Polarimetric and photometric properties of the moon: Telescope observation and laboratory simulation

Shkuratov, Yu. G.; Opanasenko, N. V.

doi:10.1016/0019-1035(92)90161-y

Cited by 99 publications

(68 citation statements)

References 11 publications

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“…Some results have been published by Shkuratov et al ( , 1989Shkuratov et al ( , 1991Shkuratov et al ( , 1992. In this series of measurements we used two broad spectral ranges with effective wavelengths of 0.62 µm (±0.06 µm) and 0.42 µm (±0.04 µm).…”

Section: Measurements In the Phase-angle Rangementioning

confidence: 95%

Opposition Effect from Clementine Data and Mechanisms of Backscatter

Shkuratov

Kreslavsky

Ovcharenko

et al. 1999

Icarus

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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: Measurements In the Phase-angle Rangementioning

confidence: 95%

Opposition Effect from Clementine Data and Mechanisms of Backscatter

Shkuratov

Kreslavsky

Ovcharenko

et al. 1999

Icarus

Self Cite

159

126

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“…• )/A(10 • ) correlates with P min and α inv (Shkuratov et al 1992), where A(α) is the bidirectional reflectance (or albedo) in the sense of Hapke's (1993) definition. The dependence P min (A) has a horseshoe shape such that |P min | increases with increasing A at small A, but with further growth of A the value |P min | decreases.…”

Section: Telescope Observationsmentioning

confidence: 99%

“…This correlation was studied in detail for the Moon, lunar samples, and many natural and artificial powders (e.g., Dollfus and Bowell 1971). At small phases the correlation between albedo and polarization degree is ambiguous: It can be inverse, direct, or even absent (Shkuratov et al 1992. Figure 6 presents phase curves of brightness and linear polarization for mixtures of chalk and soot powders taken in different proportions.…”

Section: Influence Of Albedomentioning

confidence: 99%

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

Shkuratov¹,

Ovcharenko²,

Zubko³

et al. 2002

Icarus

191

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“…To characterize the deviations, the parameter (P max ) a A has been proposed. It has been shown that the parameter bears significant information on the characteristic size and microporosity of the lunar regolith (Shkuratov, 1981;Shkuratov and Basilevsky, 1981;Shkuratov and Opanasenko, 1992;Dollfus 1998Dollfus , 1999. Analysis of the images of the distribution of (P max ) a A shows the following (Shkuratov and Opanasenko, 1992): (1) rayed young craters including the Aristarchus crater have increased values of the parameter, perhaps because of the immature character of the regolith (coarse grains); and (2) regions characterized by decreased values of (P max ) a A, e.g., Aristarchus Plateau and Marius Hills area, which are regions of volcanism that could be accompanied by ash deposits containing fine (dust) particles.…”

Section: Introductionmentioning

confidence: 99%