Confirmation of sublunarean voids and thin layering in mare deposits

Robinson, M. S.; Ashley, J. W.; Boyd, A. K.; Wagner, R. V.; Speyerer, E. J.; Hawke, B. R.; Hiesinger, H.; Bogert, C. H. van der

doi:10.1016/j.pss.2012.05.008

Cited by 140 publications

(114 citation statements)

References 20 publications

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“…Recent studies have observed thinly layered lava flows in some mare on the order of 10 m thick (Robinson et al, 2012;Enns and Robinson, 2013), possibly interbedded with ash or regolith. There are likely many mechanical layers in mare basalt sequences separated by relatively thin interbeds.…”

Section: Mechanical Discontinuity and Layer Thickness Estimatesmentioning

confidence: 99%

Small-scale lunar graben: Distribution, dimensions, and formation processes

French

Bina

Robinson

et al. 2015

Icarus

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Section: Mechanical Discontinuity and Layer Thickness Estimatesmentioning

confidence: 99%

Small-scale lunar graben: Distribution, dimensions, and formation processes

French

Bina

Robinson

et al. 2015

Icarus

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“…They could serve as a proper habitat for a small group of people and do not require construction materials in large volumes. Recently, it has been reported that 20~200 pit craters less than 50 m in size are scattered all over the surface of the Moon (Robinson et al 2012). These small scale craters are of primary interest for this study.…”

Section: M128202846l M126710873rmentioning

confidence: 93%

“…The emission angle indicates the angle between the normal direction to the camera lens and the normal direction to the surface of the Moon. The inner space wider than the area of the entrance could suggest the existence of lava tube in the pit crater (Robinson et al 2012).…”

Section: D Structure Of Pit Cratermentioning

confidence: 99%

“…The informations of the diameter, the incident angle, and the emission angle are required to generate the 3D model of the crater. The maximum diameter measured from the various images was used as a reference and the depth was obtained from the results of Robinson et al (2012) (Table 4). The images used are shown in Figs.…”

Section: D Structure Of Pit Cratermentioning

confidence: 99%

“…5 and 6. Among the results of Robinson et al (2012), the cases with no visibility of inner wall or floor and the cases whose shadow lengths are not possible to be estimated are excluded from the generation of 3D models because the depths cannot be determined.…”

Section: D Structure Of Pit Cratermentioning

confidence: 99%

See 2 more Smart Citations

Lunar Pit Craters Presumed to be the Entrances of Lava Caves by Analogy to the Earth Lava Tube Pits

Yi¹,

Kim²

2014

Journal of Astronomy and Space Sciences

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Improved discrimination of volcanic complexes, tectonic features, and regolith properties in Mare Serenitatis from Earth-based radar mapping

Campbell

Hawke

Morgan

et al. 2014

J. Geophys. Res. Planets

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Radar images at 70 cm wavelength show 4-5 dB variations in backscatter strength within regions of relatively uniform spectral reflectance properties in central and northern Mare Serenitatis, delineating features suggesting lava flow margins, channels, and superposition relationships. These backscatter differences are much less pronounced at 12.6 cm wavelength, consistent with a large component of the 70 cm echo arising from the rough or blocky transition zone between the mare regolith and the intact bedrock. Such deep probing is possible because the ilmenite content, which modulates microwave losses, of central Mare Serenitatis is generally low (2-3% by weight). Modeling of the radar returns from a buried interface shows that an average regolith thickness of 10 m could lead to the observed shifts in 70 cm echo power with a change in TiO 2 content from 2% to 3%. This thickness is consistent with estimates of regolith depth (10-15 m) based on the smallest diameter for which fresh craters have obvious blocky ejecta. The 70 cm backscatter differences provide a view of mare flow-unit boundaries, channels, and lobes unseen by other remote sensing methods. A localized pyroclastic deposit associated with Rima Calippus is identified based on its low radar echo strength. Radar mapping also improves delineation of units for crater age dating and highlights a 250 km long, east-west trending feature in northern Mare Serenitatis that we suggest is a large graben flooded by late-stage mare flows.

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Confirmation of sublunarean voids and thin layering in mare deposits

Cited by 140 publications

References 20 publications

Small-scale lunar graben: Distribution, dimensions, and formation processes

Small-scale lunar graben: Distribution, dimensions, and formation processes

Lunar Pit Craters Presumed to be the Entrances of Lava Caves by Analogy to the Earth Lava Tube Pits

Improved discrimination of volcanic complexes, tectonic features, and regolith properties in Mare Serenitatis from Earth-based radar mapping

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