Coherent Backscattering by Solar System Dust Particles

Muinonen, K.

doi:10.1017/s0074180900046593

Cited by 18 publications

(17 citation statements)

References 107 publications

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“…Note that Nelson et al measured aluminum oxide powders. These important findings are not consistent with the hypothesis (e.g., Mishchenko 1992, Mishchenko and Dlugach 1992, 1993) that the coherent backscatter enhancement is only observable, if the particle size is of the order of the wavelength. Equation (30) gives a rather good fit to experimental data (see 150-µm curve), and L = 29 µm and d = 9.5 µm (for the 15-µm curve).…”

Section: (Illumination By Nonpolarized Light)contrasting

confidence: 88%

“…The "interference" explanation for both the opposition effect and the negative polarization was given by Shkuratov (1985Shkuratov ( , 1988Shkuratov ( , 1989 and independently by Muinonen (1989). There are reviews on the backscatter phenomena of atmosphereless celestial bodies (Muinonen 1993, Shkuratov et al 1994b.…”

Section: Theoretical Studiesmentioning

confidence: 99%

“…It is assumed usually that a narrow spike is due to interference enhancement while a wide surge is a result of the shadow-hiding effect (e.g., Mishchenko and Dlugach 1992, 1993, Helfenstein et al 1997. To estimate contributions of both effects at each phase angle α is a difficult problem which is studied recently rather intensively.…”

Section: Introductionmentioning

confidence: 99%

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Opposition Effect from Clementine Data and Mechanisms of Backscatter

Shkuratov

Kreslavsky

Ovcharenko

et al. 1999

Icarus

157

126

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An analysis of Clementine data obtained from a UVVIS camera and simulating laboratory photometric and polarimetric measurements is presented with the use of a new photometric threeparameter function combining the shadow-hiding and coherent backscatter mechanisms. The fit of calculated curves to the average brightness phase function of the Moon derived from Clementine data indicates that the coherent backscatter component is nonzero. The average amplitude of the opposition surge of the Moon in the range of phase angles 0• -1• is approximately 10%. The Clementine data also show a flattening of phase-dependent brightness at angles less than 0.25• that is caused by the angular size of the solar disk. The lunar brightness phase curves at small phase angles are nearly the same in different wavelengths even though at larger phase angles (5• -50 • ) the lunar surface becomes distinctly redder with increasing phase angle. According to the model, the lack of wavelength-dependent brightness variations at small phase angles can be due to quasifractal properties of the lunar surface. Results of related laboratory measurements suggest that: (1) besides the narrow coherent backscatter opposition spike there is a broad component which can contribute to phase angles up to 10• and (2) a component of coherent backscatter can be important even for low albedo surfaces. The latter testifies the opposition effect of the lunar surface to be substantially formed by the coherent backscatter mechanism.

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Section: (Illumination By Nonpolarized Light)contrasting

confidence: 88%

Section: Theoretical Studiesmentioning

confidence: 99%

See 1 more Smart Citation

Opposition Effect from Clementine Data and Mechanisms of Backscatter

Shkuratov

Kreslavsky

Ovcharenko

et al. 1999

Icarus

157

126

View full text Add to dashboard Cite

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“…The history of photometric and polarimetric studies of planetary surfaces and their analogs has been described many times in earlier works (e.g., Lyot 1929;Hapke 1993;Dollfus 1998;Muinonen 1990Muinonen , 1994Shkuratov et al 1984Shkuratov et al , 1994Shkuratov et al , 1999. Here, we present only a short review of important telescope observations, laboratory simulations, and theoretical studies most relevant to our investigation.…”

Section: Short Review and Preliminary Remarksmentioning

confidence: 93%

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

Shkuratov¹,

Ovcharenko²,

Zubko³

et al. 2002

Icarus

189

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“…The main aspect is the opposition effect, a non-linear increase in brightness when the phase angles approaches zero degrees, observed in asteroids for the first time by Gehrels (1956). This has been studied for the connection with two important optical mechanisms of particulate media: The shadow-hiding (e.g., Hapke, 1981;Lumme et al, 1990;Stankevich et al, 1999) and the coherent-backscattering enhancement (e.g., Muinonen, 1994;Mishchenko et al, 2009). The former is related to the disappearance of mutual shadows among the regolith particles when opposition is near.…”

Section: Introductionmentioning

confidence: 99%

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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Coherent Backscattering by Solar System Dust Particles

Cited by 18 publications

References 107 publications

Opposition Effect from Clementine Data and Mechanisms of Backscatter

Opposition Effect from Clementine Data and Mechanisms of Backscatter

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

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

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