A quantitative test of the ability of models based on the equation of radiative transfer to predict the bidirectional reflectance of a well-characterized medium

Hapke, Bruce; Shepard, Michael K.; Nelson, Robert M.; Smythe, W. D.; Piatek, J. L.

doi:10.1016/j.icarus.2008.09.006

Cited by 46 publications

(36 citation statements)

References 40 publications

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“…The focus of many laboratory studies has been to test and validate the Hapke model (Buratti and Veverka, 1985;Kamei and Nakamura 2002;Cord et al, 2003;Gunderson et al, 2005;Shkuratov et al, 2007;Shepard and Helfenstein, 2007;Helfenstein and Shepard, 2011;Hapke et al, 2009;Souchon et al, 2011) as well as studies that compare the predictions of Hapke's model to numerical light-scattering simulations (Helfenstein, 1988;Shepard and Campbell, 1998;Ciarniello et al, 2014). Finally in situ studies rely on using well-sampled planetary observation data sets to derive information about the validity of Hapke's model (cf.…”

Section: Recent Testsmentioning

confidence: 99%

“…Roush et al, 1990;Calvin and Clark, 1991;Lucey, 1998;Verbiscer et al, 2006;Wilcox et al, 2006;Denevi et al, 2008;Warell and Davidsson, 2010). The model successfully predicts the scattering behavior of idealized soil samples (Hapke et al, 2009;Hapke and Wells, 1981;Hapke, 2012b). Computer simulation studies have investigated the geological interpretation of Hapke's (1984) correction for macroscopic roughness (Helfenstein 1988;Shepard and Campbell 1998).…”

Section: Recent Testsmentioning

confidence: 99%

“…Studies suggest that, in particular, the Hapke model is realistic when macroscopic surface relief and complex particle shapes can be ignored (Hapke et al, 2009). However the approach is not entirely reliable and work is especially needed to better understand the opposition effect.…”

Section: Summary and Future Perspectivementioning

confidence: 99%

See 2 more Smart Citations

Asteroid Photometry

Li¹,

Helfenstein²,

Buratti³

et al. 2015

Asteroids IV

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Asteroid photometry has three major applications: providing clues about asteroid surface physical properties and compositions, facilitating photometric corrections, and helping design and plan ground-based and spacecraft observations. The most significant advances in asteroid photometry in the past decade were driven by spacecraft observations that collected spatially resolved imaging and spectroscopy data. In the mean time, laboratory measurements and theoretical developments are revealing controversies regarding the physical interpretations of models and model parameter values. We will review the new developments in asteroid photometry that have occurred over the past decade in the three complementary areas of observations, laboratory work, and theory. Finally we will summarize and discuss the implications of recent findings. ! 2!

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Section: Recent Testsmentioning

confidence: 99%

Section: Recent Testsmentioning

confidence: 99%

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Asteroid Photometry

Li¹,

Helfenstein²,

Buratti³

et al. 2015

Asteroids IV

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“…The Hapke IMSA model (Hapke, 1993(Hapke, , 2002(Hapke, , 2008Hapke et al 2009) is one of several models developed to study the scattering properties of packed media (Lumme and Bowell, 1981;Drossart 1993;Shkuratov et al, 1999). It is an analytic two stream approximate solution to the radiative transfer equation and it has been applied successfully to perform photometric corrections of imaging data (Hudson and Ostro, 1999;Domingue et al, 2009), to investigate physical properties of regoliths (Mallama et al, 2002;Buratti et al, 2004) and to estimate surface compositions of planetary surfaces (Cruikshank et al, 2001;Cruikshank et al, 2005;Poulet et al, 2002).…”

Section: Introduction and Rationalementioning

confidence: 99%

Hapke modeling of Rhea surface properties through Cassini-VIMS spectra

Ciarniello

Capaccioni

Filacchione

et al. 2011

Icarus

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The surface properties of the icy bodies in the saturnian system have been investigated by means of the CASSINI-VIMS (Visual Infrared Mapping Spectrometer) hyperspectral imager which operates in the 0.35-5.1 m wavelength range. In particular, we have analyzed 111 full disk hyperspectral images of Rhea ranging in solar phase between 0.08° and 109.8°. These data have been previously analyzed by Filacchione et al. (2007Filacchione et al. ( , 2010 to study, adopting various "spectral indicators" (such as spectral slopes, band depth, continuum level, etc.), the relations among various saturnian satellites.As a further step we proceed in this paper to a quantitative evaluation of the physical parameters determining the spectrophotometric properties of Rhea's surface. To do this we have applied Hapke (1993) IMSA model (Isotropic Multiple Scattering Approximation) which allow us to model the phase function at VIS-IR (visible-infrared) wavelengths as well as the spectra taking into account various types of mixtures of surface materials. Thanks to this method we have been able to constrain the size of water ice particles covering the surface, the amount of organic contaminants, the large scale surface roughness and the opposition effect surge. From our analysis it appears that wavelength dependent parameters, e.g. opposition surge width (h) and single-particle phase function parameters (b,v), are strongly correlated to the estimated single-scattering albedo of particles. For Rhea the best fit solution is obtained by assuming:1) an intraparticle mixture of crystalline water ice and a small amount (0.4%) of Triton tholin; 2) a monodisperse grain size distribution having a particle diameter a m = 38 µm; and 3) a surface roughness parameter value of 33°. The study of phase function shows that both Shadow Hiding and Coherent Backscattering contribute to the opposition surge. This study represents the first attempt, in the case of Rhea, to join the spectral and the photometric analysis. The surface model we derived gives a good quantitative description of both spectrum and phase curve of the satellite. The same approach and model, with appropriate modifications, shall be applied to VIMS data of the other icy satellites of Saturn, in order to reveal similarities and differences in the surface characteristics to understand how these bodies interact with their environment.

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“…This steep spike of brightness is called the Brightness Opposition Effect (BOE). The possible explanation of the BOE by the CBE was first mentioned by Shkuratov (1988), Muinonen (1990), and Hapke (1990), and later became a subject of numerous observational, laboratory, and theoretical studies (see, e.g., reviews by Rosenbush et al 2006;Tishkovets et al 2004;Shkuratov et al 2004;Mishchenko et al 2006b;Mishchenko 2008;Hapke et al 2009). It was found that the BOE is different for different bodies and this difference can be characterized by its amplitude or enhancement factor which is defined as the ratio of the intensity in the exact backscattering direction to the background (estimated from pre-opposition photometry) intensity.…”

Section: Introductionmentioning

confidence: 98%

Impact of Coherent Backscattering on the Spectra of Icy Satellites of Saturn and the Implications of Its Effects for Remote Sensing

Kolokolova

Buratti

Тишковец

2010

ApJ

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We have found systematic variations in the spectra of Saturn's icy satellites Rhea and Iapetus obtained by the Cassini Visual and Infrared Mapping Spectrometer (VIMS). The main attribute of these variations is a significantly different depth of the absorption bands at different phase angles. We show that these variations likely result from the coherent backscattering effect (CBE). This effect has been mainly known as the probable reason for a steep opposition spike in brightness observed for some asteroids, moons, and Kuiper Belt Objects at phase angles smaller than 3• . The opposition spike has different steepness at different albedos due to the strong dependence of the CBE on the absorption of the material. As a result of this dependence, the impact of the CBE should be different within and outside of the absorption spectral bands. This produces a systematic change in the depth of the absorption bands at different phase angles, as we see in the VIMS spectra of Rhea and Iapetus. Neglecting this effect may result in misinterpretation of the spectra and misleading conclusions about compositional and particle size differences of icy bodies studied at different phase angles. Our computer modeling of the CBE reproduces the observed spectral variations and also shows that they are strongly affected by the size and packing of particles. Thus, the variations in the absorption bands produced by the CBE not only allow us to improve interpretation of the spectra, but also provide a promising approach to study size and packing of the regolith and dust particles.

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A quantitative test of the ability of models based on the equation of radiative transfer to predict the bidirectional reflectance of a well-characterized medium

Cited by 46 publications

References 40 publications

Asteroid Photometry

Asteroid Photometry

Hapke modeling of Rhea surface properties through Cassini-VIMS spectra

Impact of Coherent Backscattering on the Spectra of Icy Satellites of Saturn and the Implications of Its Effects for Remote Sensing

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