Interpreting photometry of regolith-like surfaces with different topographies: shadowing and multiple scattering

Shkuratov, Yuriy; Stankevich, D. G.; Петров, Д. В.; Pinet, P.; Cord, A.; Daydou, Y.; Chevrel, S.

doi:10.1016/j.icarus.2003.12.017

Cited by 91 publications

(43 citation statements)

References 24 publications

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“…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 . At sub-mm to cm scales, typical lunar surface roughness values, defined as a root mean square (RMS) slope are 16-25°(ref.…”

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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“…It has been noted that variations in the shape of the disk-integrated solar phase curves produced by different values of the single particle scattering function can be compensated for by changes in the surface roughness parameter, which in turn can be compensated for by variations in the single scattering albedo (Harris et al, 1989;Shkuratov et al, 2005). Observations at very high solar phase angle (> 120…”

Section: Modeling Methodsmentioning

confidence: 99%

“…Shkuratov et al (2005) have shown through Monte Carlo ray-tracing methods that interpretations of surface roughness based on the Hapke roughness parameter need to be made with care. Multiple scattering effects on bright objects produces an underestimation of roughness by θ , and in some of their simulations θ did not accurately predict the surface roughness where large-scale roughness was present.…”

Section: Hapke Photometric Modelingmentioning

confidence: 99%

The 2004 Las Campanas/Lowell Observatory campaign II. Surface properties of Hayabusa target Asteroid 25143 Itokawa inferred from Hapke modeling

et al. 2008

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We present an analysis of Hapke photometric modeling applied to uniform ground-based UBVRIJHK broadband data of asteroid 25143 Itokawa collected over a wide range of solar phase angles (4• -130• ) during the 2004 apparition (Thomas-Osip et al., this issue, hereafter Paper I). Our photometric analyses indicate that Itokawa has a blocky surface with properties different from other, albeit larger, S-class asteroids studied using similar Hapke modeling analyses. Images from the Hayabusa spacecraft affirm the Hapke modeling results, demonstrating the ability of Hapke photometric modeling to predict a rocky asteroid surface correctly; this is the first time that a predicted rocky surface has been observed by a spacecraft. The single particle scattering functions are dominantly forward scattering, suggesting the surface material is composed primarily of clear particles whose scattering is dictated by the particle's surface as opposed to internal scatterers (more typical of S-class asteroids), while the opposition parameters indicate that the regolith may be more compact than most of the limited number of asteroids visited by spacecraft to date. The roughness properties, single particle scattering properties, and opposition surge characteristics are all indicative of a surface where multiple scattering does not play a major role in defining the photometric properties of the regolith.

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“…At opposition (g = 0), shadows are hidden behind the objects casting them, and hence an observer sees a surface that is much brighter than the same surface observed at nonzero phase, when shadows are visible to varying degrees. The texture of the surface determines the amount of shadowing, and also influences the extent to which incident illumination is multiply scattered between surface facets or among and within regolith particles (Shkuratov et al, 2005). Multiple scattering in turn causes shadowed areas to be partially illuminated, thus affecting the reflectance of the surface as measured by a distant observer.…”

Section: Introductionmentioning

confidence: 99%