Chronological and compositional mapping of the Mare Orientale basin using Chandrayaan-1 – M3 and LRO datasets

Karthi, A.; Arivazhagan, S.

doi:10.1016/j.icarus.2021.114844

Cited by 8 publications

(5 citation statements)

References 107 publications

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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%

“…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%

“…To determine the age from remote sensing data, most chronological studies of a planetary surface use a welldeveloped and recognized statistical approach that is called "crater size frequency distribution" (CSFD). Traditionally, many academics estimate the CSFD by manually counting craters and determining sizes of the craters to highlight the ages of the craters using satellite imagery (Kneissl et al 2011;Michael and Neukum 2010;Qiao et al 2014;Atheer et al 2016;Arivazhagan & Karthi 2018;Qiao et al 2021c;Howari et al 2021;Karthi & Arivazhagan 2022).…”

Section: Chronological Investigationmentioning

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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Section: Standard Band Ratio (Sbr)mentioning

confidence: 99%

Section: μM and 2 μM Ibd Mappingmentioning

confidence: 99%

Section: Chronological Investigationmentioning

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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“…Up to now, several studies on mare geological structure and chemistry components were conducted, mainly based on FTA (FeO + TiO 2 abundance) data, moon mineralogy mapper (M 3 ) data, UV/VIS (ultraviolet-visible spectroscopy) data, the crater size-frequency distribution (CSFD) technique and so on [4][5][6][7][8][9][10][11]. For instance, Karthi et al, mapped the Mare Orientale impact basin using Chandrayaan-1 M 3 data and Lunar Reconnaissance Orbiter (LRO)-Wide Angle Camera (WAC) images [4]. Kramer et al, mapped the basalt units of the map of Mare Moscoviense and Mare Nectaris based on FTA data and Clementine UV-VIS data [5].…”

Section: Introductionmentioning

confidence: 99%

A Unified Brightness Temperature Features Analysis Framework for Mapping Mare Basalt Units Using Chang’e-2 Lunar Microwave Sounder (CELMS) Data

Yuan

Meng

et al. 2023

Remote Sensing

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The brightness temperature (TB) features extracted from Chang’e-2 Lunar Microwave Sounder (CELMS) data represent the passive microwave thermal emission (MTE) from the lunar regolith at different depths. However, there have been few studies assessing the importance and contribution of each TB feature for mapping mare basalt units. In this study, a unified framework of TB features analysis is proposed through a case study of Mare Fecunditatis, which is a large basalt basin on the eastern nearside of the Moon. Firstly, TB maps are generated from original CELMS data. Next, all TB features are evaluated systematically using a range of analytical approaches. The Pearson coefficient is used to compute the correlation of features and basalt classes. Two distance metrics, normalized distance and J-S divergence, are selected to measure the discrimination of basalt units by each TB feature. Their contributions to basalt classification are quantitatively evaluated by the ReliefF method and out-of-bag (OOB) importance index. Then, principal component analysis (PCA) is applied to reduce the dimension of TB features and analyze the feature space. Finally, a new geological map of Mare Fecunditatis is generated using CELMS data based on a random forest (RF) classifier. The results will be of great significance in utilizing CELMS data more widely as an additional tool to study the geological structure of the lunar basalt basin.

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“…Actualmente, gracias al avance de la ciencia y la tecnología de la mano con diversas investigaciones realizadas, se tiene información más precisa de nuestro satélite natural, conociéndose que la atmósfera lunar (en la Luna se le denomina exósfera) es muy débil, casi inexistente por ser muy tenue y delgada, por ello, únicamente se registran vientos que pueden provocar tormentas de polvo (GeoEnciclopedia, 2019). Además, diversas investigaciones mencionan que la superficie lunar es una cubierta de lava endurecida en la cual hay dos áreas diferenciadas: los mares que son la parte llana y más oscura representada por cuencas que se llenaron de lava hace 4200 y 1200 millones de años, y las áreas más claras que son más accidentadas, en las que resaltan la presencia de cráteres de distinto tamaño, proporcionando evidencia de cómo la corteza primitiva se pudo haber cristalizado a partir de un océano de magma que son de distintas composiciones y edades (Netting, 2014;Gaddis, 2003;Trang, 2022;Karthi, 2022). Los descubrimientos del Orbitador del Renacimiento Lunar de la NASA indican que la Luna podría haber tenido flujos volcánicos hasta hace solo decenas de millones de años, durante la era de los dinosaurios de la Tierra (Yan, 2019).…”

Section: Introductionunclassified

Teoría de la Luna volcánica, ¿TES y TEV son aplicables a otros cuerpos celestes?

Ramírez

Romero

et al. 2022

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Al valorar lo planteado en la Teoría de la Energía Sísmica (TES) y la Teoría de la Energía Volcánica (TEV) (entre otros pormenores, precisan la importancia de analizar a la Tierra como un todo, es decir, como un cuerpo) reflexionamos que para que sean teorías universales deben de ser aplicables a otros cuerpos celestes o por lo menos brindarnos algunas respuestas por analogía. Por ello, principalmente nos centraros en estudiar a nuestro satélite natural, la Luna, debido a que por su cercanía a la Tierra es el cuerpo celeste del que poseemos mayor información, no pudiendo evitar hacer un análisis referencial con otros cuerpos celestes. A la investigación se revela que la Luna ha tenido las condiciones para una actividad volcánica muy intensa, a consecuencia de ello la consumación de los componentes reactivos han sido en menos tiempo (en comparación con la actividad volcánica terrestre), por ello, a diferencia de la Tierra, en la Luna pronto la actividad volcánica cesó, dejando vestigios que nos traducen ese pasado violento con abundantes conos volcánicos activos, lo suficiente como para formar mares de lava que se conservan hasta nuestros días, los que los observamos en un ambiente gris de aparente eternidad.

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Chronological and compositional mapping of the Mare Orientale basin using Chandrayaan-1 – M3 and LRO datasets

Cited by 8 publications

References 107 publications

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

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

A Unified Brightness Temperature Features Analysis Framework for Mapping Mare Basalt Units Using Chang’e-2 Lunar Microwave Sounder (CELMS) Data

Teoría de la Luna volcánica, ¿TES y TEV son aplicables a otros cuerpos celestes?

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