Compositional and chronological characterization of mare crisium using Chandrayaan-1 and LROC-WAC data

Arivazhagan, S.; Karthi, A.

doi:10.1016/j.pss.2018.06.010

Cited by 6 publications

(9 citation statements)

References 45 publications

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“…Mare Crisium is chosen as one of the four landing areas for the LGN mission, because it is an ideal location for constraining the thermal structure of the mantle away from the PKT. Heat flow through the surface of the basin should be least affected by the radiogenic heat production within the thin (∼10 km), mafic crust (Wieczorek et al 2013;Arivazhagan & Karthi 2018). In narrowing down the potential area for landing, we start with the area inside the 10 km crustal thickness contour (Figure 8).…”

Section: Mare Crisium Detailed Site Survey-case Studymentioning

confidence: 99%

The Lunar Geophysical Network Landing Sites Science Rationale

Haviland¹,

Weber²,

Neal³

et al. 2022

Planet. Sci. J.

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The Lunar Geophysical Network (LGN) mission is proposed to land on the Moon in 2030 and deploy packages at four locations to enable geophysical measurements for 6–10 yr. Returning to the lunar surface with a long-lived geophysical network is a key next step to advance lunar and planetary science. LGN will greatly expand our primarily Apollo-based knowledge of the deep lunar interior by identifying and characterizing mantle melt layers, as well as core size and state. To meet the mission objectives, the instrument suite provides complementary seismic, geodetic, heat flow, and electromagnetic observations. We discuss the network landing site requirements and provide example sites that meet these requirements. Landing site selection will continue to be optimized throughout the formulation of this mission. Possible sites include the P-5 region within the Procellarum KREEP Terrane (PKT; (lat: 15°; long: −35°), Schickard Basin (lat: −44.°3; long: −55.°1), Crisium Basin (lat: 18.°5; long: 61.°8), and the farside Korolev Basin (lat: −2.°4; long: −159.°3). Network optimization considers the best locations to observe seismic core phases, e.g., ScS and PKP. Ray path density and proximity to young fault scarps are also analyzed to provide increased opportunities for seismic observations. Geodetic constraints require the network to have at least three nearside stations at maximum limb distances. Heat flow and electromagnetic measurements should be obtained away from terrane boundaries and from magnetic anomalies at locations representative of global trends. An in-depth case study is provided for Crisium. In addition, we discuss the consequences for scientific return of less than optimal locations or number of stations.

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Section: Mare Crisium Detailed Site Survey-case Studymentioning

confidence: 99%

The Lunar Geophysical Network Landing Sites Science Rationale

Haviland¹,

Weber²,

Neal³

et al. 2022

Planet. Sci. J.

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“…Using Clementine data, Lucey et al (1998) and Lucey et al (2000aLucey et al ( , 2000b produced several ratio combinations for distinguishing lithological variances on the lunar surface. The SBR approach was utilized by Arivazhagan & Anbazhagan (2012); Arivazhagan & Karthi (2018) and Karthi & Arivazhagan (2022) to differentiate the diverse lithologies of the Apollo 17 landing area, Mare Crisium basin and Mare Orientale basin, respectively. To differentiate distinct lithologies in the basin, M 3 data have been utilized to produce the SBR map using band combinations of R-750 nm/540 nm, G-750/950 nm and B-540 nm/750 nm.…”

Section: Standard Band Ratio (Sbr)mentioning

confidence: 99%

“…Absorption features of 1 μm and 2 μm are the primary resources for evaluating lunar surface mineralogy, particularly for mafic minerals like olivine and pyroxenes (Burns 1993;Isaacson et al 2013;Arivazhagan & Karthi 2018;Salem et al 2022). The Integrated Band Depth (IBD) defines the band depths of absorption characteristics at 1 μm and 2 μm to distinguish spectral differences related with mafic minerals, soil maturity and space weathering (Mustard et al 2011).…”

Section: μM and 2 μM Ibd Mappingmentioning

confidence: 99%

“…The IBD spectral parameters of 1 μm and 2 μm were used in the Copernicus crater on the Moon to map the olivine exposures using Clementine data (Le Mouélic 2001). The M 3 and related ground truth data (RELAB) were used to map the distribution of mafic minerals like "olivine" and "pyroxene" on the lunar surface in Copernicus, Aristarchus, Marius and Naonobu craters, and northern Mare Imbrium, northeastern Oceanus Procellarum, Mare Crisium and Mare Orientale basins (Isaacson et al 2011;Klima et al 2011;Mustard et al 2011;Qiao et al 2014;Bharti et al 2014;Arivazhagan & Karthi 2018;Qiao et al 2021b;Karthi & Arivazhagan 2022).…”

Section: μM and 2 μM Ibd Mappingmentioning

confidence: 99%

“…This part of the mare associated highland locations may still contain ample evidence for the original flotation of crust and secondary petrogenesis associated with the LMO concept (Smith et al 1970;Wood et al 1970;Warren 1985;Thaisen et al 2011). Interpreting the recent lunar mission's high spatial and spectral resolution data has revealed an overall understanding of the origin and evolution of lunar surfaces (Jolliff 2006;Kumar et al 2009;Ouyang et al 2010;Pieters et al 2011;Thaisen et al 2011;Arivazhagan & Karthi 2018;Howari et al 2021;Howari et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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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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Insight into three-dimensional structure of the lunar crust and upper mantle in the Mare Crisium from gravity imaging

Yu,

Wang,

et al. 2024

Advances in Space Research

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Compositional and chronological characterization of mare crisium using Chandrayaan-1 and LROC-WAC data

Cited by 6 publications

References 45 publications

The Lunar Geophysical Network Landing Sites Science Rationale

The Lunar Geophysical Network Landing Sites Science Rationale

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

Insight into three-dimensional structure of the lunar crust and upper mantle in the Mare Crisium from gravity imaging

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