Emission spectroscopy of clay minerals and evidence for poorly crystalline aluminosilicates on Mars from Thermal Emission Spectrometer data

Joseph R. Michalski, Michael D. Kraft, Thomas Sharp, Lynda Williams, Philip Christensen

Research output: Contribution to journalArticle

54 Citations (Scopus)

Abstract

To understand the aqueous history of Mars, it is critical to constrain the alteration mineralogy of the Martian surface. Previously published analyses of thermal infrared (λ = 6-25 μm) remote sensing data of Mars suggest that dark regions have ∼15-20% clay minerals. However, near-infrared (λ = 1-3 μm) spectral results generally do not identify widespread clay minerals. Thermal infrared detections of clays on Mars are difficult to interpret owing in part to the relative paucity of published spectral analyses of clay minerals and clay-bearing materials using similar spectra (thermal infrared emission spectra). In this study, we present an analysis of the thermal emission spectral features (λ = ∼6-25 μm or 400-1650 cm-1) of a suite of clay mineral reference materials and clay-bearing rocks, linking their spectral features to the crystal chemical properties of the clays. On the basis of this context provided by the emission spectral analysis of clay minerals and clay-bearing rocks, we reconsider the evidence for clay minerals on Mars from Thermal Emission Spectrometer (TES) results. We propose that global-scale clay abundances determined from TES probably represent a geologically significant surface component, though they may actually correspond to poorly crystalline aluminosilicates with similar Si/O ratios to clay minerals (0.3-0.4), rather than well-crystalline clays. If clay minerals or clay-like materials on Mars are poorly crystalline and/or dessicated, they may be detectable in the thermal infrared, but not easily detected with near-infrared data sets.

Original languageEnglish (US)
Article numberE03004
JournalJournal of Geophysical Research E: Planets
Volume111
Issue number3
DOIs
StatePublished - Mar 20 2006

Fingerprint

Emission spectroscopy
aluminosilicate
thermal emission
Clay minerals
mars
clays
clay mineral
Spectrometers
Mars
spectrometer
spectroscopy
minerals
spectrometers
Crystalline materials
clay
Bearings (structural)
Infrared radiation
near infrared
Rocks
Mineralogy

ASJC Scopus subject areas

  • Oceanography
  • Astronomy and Astrophysics
  • Atmospheric Science
  • Space and Planetary Science
  • Earth and Planetary Sciences (miscellaneous)
  • Geophysics
  • Geochemistry and Petrology

Cite this

@article{65d1d794d5d745f18354f25d864a4ee3,
title = "Emission spectroscopy of clay minerals and evidence for poorly crystalline aluminosilicates on Mars from Thermal Emission Spectrometer data",
abstract = "To understand the aqueous history of Mars, it is critical to constrain the alteration mineralogy of the Martian surface. Previously published analyses of thermal infrared (λ = 6-25 μm) remote sensing data of Mars suggest that dark regions have ∼15-20{\%} clay minerals. However, near-infrared (λ = 1-3 μm) spectral results generally do not identify widespread clay minerals. Thermal infrared detections of clays on Mars are difficult to interpret owing in part to the relative paucity of published spectral analyses of clay minerals and clay-bearing materials using similar spectra (thermal infrared emission spectra). In this study, we present an analysis of the thermal emission spectral features (λ = ∼6-25 μm or 400-1650 cm-1) of a suite of clay mineral reference materials and clay-bearing rocks, linking their spectral features to the crystal chemical properties of the clays. On the basis of this context provided by the emission spectral analysis of clay minerals and clay-bearing rocks, we reconsider the evidence for clay minerals on Mars from Thermal Emission Spectrometer (TES) results. We propose that global-scale clay abundances determined from TES probably represent a geologically significant surface component, though they may actually correspond to poorly crystalline aluminosilicates with similar Si/O ratios to clay minerals (0.3-0.4), rather than well-crystalline clays. If clay minerals or clay-like materials on Mars are poorly crystalline and/or dessicated, they may be detectable in the thermal infrared, but not easily detected with near-infrared data sets.",
author = "Michalski, {Joseph R.} and Kraft, {Michael D.} and Thomas Sharp and Lynda Williams and Philip Christensen",
year = "2006",
month = "3",
day = "20",
doi = "10.1029/2005JE002438",
language = "English (US)",
volume = "111",
journal = "Journal of Geophysical Research: Atmospheres",
issn = "2169-897X",
publisher = "Wiley-Blackwell",
number = "3",

}

TY - JOUR

T1 - Emission spectroscopy of clay minerals and evidence for poorly crystalline aluminosilicates on Mars from Thermal Emission Spectrometer data

AU - Michalski, Joseph R.

AU - Kraft, Michael D.

AU - Sharp, Thomas

AU - Williams, Lynda

AU - Christensen, Philip

PY - 2006/3/20

Y1 - 2006/3/20

N2 - To understand the aqueous history of Mars, it is critical to constrain the alteration mineralogy of the Martian surface. Previously published analyses of thermal infrared (λ = 6-25 μm) remote sensing data of Mars suggest that dark regions have ∼15-20% clay minerals. However, near-infrared (λ = 1-3 μm) spectral results generally do not identify widespread clay minerals. Thermal infrared detections of clays on Mars are difficult to interpret owing in part to the relative paucity of published spectral analyses of clay minerals and clay-bearing materials using similar spectra (thermal infrared emission spectra). In this study, we present an analysis of the thermal emission spectral features (λ = ∼6-25 μm or 400-1650 cm-1) of a suite of clay mineral reference materials and clay-bearing rocks, linking their spectral features to the crystal chemical properties of the clays. On the basis of this context provided by the emission spectral analysis of clay minerals and clay-bearing rocks, we reconsider the evidence for clay minerals on Mars from Thermal Emission Spectrometer (TES) results. We propose that global-scale clay abundances determined from TES probably represent a geologically significant surface component, though they may actually correspond to poorly crystalline aluminosilicates with similar Si/O ratios to clay minerals (0.3-0.4), rather than well-crystalline clays. If clay minerals or clay-like materials on Mars are poorly crystalline and/or dessicated, they may be detectable in the thermal infrared, but not easily detected with near-infrared data sets.

AB - To understand the aqueous history of Mars, it is critical to constrain the alteration mineralogy of the Martian surface. Previously published analyses of thermal infrared (λ = 6-25 μm) remote sensing data of Mars suggest that dark regions have ∼15-20% clay minerals. However, near-infrared (λ = 1-3 μm) spectral results generally do not identify widespread clay minerals. Thermal infrared detections of clays on Mars are difficult to interpret owing in part to the relative paucity of published spectral analyses of clay minerals and clay-bearing materials using similar spectra (thermal infrared emission spectra). In this study, we present an analysis of the thermal emission spectral features (λ = ∼6-25 μm or 400-1650 cm-1) of a suite of clay mineral reference materials and clay-bearing rocks, linking their spectral features to the crystal chemical properties of the clays. On the basis of this context provided by the emission spectral analysis of clay minerals and clay-bearing rocks, we reconsider the evidence for clay minerals on Mars from Thermal Emission Spectrometer (TES) results. We propose that global-scale clay abundances determined from TES probably represent a geologically significant surface component, though they may actually correspond to poorly crystalline aluminosilicates with similar Si/O ratios to clay minerals (0.3-0.4), rather than well-crystalline clays. If clay minerals or clay-like materials on Mars are poorly crystalline and/or dessicated, they may be detectable in the thermal infrared, but not easily detected with near-infrared data sets.

UR - http://www.scopus.com/inward/record.url?scp=33646430319&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=33646430319&partnerID=8YFLogxK

U2 - 10.1029/2005JE002438

DO - 10.1029/2005JE002438

M3 - Article

VL - 111

JO - Journal of Geophysical Research: Atmospheres

JF - Journal of Geophysical Research: Atmospheres

SN - 2169-897X

IS - 3

M1 - E03004

ER -