Thermal infrared emission spectroscopy of anhydrous carbonates

Melissa D. Lane, Philip Christensen

Research output: Contribution to journalArticle

76 Citations (Scopus)

Abstract

The objective of this study is to present the thermal emission spectra of various anhydrous, calcite- and dolomite-series carbonate minerals to illustrate the effect of the structural cation (Ca 2+, Mg 2+, Fe 2+, Mn 2+, Zn 2+) on shifting the positions of the carbonate absorption bands. All of the carbonate mineral emission spectra included in this study exhibit three absorption features related to three specific vibrational modes of the carbonate anion (CO 3 2-). These anion vibrations include the out-of-plane bend, the asymmetric stretch, and the in-plane bend (i.e., the ν 2, ν 3, and ν 4 modes, respectively). The positions of the absorption-band emissivity minima are unique for each carbonate chemistry and are thus diagnostic of mineralogy. The average ν 2, ν 3, and ν 4 wavenumber positions for the various carbonate minerals are as follows: calcite (CaCO 3) 883, 1523, and 712 cm -1; magnesite (MgCO 3) 901, 1572, and 748 cm -1; siderite (FeCO 3) 876, 1523, and 736 cm -1; rhodochrosite (MnCO 3) 877, 1535, and 726 cm -1; smithsonite (ZnCO 3) 882, 1509, and 742 cm -1; dolomite (CaMg(CO 3) 2) 894, 1547, and 728 cm -1; and kutnahorite (CaMn(CO 3) 2) 882, 1526, and 716 cm -1. Carbonates as a general mineral class crystallize in a variety of geological environments; however, each specific carbonate mineralogy typically is limited to a narrow range of geologic settings in which it forms. Thermal infrared emission data to be received from the Mars Global Surveyor thermal emission spectrometer will contain the spectral signature of carbonates if they are present above the detectibility limit on the surface of Mars. This study presents the spectral information necessary to recognize carbonate as a mineral class as well as identify the specific type of carbonate from thermal emissivity data. Knowledge of distinct carbonate mineralogy will be useful for interpreting the environmental conditions that were present on Mars during the carbonate formation. The result of this study is that the major carbonate mineral species (calcite, dolomite, magnesite, siderite, and smithsonite) can be identified from thermal infrared emission data, provided moderate (10 cm -1) spectral sampling. Because of the similarity of absorption band positions between kutnahorite and calcite, high (2 cm -1) spectral sampling is required to distinguish kutnahorite. Moderate spectral sampling data are also sufficient to determine the amount of Mg and Fe in Mg-Fe solid solution minerals to within 3-5% of the cation abundance.

Original languageEnglish (US)
Article number97JE02046
Pages (from-to)25581-25592
Number of pages12
JournalJournal of Geophysical Research E: Planets
Volume102
Issue numberE11
StatePublished - 1997

Fingerprint

Carbonates
Emission spectroscopy
Carbonate minerals
Infrared spectroscopy
carbonates
spectroscopy
carbonate
Calcium Carbonate
minerals
Minerals
Absorption spectra
calcite
mineral
Carbon Monoxide
Sampling
mineralogy
Anions
Cations
siderites
dolomite

Keywords

  • Adsorption isotopic effects
  • Adsorption-desorption
  • Collision-induced dissociation
  • Gas mass spectrometry
  • Guanine
  • Isotope amount ratios
  • Leak rate
  • Methylguanines
  • Nucleic acid bases
  • Silicon tetrafluoride

ASJC Scopus subject areas

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

Cite this

Thermal infrared emission spectroscopy of anhydrous carbonates. / Lane, Melissa D.; Christensen, Philip.

In: Journal of Geophysical Research E: Planets, Vol. 102, No. E11, 97JE02046, 1997, p. 25581-25592.

Research output: Contribution to journalArticle

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abstract = "The objective of this study is to present the thermal emission spectra of various anhydrous, calcite- and dolomite-series carbonate minerals to illustrate the effect of the structural cation (Ca 2+, Mg 2+, Fe 2+, Mn 2+, Zn 2+) on shifting the positions of the carbonate absorption bands. All of the carbonate mineral emission spectra included in this study exhibit three absorption features related to three specific vibrational modes of the carbonate anion (CO 3 2-). These anion vibrations include the out-of-plane bend, the asymmetric stretch, and the in-plane bend (i.e., the ν 2, ν 3, and ν 4 modes, respectively). The positions of the absorption-band emissivity minima are unique for each carbonate chemistry and are thus diagnostic of mineralogy. The average ν 2, ν 3, and ν 4 wavenumber positions for the various carbonate minerals are as follows: calcite (CaCO 3) 883, 1523, and 712 cm -1; magnesite (MgCO 3) 901, 1572, and 748 cm -1; siderite (FeCO 3) 876, 1523, and 736 cm -1; rhodochrosite (MnCO 3) 877, 1535, and 726 cm -1; smithsonite (ZnCO 3) 882, 1509, and 742 cm -1; dolomite (CaMg(CO 3) 2) 894, 1547, and 728 cm -1; and kutnahorite (CaMn(CO 3) 2) 882, 1526, and 716 cm -1. Carbonates as a general mineral class crystallize in a variety of geological environments; however, each specific carbonate mineralogy typically is limited to a narrow range of geologic settings in which it forms. Thermal infrared emission data to be received from the Mars Global Surveyor thermal emission spectrometer will contain the spectral signature of carbonates if they are present above the detectibility limit on the surface of Mars. This study presents the spectral information necessary to recognize carbonate as a mineral class as well as identify the specific type of carbonate from thermal emissivity data. Knowledge of distinct carbonate mineralogy will be useful for interpreting the environmental conditions that were present on Mars during the carbonate formation. The result of this study is that the major carbonate mineral species (calcite, dolomite, magnesite, siderite, and smithsonite) can be identified from thermal infrared emission data, provided moderate (10 cm -1) spectral sampling. Because of the similarity of absorption band positions between kutnahorite and calcite, high (2 cm -1) spectral sampling is required to distinguish kutnahorite. Moderate spectral sampling data are also sufficient to determine the amount of Mg and Fe in Mg-Fe solid solution minerals to within 3-5{\%} of the cation abundance.",
keywords = "Adsorption isotopic effects, Adsorption-desorption, Collision-induced dissociation, Gas mass spectrometry, Guanine, Isotope amount ratios, Leak rate, Methylguanines, Nucleic acid bases, Silicon tetrafluoride",
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AU - Christensen, Philip

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N2 - The objective of this study is to present the thermal emission spectra of various anhydrous, calcite- and dolomite-series carbonate minerals to illustrate the effect of the structural cation (Ca 2+, Mg 2+, Fe 2+, Mn 2+, Zn 2+) on shifting the positions of the carbonate absorption bands. All of the carbonate mineral emission spectra included in this study exhibit three absorption features related to three specific vibrational modes of the carbonate anion (CO 3 2-). These anion vibrations include the out-of-plane bend, the asymmetric stretch, and the in-plane bend (i.e., the ν 2, ν 3, and ν 4 modes, respectively). The positions of the absorption-band emissivity minima are unique for each carbonate chemistry and are thus diagnostic of mineralogy. The average ν 2, ν 3, and ν 4 wavenumber positions for the various carbonate minerals are as follows: calcite (CaCO 3) 883, 1523, and 712 cm -1; magnesite (MgCO 3) 901, 1572, and 748 cm -1; siderite (FeCO 3) 876, 1523, and 736 cm -1; rhodochrosite (MnCO 3) 877, 1535, and 726 cm -1; smithsonite (ZnCO 3) 882, 1509, and 742 cm -1; dolomite (CaMg(CO 3) 2) 894, 1547, and 728 cm -1; and kutnahorite (CaMn(CO 3) 2) 882, 1526, and 716 cm -1. Carbonates as a general mineral class crystallize in a variety of geological environments; however, each specific carbonate mineralogy typically is limited to a narrow range of geologic settings in which it forms. Thermal infrared emission data to be received from the Mars Global Surveyor thermal emission spectrometer will contain the spectral signature of carbonates if they are present above the detectibility limit on the surface of Mars. This study presents the spectral information necessary to recognize carbonate as a mineral class as well as identify the specific type of carbonate from thermal emissivity data. Knowledge of distinct carbonate mineralogy will be useful for interpreting the environmental conditions that were present on Mars during the carbonate formation. The result of this study is that the major carbonate mineral species (calcite, dolomite, magnesite, siderite, and smithsonite) can be identified from thermal infrared emission data, provided moderate (10 cm -1) spectral sampling. Because of the similarity of absorption band positions between kutnahorite and calcite, high (2 cm -1) spectral sampling is required to distinguish kutnahorite. Moderate spectral sampling data are also sufficient to determine the amount of Mg and Fe in Mg-Fe solid solution minerals to within 3-5% of the cation abundance.

AB - The objective of this study is to present the thermal emission spectra of various anhydrous, calcite- and dolomite-series carbonate minerals to illustrate the effect of the structural cation (Ca 2+, Mg 2+, Fe 2+, Mn 2+, Zn 2+) on shifting the positions of the carbonate absorption bands. All of the carbonate mineral emission spectra included in this study exhibit three absorption features related to three specific vibrational modes of the carbonate anion (CO 3 2-). These anion vibrations include the out-of-plane bend, the asymmetric stretch, and the in-plane bend (i.e., the ν 2, ν 3, and ν 4 modes, respectively). The positions of the absorption-band emissivity minima are unique for each carbonate chemistry and are thus diagnostic of mineralogy. The average ν 2, ν 3, and ν 4 wavenumber positions for the various carbonate minerals are as follows: calcite (CaCO 3) 883, 1523, and 712 cm -1; magnesite (MgCO 3) 901, 1572, and 748 cm -1; siderite (FeCO 3) 876, 1523, and 736 cm -1; rhodochrosite (MnCO 3) 877, 1535, and 726 cm -1; smithsonite (ZnCO 3) 882, 1509, and 742 cm -1; dolomite (CaMg(CO 3) 2) 894, 1547, and 728 cm -1; and kutnahorite (CaMn(CO 3) 2) 882, 1526, and 716 cm -1. Carbonates as a general mineral class crystallize in a variety of geological environments; however, each specific carbonate mineralogy typically is limited to a narrow range of geologic settings in which it forms. Thermal infrared emission data to be received from the Mars Global Surveyor thermal emission spectrometer will contain the spectral signature of carbonates if they are present above the detectibility limit on the surface of Mars. This study presents the spectral information necessary to recognize carbonate as a mineral class as well as identify the specific type of carbonate from thermal emissivity data. Knowledge of distinct carbonate mineralogy will be useful for interpreting the environmental conditions that were present on Mars during the carbonate formation. The result of this study is that the major carbonate mineral species (calcite, dolomite, magnesite, siderite, and smithsonite) can be identified from thermal infrared emission data, provided moderate (10 cm -1) spectral sampling. Because of the similarity of absorption band positions between kutnahorite and calcite, high (2 cm -1) spectral sampling is required to distinguish kutnahorite. Moderate spectral sampling data are also sufficient to determine the amount of Mg and Fe in Mg-Fe solid solution minerals to within 3-5% of the cation abundance.

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KW - Adsorption-desorption

KW - Collision-induced dissociation

KW - Gas mass spectrometry

KW - Guanine

KW - Isotope amount ratios

KW - Leak rate

KW - Methylguanines

KW - Nucleic acid bases

KW - Silicon tetrafluoride

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