Stability of hydrated minerals on Mars

Edward A. Cloutis; Michael A. Craig; John F. Mustard; Roman V. Kruzelecky; Wes R. Jamroz; Alan Scott; David L. Bish; François Poulet; Jean Pierre Bibring; Penelope L. King

doi:10.1029/2007GL031267

Stability of hydrated minerals on Mars

Edward A. Cloutis^*, Michael A. Craig, John F. Mustard, Roman V. Kruzelecky, Wes R. Jamroz, Alan Scott, David L. Bish, François Poulet, Jean Pierre Bibring, Penelope L. King

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

45 Citations (Scopus)

Abstract

The validity of recent identification of various hydrated minerals (kieserite, gypsum, hexahydrite, nontronite, chamosite, and montmorillonite) on Mars was assessed by exposing these minerals to simulated Martian surface conditions of atmospheric composition and pressure, temperature, and ultraviolet light irradiation. When exposed to such conditions the hydrated minerals exhibit in general, greater losses of interlayer H₂O than structural OH. Minerals such as gypsum that contain structural H₂O are more resistant to H₂O loss than phyllosilicates. The partial loss of OH in some of the phyllosilicates is not accompanied by a measurable and systematic change in the wavelength position or intensity of metal-OH absorption bands. The characteristic absorption features that allow for identification of these minerals on Mars may be reduced in intensity, but are nevertheless largely preserved.

Original language	English
Article number	L20202
Journal	Geophysical Research Letters
Volume	34
Issue number	20
DOIs	https://doi.org/10.1029/2007GL031267
Publication status	Published - Oct 2007
Externally published	Yes

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title = "Stability of hydrated minerals on Mars",

abstract = "The validity of recent identification of various hydrated minerals (kieserite, gypsum, hexahydrite, nontronite, chamosite, and montmorillonite) on Mars was assessed by exposing these minerals to simulated Martian surface conditions of atmospheric composition and pressure, temperature, and ultraviolet light irradiation. When exposed to such conditions the hydrated minerals exhibit in general, greater losses of interlayer H2O than structural OH. Minerals such as gypsum that contain structural H2O are more resistant to H2O loss than phyllosilicates. The partial loss of OH in some of the phyllosilicates is not accompanied by a measurable and systematic change in the wavelength position or intensity of metal-OH absorption bands. The characteristic absorption features that allow for identification of these minerals on Mars may be reduced in intensity, but are nevertheless largely preserved.",

author = "Cloutis, {Edward A.} and Craig, {Michael A.} and Mustard, {John F.} and Kruzelecky, {Roman V.} and Jamroz, {Wes R.} and Alan Scott and Bish, {David L.} and Fran{\c c}ois Poulet and Bibring, {Jean Pierre} and King, {Penelope L.}",

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AU - Cloutis, Edward A.

AU - Craig, Michael A.

AU - Mustard, John F.

AU - Kruzelecky, Roman V.

AU - Jamroz, Wes R.

AU - Scott, Alan

AU - Bish, David L.

AU - Poulet, François

AU - Bibring, Jean Pierre

AU - King, Penelope L.

PY - 2007/10

Y1 - 2007/10

N2 - The validity of recent identification of various hydrated minerals (kieserite, gypsum, hexahydrite, nontronite, chamosite, and montmorillonite) on Mars was assessed by exposing these minerals to simulated Martian surface conditions of atmospheric composition and pressure, temperature, and ultraviolet light irradiation. When exposed to such conditions the hydrated minerals exhibit in general, greater losses of interlayer H2O than structural OH. Minerals such as gypsum that contain structural H2O are more resistant to H2O loss than phyllosilicates. The partial loss of OH in some of the phyllosilicates is not accompanied by a measurable and systematic change in the wavelength position or intensity of metal-OH absorption bands. The characteristic absorption features that allow for identification of these minerals on Mars may be reduced in intensity, but are nevertheless largely preserved.

AB - The validity of recent identification of various hydrated minerals (kieserite, gypsum, hexahydrite, nontronite, chamosite, and montmorillonite) on Mars was assessed by exposing these minerals to simulated Martian surface conditions of atmospheric composition and pressure, temperature, and ultraviolet light irradiation. When exposed to such conditions the hydrated minerals exhibit in general, greater losses of interlayer H2O than structural OH. Minerals such as gypsum that contain structural H2O are more resistant to H2O loss than phyllosilicates. The partial loss of OH in some of the phyllosilicates is not accompanied by a measurable and systematic change in the wavelength position or intensity of metal-OH absorption bands. The characteristic absorption features that allow for identification of these minerals on Mars may be reduced in intensity, but are nevertheless largely preserved.

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DO - 10.1029/2007GL031267

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SN - 0094-8276

VL - 34

JO - Geophysical Research Letters

JF - Geophysical Research Letters

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ER -

Stability of hydrated minerals on Mars

Abstract

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