The Opposition Effect and Negative Polarization of Structural Analogs for Planetary Regoliths

Shkuratov, Yu. G.; Ovcharenko, Andrey; Zubko, Evgenij; Miloslavskaya, O. V.; Muinonen, K.; Piironen, J.; Nelson, Robert M.; Smythe, W. D.; Rosenbush, V. K.; Helfenstein, P.

doi:10.1006/icar.2002.6923

Cited by 188 publications

(92 citation statements)

References 56 publications

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“…When comparing Lutetia polarimetric curve with laboratory powder of meteorites, only the carbonaceous chondrites, specially the CV3, show similar minimum of negative branch and inversion angle. Multiple hypothesis have been evoked to explain this phenomena (Shkuratov et al, 1994, for a review), but the shadow-hiding and coherent-backscattering seems to prevail as the main mechanisms (Shkuratov et al, 2002). The connection with such dark meteoritic composition should rule out the contribution of CBOE, since the mechanism is also connect to grain shape and size.…”

Section: Discussionmentioning

confidence: 99%

“…The connection with such dark meteoritic composition should rule out the contribution of CBOE, since the mechanism is also connect to grain shape and size. Shkuratov et al (2002) states that scattering of higher orders still significantly contribute to negative polarization, even for very dark surfaces. Therefore, the wide negative branch of Lutetia may still be a product of both mechanisms.…”

Section: Discussionmentioning

confidence: 99%

“…Generally, the CBOE can be solely confirm at the observation of a sharp negative branch at small phase angles (Shkuratov et al, 2002) in the polarimetric curves or the measurement of dependence of HWHM with wavelength (Akkermans et al, 1988). To test that, a initial input for Bc 0 and h c are set both to 0.05 (∆α CBOE = 1 • ).…”

Section: H3mentioning

confidence: 99%

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Asteroid (21) Lutetia: Disk-resolved photometric analysis of Baetica region

Hasselmann

Fornasier

Leyrat

et al. 2016

Icarus

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ABSTRACT. (21) Lutetia has been visited by Rosetta mission on July 2010 and observed with a phase angle ranging from 0.15 to 156.8 degrees. The Baetica region, located at the north pole has been extensively observed by OSIRIS cameras system. Baetica encompass a region called North Pole Crater Cluster (NPCC), shows a cluster of superposed craters which presents signs of variegation at the small phase angle images. For studying the location, we used 187 images distributed throughout 14 filter recorded by the NAC (Narrow Angle Camera) and WAC (Wide Angle Camera) of the OSIRIS system on-board Rosetta taken during the fly-by. Then, we photometrically modeled the region using Minnaert diskfunction and Akimov phase function to obtain a resolved spectral slope map at phase angles of 5 • and 20 • . We observed a dicothomy between Gallicum and Danuvius-Sarnus Labes in the NPCC, but no significant phase reddening (−0.04 ± 0.045% · microns −1 deg −1 ). In the next step, we applied the Hapke (2008Hapke ( ,2012 model for the NAC F82+F22 (649.2 nm), WAC F13 (375 nm) and WAC F17 (631.6 nm) and we obtained normal albedo maps and Hapke parameter maps for NAC F82+F22. On Baetica, at 649.2 nm, the geometric albedo is 0.205 ± 0.005, the average single-scattering albedo is 0.181 ± 0.005, the average asymmetric factor is −0.342 ± 0.003, the average shadow-hiding opposition effect amplitude and width are 0.824 ± 0.002 and 0.040 ± 0.0007, the average roughness slope is 11.45 • ± 3 • and the average porosity is 0.85 ± 0.002. We are unable to confirm the presence of coherent-backscattering mechanism. In the NPCC, the normal albedo variegation among the craters walls reach 8% brighter for Gallicum Labes and 2% fainter for Danuvius Labes. The Hapke parameter maps also show a dicothomy at the opposition effect coefficients, single-scattering albedo and asymmetric factor, that may be attributed to the maturation degree of the regolith or to compositonal variation. In addition, we compared the Hapke (2008Hapke ( , 2012 and Hapke (1993) parameters with laboratory samples and other small-solar system bodies visited by space missions.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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Asteroid (21) Lutetia: Disk-resolved photometric analysis of Baetica region

Hasselmann

Fornasier

Leyrat

et al. 2016

Icarus

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“…Muñoz et al 2000;Shkuratov et al 2002). The negative branch was found to become more prominent and the inversion angle to increase in the cases of a) an increase in the refractive index; b) a decrease in the particle sizes to sizes comparable wavelength; c) complex internal structure of particles; and d) the mixture of particles with high contrast in albedo (Muñoz et al 2000;Shkuratov et al 1994Shkuratov et al , 2002Zubko et al 2005). One or several of the abovementioned properties can be responsible for the particular polarization characteristics of Lutetia.…”

Section: Polarimetrymentioning

confidence: 99%

“…The contribution of the mechanism of the single particle scattering remains poorly understood but its efficiency in producing wide negative polarization branch has been demonstrated by laboratory and numerical modeling (e.g. Muñoz et al 2000;Shkuratov et al 2002). The negative branch was found to become more prominent and the inversion angle to increase in the cases of a) an increase in the refractive index; b) a decrease in the particle sizes to sizes comparable wavelength; c) complex internal structure of particles; and d) the mixture of particles with high contrast in albedo (Muñoz et al 2000;Shkuratov et al 1994Shkuratov et al , 2002Zubko et al 2005).…”

Section: Polarimetrymentioning

confidence: 99%

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

Belskaya

Fornasier

Krugly

et al. 2010

A&A

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Aims. A wide observational campaign was carried out in [2004][2005][2006][2007][2008][2009] that aimed to complete the ground-based investigation of Lutetia prior to the Rosetta fly-by in July 2010. Methods. We obtained BVRI photometric and V-band polarimetric measurements over a wide range of phase angles, and visible and infrared spectra in the 0.4-2.4 μm range. We analyze them with previously published data to retrieve information about Lutetia's surface properties.Results. Values of lightcurve amplitudes, absolute magnitude, opposition effect, phase coefficient, and BVRI colors of Lutetia surface seen at near pole-on aspect are determined. We define more precisely parameters of polarization phase curve and show their distinct deviation from any other moderate-albedo asteroid. An indication of possible variations in both polarization and spectral data across the asteroid surface are found. To explain features found by different techniques, we propose that (i) Lutetia has a non-convex shape, probably due to a large crater, and heterogeneous surface properties probably related to surface morphology; (ii) at least part of the surface is covered by a fine-grained regolith of particle size smaller than 20 μm; (iii) the closest meteorite analogues of Lutetia's surface composition are particular types of carbonaceous chondrites, or Lutetia has specific surface composition that is not representative among studied meteorites.

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Photometric properties of Mars soils analogs

et al. 2013

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[1] We have measured the bidirectional reflectance of analogs of dry, wet, and frozen Martian soils over a wide range of phase angles in the visible spectral range. All samples were produced from two geologic samples: the standard JSC Mars-1 soil simulant and Hawaiian basaltic sand. In a first step, experiments were conducted with the dry samples to investigate the effects of surface texture. Comparisons with results independently obtained by different teams with similar samples showed a satisfying reproducibility of the photometric measurements as well as a noticeable influence of surface textures resulting from different sample preparation procedures. In a second step, water was introduced to produce wet and frozen samples and their photometry investigated. Optical microscope images of the samples provided information about their microtexture. Liquid water, even in relatively low amount, resulted in the disappearance of the backscattering peak and the appearance of a forward-scattering peak whose intensity increases with the amount of water. Specular reflections only appeared when water was present in an amount large enough to allow water to form a film at the surface of the sample. Icy samples showed a wide variability of photometric properties depending on the physical properties of the water ice. We discuss the implications of these measurements in terms of the expected photometric behavior of the Martian surface, from equatorial to circum-polar regions. In particular, we propose some simple photometric criteria to improve the identification of wet and/or icy soils from multiple observations under different geometries.

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The Opposition Effect and Negative Polarization of Structural Analogs for Planetary Regoliths

Cited by 188 publications

References 56 publications

Asteroid (21) Lutetia: Disk-resolved photometric analysis of Baetica region

Asteroid (21) Lutetia: Disk-resolved photometric analysis of Baetica region

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

Photometric properties of Mars soils analogs

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