Reflectance spectroscopy of palagonite and iron-rich montmorillonite clay mixtures: Implications for the surface composition of Mars

Orenberg, J. B.; Handy, J.

doi:10.1016/0019-1035(92)90076-j

Cited by 28 publications

(23 citation statements)

References 27 publications

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“…Palagonitic soils are an amorphous weathering product of basaltic glass that often have a similar bulk chemical composition to smectite clay-iron oxide/oxyhydroxide mixtures. Their mineralogy in general is variable and may reflect starting composition and the weathering environment (e.g., Singer 1982, Crisp and Bartholomew 1992, Orenberg and Handy 1992, Bishop et al 1998. Visible to near infrared spectra of many palagonitic soils are close matches to remotely acquired spectra of Mars.…”

Section: Figmentioning

confidence: 94%

“…Visible to near infrared spectra of many palagonitic soils are close matches to remotely acquired spectra of Mars. Many of these samples have well-developed water features (1.4-and 1.9-µm absorptions) and often exhibit weak 2.2-µm absorptions due to the presence of smectite clays, allophane, or incipient phyllosilicates (e.g., Crisp and Bartholomew 1992, Orenberg and Handy 1992. The amorphous portion of Hawaiian soils is converted with time into phyllosilicates and other crystalline alteration products (Vitousek et al 1997).…”

Section: Figmentioning

confidence: 97%

“…Researchers have used the absence of a strong 2.2-µm feature to place upper limits on the abundance of clays on the surface of Mars (e.g., Orenberg andHandy 1992, Dalton andClark 1995). If analog materials with inappropriate particle sizes or crystallinities are used then estimates of phyllosilicate or other component abundances will be inaccurate.…”

Section: Implications and Conclusionmentioning

confidence: 99%

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Effects of Very Fine Particle Size on Reflectance Spectra of Smectite and Palagonitic Soil

Cooper¹

1999

Icarus

105

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Section: Figmentioning

confidence: 94%

Section: Figmentioning

confidence: 97%

Section: Implications and Conclusionmentioning

confidence: 99%

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Effects of Very Fine Particle Size on Reflectance Spectra of Smectite and Palagonitic Soil

Cooper¹

1999

Icarus

105

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“…The high reflectance of zeolites in the visible and near-infrared wavelength region can easily be reduced, and the absorption bands reduced in intensity, by small quantities of intimately mixed opaque minerals [Clark, 1983;Orenberg and Handy, 1992]. In this sense they are similar to other common hydrated aluminosilicates such as kaolinite and montmorillonite [e.g., Clark et al 1990].…”

Section: Remote Sensing Implicationsmentioning

confidence: 99%

Spectral reflectance properties of zeolites and remote sensing implications

2002

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[1] The 0.3-to 26-mm reflectance spectra of a suite of 28 zeolites were measured and analyzed to derive spectral-compositional-structural relationships. Below $7 mm, the spectra are largely dominated by absorption features associated with zeolitic water. At longer wavelengths, the spectra are dominated by absorption features associated with the aluminosilicate framework. The spectra exhibit a number of systematic variations which can be used for both structural and compositional determinations. These include: (1) distinguishing different structural groups on the basis of wavelength position variations associated with absorption features in the 8.5-to 26-mm region that are related to differences in the structure of the aluminosilicate framework; (2) determining the major cation which is present (Ca, Na, K) and the associated electronic environment of the zeolitic water on the basis of how these cations hydrogen bond to the water molecules in the void spaces and consequently affect water-related absorption band positions, particularly in the 1.4, 1.9, and 2.0-to 2.5-mm regions; (3) determining the Al:(Al + Si) ratio and SCFM chemical index on the basis of absorption features in the 7-to 26-mm region which are most sensitive to these compositional variations; and (4) identifying ironbearing zeolites on the basis of absorption features in the 0.35-to 0.9-mm region. The wavelength position and number of H 2 O-associated absorption bands are sensitive to factors such as the type of major cation, degree of hydrogen bonding, and size of the void space, all of which are somewhat interrelated.

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“…Based on the desertic origin of our cosmic dust analogue, we can assume hematite (Jeong & Nousiainen 2014;Kemppinen et al 2015) and clay particles (Banin et al 1988;Orenberg & Handy 1992) as good candidates for simulating its internal and external inhomogeneities. Hematite is also found on Mars (Kula & Baldwin 2012), and is of interest in the study of the history of water on the planet.…”

Section: Input Matricesmentioning

confidence: 99%

Scattering Properties of Large Irregular Cosmic Dust Particles at Visible Wavelengths

Escobar-Cerezo

Palmer

Muñoz

et al. 2017

ApJ

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The effect of internal inhomogeneities and surface roughness on the scattering behavior of large cosmic dust particles is studied by comparing model simulations with laboratory measurements. The present work shows the results of an attempt to model a dust sample measured in the laboratory with simulations performed by a ray-optics model code. We consider this dust sample as a good analogue for interplanetary and interstellar dust as it shares its refractive index with known materials in these media. Several sensitivity tests have been performed for both structural cases (internal inclusions and surface roughness). Three different samples have been selected to mimic inclusion/coating inhomogeneities: two measured scattering matrices of hematite and white clay, and a simulated matrix for water ice. These three matrices are selected to cover a wide range of imaginary refractive indices. The selection of these materials also seeks to study astrophysical environments of interest such as Mars, where hematite and clays have been detected, and comets. Based on the results of the sensitivity tests shown in this work, we perform calculations for a size distribution of a silicate-type host particle model with inclusions and surface roughness to reproduce the experimental measurements of a dust sample. The model fits the measurements quite well, proving that surface roughness and internal structure play a role in the scattering pattern of irregular cosmic dust particles.

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Reflectance spectroscopy of palagonite and iron-rich montmorillonite clay mixtures: Implications for the surface composition of Mars

Cited by 28 publications

References 27 publications

Effects of Very Fine Particle Size on Reflectance Spectra of Smectite and Palagonitic Soil

Effects of Very Fine Particle Size on Reflectance Spectra of Smectite and Palagonitic Soil

Spectral reflectance properties of zeolites and remote sensing implications

Scattering Properties of Large Irregular Cosmic Dust Particles at Visible Wavelengths

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