the Ling et al (2011) parameter that was altered and applied on the 540 nm and 750 nm bands. Figure 8…”

Section: Tio 2 Mappingmentioning

confidence: 99%

Mapping of Compositional Diversity and Chronological Ages of Lunar Farside Multiring Mare Moscoviense Basin: Implications to the Middle Imbrian Mare Basalts

Karthi

Arivazhagan²,

Sharma³

2022

Res. Astron. Astrophys.

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The Mare Moscoviense is an astonishing rare flatland multi-ring basin and one of the recognizable mare regions on Moon’s farside. The mineralogical, chronological, topographical, and morphological studies of maria surface of the Moon provide a primary understanding of the origin and evolution of the mare provinces. In this study, the Chandrayaan-1- M3 data have been employed to prepare optical maturity index, FeO and TiO2 concentration, and standard band ratio map to detect the mafic indexes like olivine and pyroxene minerals. Crater size frequency distribution method has been applied LROC WAC data to obtain the absolute model ages of the Moscoviense basin. The four geological unit ages were observed as 3.57 Ga (U-2), 3.65 Ga (U-1), 3.8 Ga (U-3), 3.92 Ga (U-4), which could have been formed between Imbrain to Nectarian epoch. The M3 imaging and reflectance spectral parameters were used to reveal the minerals like pyroxene, olivine, ilmenite, plagioclase, orthopyroxene-olivine-spinel lithology, and olivine-pyroxene mixtures present in the gabbroic basalt, anorthositic, and massive ilmenite rocks and validated with the existing database. The results show that the Moscoviense basin is dominated by intermediate TiO2 basalts that derived from ol

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“…It has been a very effective tool to use visible and near-infrared spectroscopy technology to derive the surface material composition and distribution. It can not only obtain the content and distribution of some useful elements, such as Fe, Ti, Mg, and Al (Lucey et al 1998(Lucey et al , 2000Ling et al 2011aLing et al , 2011bWu et al 2012;Yan et al 2012;Lu et al 2021) but also the content and distribution of some composed minerals, such as pyroxene, plagioclase, olivine and ilmenite Pieters 2002;Shkuratov 2003;Shuai et al 2013). However, there are still many uncertainties in the identification and quantification of the minerals on lunar surface.…”

Section: Introductionmentioning

confidence: 99%

Detection Capability Evaluation of Lunar Mineralogical Spectrometer: Results from Ground Experimental Data

Gao,

Liu,

Ren

et al. 2023

Res. Astron. Astrophys.

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Chang’E-6 mission willfirstlandon the far side ofthe moon andbring lunar samples back. as a hyperspectral imager aboard the Chang’E-6 lander, the Lunar Mineralogical Spectrometer (LMS), will achieve the goalof spectral detection and mineral composition analysis in sampling area, the data of LMS will alsobe compared with the results of the returned sample laboratory measurements.The visible and near-infrared hyperspectral remote sensing is an effective tool for lunar minerals identification and quantification. Ground validation experiment can be used to evaluate the detection ability of LMS. According to the modal abundances of lunar minerals and glasses ofAPOLLOsamples, binary mixed samples, ternary mixed samples and seven-membered mixed samples were prepared. The samples were ground and stirred homogeneous to about 200 mesh (median particle size about 75μm), to simulate the soil state of lunar surface. Under the laboratory ambient condition, the 480-3200 nm spectral data of the samples were acquired using the Engineering Qualification Model (EQM) of Chang’E-5 LMS, the performance of which is consistent with theflight model of Chang’E-6 LMS. By fitting the mixed samples’ spectral data of the EQM using the Modified Gaussian Methods (MGM), the following conclusions can be drawn：The subtle spectral changes of mixed samples can be detected. The modal abundance of low-Ca pyroxene, high- Ca pyroxene and plagioclase can be derived based on the spectral parameters such as absorption position, depth or width of the mixed samples, and the correlation coefficient R2 are better than 82%, indicating that the LMS has good quantitative detection capability.

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Preliminary results of TiO2 mapping using Imaging Interferometer data from Chang’E-1

Cited by 19 publications

References 28 publications

Mapping of the lunar surface by average atomic number based on positron annihilation radiation from Chang’e-1

Mapping of the lunar surface by average atomic number based on positron annihilation radiation from Chang’e-1

Mapping of Compositional Diversity and Chronological Ages of Lunar Farside Multiring Mare Moscoviense Basin: Implications to the Middle Imbrian Mare Basalts

Detection Capability Evaluation of Lunar Mineralogical Spectrometer: Results from Ground Experimental Data

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