Lunar regolith thickness estimation using dual frequency microwave brightness temperature and influence of vertical variation of FeO+TiO2

Vijayan, S.; Mohan, Shiv; Murty, SripadaV.S.

doi:10.1016/j.pss.2014.11.017

Cited by 12 publications

(4 citation statements)

References 30 publications

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“…-Dark materials (maria and basins) from the Imbrian and Eratosthenian epochs; -Terra and plains from pre-Imbrian and Imbrian epochs; and -Crater materials from pre-Imbrian, Imbrian, Eratosthenian and Copernican epochs. Moreover, the lunar surface is covered by the regolith, a thin layer (< 15 m) of fine material, exposed to a continuous particle bombardment [29], [30].…”

Section: Study Areamentioning

confidence: 99%

New Morphometric Data of Lunar Sinuous Rilles

Podda

Melis

Collu

et al. 2020

IEEE J. Sel. Top. Appl. Earth Observations Remote Sensing

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On the surface of the Moon a large number of linear features are recognizable. Long and narrow depressions are defined as lunar rilles. Their morphology has different characteristics, related to their origin. Among these, the sinuous rilles represent lineaments considered remnants of shallow lava channels. In this study, a quadrant of the Moon has been analyzed to recognize and map this type of morphology. An accurate morphometric analysis has been accomplished, using the Lunar Reconnaissance Orbiter Camera (LROC) which has a resolution of 100 m/pixel, and the Digital Elevation Model from Lunar Orbiter Laser Altimeter (LOLA) with a resolution of 6 m/pixel. Fifty-one sinuous rilles have been recognized in the study area, eighteen of which are new, improving a previous catalogue. The resulting quantitative and qualitative measurements were analyze and compared each other' to identify potential morphological trends. Different relationships between morphological parameters have been proposed, and the results enhance the importance of substrate composition in the evolution of these features, emerged mainly from the variations in width and depth values. The linear relationship between these two parameters is consistent with the idea that erosion efficiency acts proportionally in both vertical and horizontal directions. Partial filling phenomena by subsequent lava flows probably occurred in some sinuous rilles located in maria. The hypothesis of a constructive genesis requires further investigation to identify the levees created by sinuous rilles' formation process.

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Section: Study Areamentioning

confidence: 99%

New Morphometric Data of Lunar Sinuous Rilles

Podda

Melis

Collu

et al. 2020

IEEE J. Sel. Top. Appl. Earth Observations Remote Sensing

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“…Interaction of radar waves with lunar regolith can provide numerous important information, which can be used to decipher regolith thickness distribution. Studies have been done to estimate the regolith thickness using simulated passive microwave brightness temperature (TB) expected from upcoming Chandrayaan-2 mission at L (1.25 GHz)-and S (2.1 GHz)-bands (Vijayan et al 2015). Bulk density (), dielectric permittivity and FeO+TiO 2 (S) content were used as varying parameters to simulate TB from a three-layermodel to estimate the thickness.…”

Section: Utilization Of Radar Data For Studying Lunar Surfacementioning

confidence: 99%

Understanding our Celestial Neighbors: An Indian Perspective in Planetary Sciences and Exploration

Chauhan

Bhardwa²,

Kumar³

et al. 2016

Proceedings of the Indian National Science Academy

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The planetary exploration program of the Indian Space Research Organization is described. The important results obtained from the two successful missions, Mars orbiter Mission (2014) and the earlier Chandrayaan-1 mission (2008-9) to moon are summarized. High-resolution maps of Valles Marineris enabled several surface, aqueous and atmospheric features to be delineated and the highly elliptical orbit of MOM enabled imaging of the surface of the farther side of Deimos as well as study of Mars exospheric constituents. The results from Chandrayaan-1 mission changed many lunar concepts e.g. from dry, passive and inactive to moon to wet, tectonically and volcanically active moon. Some recent results based on the space borne and laboratory based study of Titan, Pluto, Comets and meteorites coming from Mars and Vesta are summarized. The future planetary exploration plans, such as Chandrayaan-2 and second Mars mission are briefly mentioned.

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“…Vijayan et al. (2015) proposed a method to estimate both the permittivity and thickness of the lunar regolith with simulated brightness temperature data from a dual frequency SAR of Chandrayaan‐2 mission. So far, the permittivity of lunar regolith has been roughly estimated using many indirect methods.…”

Section: Introductionmentioning

confidence: 99%

“…The velocity of electromagnetic waves within the regolith layer is completely influenced by the average permittivity of regolith materials, which can be constrained by the propagating time between the surface and subsurface echoes in radargrams. Vijayan et al (2015) proposed a method to estimate both the permittivity and thickness of the lunar regolith with simulated brightness temperature data from a dual frequency SAR of Chandrayaan-2 mission. So far, the permittivity of lunar regolith has been roughly estimated using many indirect methods.…”

mentioning

confidence: 99%

Properties of Lunar Regolith on the Moon's Farside Unveiled by Chang'E‐4 Lunar Penetrating Radar

et al. 2021

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The complex thermal history of the Moon leads to an unequal distribution of volcanic products between the lunar nearside and the farside. So far, no lunar materials have been sampled from the Moon's farside and no detailed properties of lunar regolith on the farside have been detected before. On January 3, 2019, Chang'E‐4 (CE‐4) touched down onto the Von Kármán crater on the Moon's farside. CE‐4 Lunar Penetrating Radar (LPR) onboard the Yutu‐2 rover is the first surface radar on the Moon's farside. Here we show the subsurface structure and properties of regolith materials at the landing region with LPR data during the first five lunar days. The thickness of lunar regolith is constrained as ∼12 m, much thicker than that at Chang'E‐3 (CE‐3) landing site, which is expected since CE‐3 landed on lunar maria. The relative permittivity of lunar surface (<30 cm) at CE‐4 landing region is identified to be 2.35 ± 0.20. The loss tangent and TiO2 + FeO content of the regolith materials layer (0–∼12 m) are constrained to be (4.4±0.5)×10−3 and 11.6±1.1 wt.%, respectively, much lower than those at CE‐3 landing site. It indicates that local surface materials possess less attenuation for radiowave, in accordance with the greater penetrating depth of CE‐4 LPR than that of CE‐3 LPR. Furthermore, the results also prove that the growth rate of lunar weathered regolith successively declines over time and the growth rate of lunar regolith on the Moon's farside may well be higher than that on the nearside due to the more frequent meteorite impacts.

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Lunar regolith thickness estimation using dual frequency microwave brightness temperature and influence of vertical variation of FeO+TiO2

Cited by 12 publications

References 30 publications

New Morphometric Data of Lunar Sinuous Rilles

New Morphometric Data of Lunar Sinuous Rilles

Understanding our Celestial Neighbors: An Indian Perspective in Planetary Sciences and Exploration

Properties of Lunar Regolith on the Moon's Farside Unveiled by Chang'E‐4 Lunar Penetrating Radar

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