Radiative transfer modeling of near‐infrared reflectance of lunar highland and mare soils

Cahill, J. T. S.; Lucey, P. G.; Stockstill-Cahill, K. R.; Hawke, B. R.

doi:10.1029/2009je003500

Cited by 15 publications

(16 citation statements)

References 37 publications

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“…; Cahill et al. , ; Li and Li ). The significant difference between the two models is in how they approximate different scattering processes for photons.…”

Section: Introductionmentioning

confidence: 97%

Estimating the modal mineralogy of eucrite and diogenite meteorites using visible–near infrared reflectance spectroscopy

Milliken

2015

Meteorit & Planetary Scien

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Reliable quantitative mapping of minerals exposed on Vesta's surface is crucial for understanding the crustal composition, petrologic evolution, and surface modification of the howardite, eucrite, and diogenite (HED) parent body. However, mineral abundance estimates derived from visible-near infrared (VIS-NIR) reflectance spectra are complicated by multiple scattering, particle size, and nonlinear mixing effects. Radiative transfer models can be employed to accommodate these issues, and here we assess the utility of such models to accurately and efficiently determine modal mineralogy for a suite of eucrite and olivinebearing (harzburgitic) diogenite meteorites. Hapke and Shkuratov radiative transfer models were implemented to simultaneously estimate mineral abundances and particle size from VIS-NIR reflectance spectra of these samples. The models were tested and compared for laboratory-made binary (pyroxene-plagioclase) and ternary mixtures (pyroxene-olivineplagioclase) as well as eucrite and diogenite meteorite samples. Results for both models show that the derived mineral abundances are commonly within 5-10% of modal values and the estimated particle sizes are within the expected ranges. Results for the Hapke model suggest a lower detection limit for olivine in HEDs when compared with the Shkuratov model (5% versus 15%). Our current implementation yields lower uncertainties in mineral abundance (commonly <5%) for the Hapke model, though both models have an advantage over typically used parameters such as band depth, position, and shape in that they provide quantitative information on mineral abundance and particle size. These results indicate that both the Hapke and Shkuratov models may be applied to Dawn VIR data in a computationally efficient manner to quantify the spatial distribution of pyroxene, plagioclase, and olivine on the surface of Vesta.

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“…; Cahill et al. , ; Li and Li ). The significant difference between the two models is in how they approximate different scattering processes for photons.…”

Section: Introductionmentioning

confidence: 97%

Estimating the modal mineralogy of eucrite and diogenite meteorites using visible–near infrared reflectance spectroscopy

Milliken

2015

Meteorit & Planetary Scien

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“…Additionally, the Fe 2 + absorption is affected by amorphization due to shock [Adams et al, 1979], resulting in a weaker 1.2-1.3 μm band and a shift in the main absorption feature toward 1 μm [Pieters, 1996;Johnson and Hörz, 2003]. Although estimates of plagioclase, pyroxene, and olivine abundances can be derived from VNIR spectra through nonlinear spectral unmixing (typically using the Hapke [1981, 1993]-or Shkuratov et al [1999-based implementations of radiative transfer theory [e.g., Tompkins and Pieters, 1999;Cahill et al, 2010]), Cahill et al [2010] found that plagioclase abundance is typically underestimated, while no single phase is correspondingly overestimated. Yamamoto et al [2010] Supporting Online Material (SOM) fit SP spectra (0.5-2.6 μm) for 6 out of 33 total regional detections with a radiative transfer-based intimate mixture model [Denevi et al, 2008].…”

Section: Introductionmentioning

confidence: 99%

Constraints on olivine‐rich rock types on the Moon as observed by Diviner and M³: Implications for the formation of the lunar crust

et al. 2016

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We place upper limits on lunar olivine abundance using midinfrared (5–25 µm) data from the Lunar Reconnaissance Orbiter Diviner Lunar Radiometer Experiment (Diviner) along with effective emissivity spectra of mineral mixtures in a simulated lunar environment. Olivine‐bearing, pyroxene‐poor lithologies have been identified on the lunar surface with visible‐near‐infrared (VNIR) observations. Since the Kaguya Spectral Profiler (SP) VNIR survey of olivine‐rich regions is the most complete to date, we focus this work on exposures identified by that study. We first confirmed the locations with VNIR data from the Moon Mineralogy Mapper (M3) instrument. We then developed a Diviner olivine index from our laboratory data which, along with M3 and Lunar Reconnaissance Orbiter Camera wide‐angle camera data, was used to select the geographic area over which Diviner emissivity data were extracted. We calculate upper limits on olivine abundance for these areas using laboratory emissivity spectra of anorthite‐forsterite mixtures acquired under lunar‐like conditions. We find that these exposures have widely varying olivine content. In addition, after applying an albedo‐based space weathering correction to the Diviner data, we find that none of the areas are unambiguously consistent with concentrations of forsterite exceeding 90 wt %, in contrast to the higher abundance estimates derived from VNIR data.

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“…This method allows a planetary spectrum to be modeled on the basis of optical properties determined for suspected constituents and assumptions regarding the physical state of the surface. Initial applications of radiative transfer theory, based upon work from Bruce Hapke [e.g., Hapke, 1981, to planetary spectra yield encouraging results [e.g., Harker et al, 2002;Birlan et al, 2007;Cahill et al, 2010;Emery et al, 2011]. The accuracy of such models is limited by the quality of the inputs (i.e., optical constants).…”

Section: Introductionmentioning

confidence: 99%

Near‐infrared optical constants of naturally occurring olivine and synthetic pyroxene as a function of mineral composition

et al. 2013

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[1] Radiative transfer theory will assist in determining olivine and pyroxene proportions and compositions from the surface of a planetary body composed of intimately mixed minerals. In order to use radiative transfer techniques, the model requires the optical constants of olivine and pyroxene. Optical constants are parameters that describe the degree light absorbed (k) and refracted (n) in a medium. Here we only parameterize k in the near infrared from 0.6 to 2.5 mm of natural olivine as a function of forsterite number and synthetic pyroxene with respect to wollastonite and ferrosilite number. In contrast to previous work, this study is an improvement on previous work because we have a diverse and larger sample size leading to robust optical parameters. Additionally, we characterize each k-spectrum with the modified Gaussian model (MGM). MGM is a physically realistic model of near-infrared absorptions due to electronic transitions. In each spectrum, we model each absorption and continuum with Gaussians and an inverse of a linear function, respectively. We find that our fitting routine characterizes the olivine and pyroxene k-spectra in a robust and consistent manner. Then we use regression analysis to characterize each parameter of the Gaussians and the continuum as a function of mineral composition. The developed optical parameters from this work will allow calculations of mineral proportions and compositions on planetary surfaces with use of data from missions such as Dawn, MESSENGER, SELENE, and Chandrayaan-1.

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Radiative transfer modeling of near‐infrared reflectance of lunar highland and mare soils

Cited by 15 publications

References 37 publications

Estimating the modal mineralogy of eucrite and diogenite meteorites using visible–near infrared reflectance spectroscopy

Estimating the modal mineralogy of eucrite and diogenite meteorites using visible–near infrared reflectance spectroscopy

Constraints on olivine‐rich rock types on the Moon as observed by Diviner and M³: Implications for the formation of the lunar crust

Near‐infrared optical constants of naturally occurring olivine and synthetic pyroxene as a function of mineral composition

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Radiative transfer modeling of near‐infrared reflectance of lunar highland and mare soils

Cited by 15 publications

References 37 publications

Estimating the modal mineralogy of eucrite and diogenite meteorites using visible–near infrared reflectance spectroscopy

Estimating the modal mineralogy of eucrite and diogenite meteorites using visible–near infrared reflectance spectroscopy

Constraints on olivine‐rich rock types on the Moon as observed by Diviner and M3: Implications for the formation of the lunar crust

Near‐infrared optical constants of naturally occurring olivine and synthetic pyroxene as a function of mineral composition

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Constraints on olivine‐rich rock types on the Moon as observed by Diviner and M³: Implications for the formation of the lunar crust