Submillimeter-Scale Topography of the Lunar Regolith

Helfenstein, P.; Shepard, Michael K.

doi:10.1006/icar.1999.6160

Cited by 138 publications

(138 citation statements)

References 54 publications

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“…6) and Diviner daytime measurements in channels 3 and 6 (12.5-25 mm) to determine the spectral aniosthermality caused by surface roughness at Reiner Gamma. Surface roughness varies with length scale, and becomes greater with decreasing scale 29 . Previous lunar surface roughness estimates have included Lunar Orbiter Laser Altimeter data at metre to decametre scales 30 , visible photometric studies typically at sub-mm scales 31,32 and additional sub-mm surface roughness estimates from in situ high-resolution imagery 29 .…”

Section: Resultsmentioning

confidence: 99%

Formation of lunar swirls by magnetic field standoff of the solar wind

et al. 2015

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Lunar swirls are high-albedo markings on the Moon that occur in both mare and highland terrains; their origin remains a point of contention. Here, we use data from the Lunar Reconnaissance Orbiter Diviner Lunar Radiometer to support the hypothesis that the swirls are formed as a result of deflection of the solar wind by local magnetic fields. Thermal infrared data from this instrument display an anomaly in the position of the silicate Christiansen Feature consistent with reduced space weathering. These data also show that swirl regions are not thermophysically anomalous, which strongly constrains their formation mechanism. The results of this study indicate that either solar wind sputtering and implantation are more important than micrometeoroid bombardment in the space-weathering process, or that micrometeoroid bombardment is a necessary but not sufficient process in space weathering, which occurs on airless bodies throughout the solar system.

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Section: Resultsmentioning

confidence: 99%

Formation of lunar swirls by magnetic field standoff of the solar wind

et al. 2015

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“…Haldemann el al. (1997, personal communication) found H -0.5 for the terrain around the Mars Pathfinder landing site at scales of centimeters to tens of meters, while Helfenstein and Shepard (1999) report H values of 0.54.7 for undisturbed lunar regolith at scales of submillimeters to centimeters.…”

Section: J~tstifica~ion For-assumplion Of Self-affine Behavior-mentioning

confidence: 99%

Radar Scattering from a Self-Affine Fractal Surface: Near-Nadir Regime

Shepard¹,

Campbell

1999

Icarus

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“…Shepard and Campbell (1998) argued that the photometric roughness measured byθ is dominated by the smallest size scale for which shadows still exist -which is a few times the wavelength of incident radiation if diffraction dominates shadow removal (∼ 1 μm), although it could be substantially larger (centimeters) if shadows are removed by efficient multiple scattering (a mechanism which decreases in importance when A v is reduced). In this context it is interesting that < ∼ 5% of the roughness measured for lunar regolith originates from topographic features larger than ∼ 8 cm according to Helfenstein and Shepard (1999). In their laboratory investigation of regolith analogues, Cord et al (2003) found thatθ primarily was determined by roughness on the sub-mm to cm level.…”

Section: Accepted M Manuscriptmentioning

confidence: 99%

Physical properties of morphological units on Comet 9P/Tempel 1 derived from near-IR Deep Impact spectra

Davidsson

Gutiérrez

Rickman

2009

Icarus

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In this paper we analyze near-infrared thermal emission spectra of the spatially resolved nucleus of Comet 9P/Tempel 1 obtained by the NASA spacecraft Deep Impact. Maps of spectral reddening, the product X between the beaming function and directional emissivity, as well as surface temperature are constructed. Thermophysical modeling is used to estimate the degree of small scale surface roughness and thermal inertia by detailed reproduction of the Surface variations in reddening, roughness, thermal inertia, composition and/or grain size are moderately to strongly correlated to the locations of morphological units on the surface.The existence of morphological units with differing physical properties may be primordial, hence reflecting a diversity in the building block cometesimals, or resulting from evolutionary processes.

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Submillimeter-Scale Topography of the Lunar Regolith

Cited by 138 publications

References 54 publications

Formation of lunar swirls by magnetic field standoff of the solar wind

Formation of lunar swirls by magnetic field standoff of the solar wind

Radar Scattering from a Self-Affine Fractal Surface: Near-Nadir Regime

Physical properties of morphological units on Comet 9P/Tempel 1 derived from near-IR Deep Impact spectra

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