The role of H<sub>2</sub>O in Martian magmatic systems

Mysen, Bjørn O.; Virgo, David; Popp, Robert; Bertka, C. M.

doi:10.2138/am-1998-9-1002

Cited by 69 publications

(55 citation statements)

References 17 publications

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“…The highest emission shifted from 880 to 1 030 cm Ϫ1 by increasing silica content from 9 to 100 mass%. This tendency agrees with those reported in the literature 11) where the wave number of silicate absorption increases with increasing the ratio bridging/non-bridging oxygen for a silicon.…”

supporting

confidence: 93%

Infrared Emission Spectra of CaF2-CaO-SiO2 Melt.

et al. 2000

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The infrared emission spectra of CaF 2 -CaO-SiO 2 melt were investigated by a method combining infrared emission spectroscopy and the hot-filament technique. Emission for spectra related to Si-O bond can be observed by this in situ technique. The influence of SiO 2 and fluoride content on the spectrum was investigated, and the emission attributable to bonds corresponding to silicon-bridging oxygen and silicon-non bridging oxygen was discussed. Results suggest that fluoride ion dominantly substitutes for a non-bridging bond in low SiO 2 concentration region. The structure of silicate was compared with calculated infrared emission of Si-F-O.

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confidence: 93%

Infrared Emission Spectra of CaF2-CaO-SiO2 Melt.

et al. 2000

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“…In the case of the Martian meteorites, it is also possible that in situ weathering occurred before the fragment was ejected from Mars-this, of course, in part depends on the availability of surface water and the ancient Martian climate. Studies of pre-eruptive water content of the Martian basalts have suggested possible ranges between a few hundred ppm H 2 O (Mysen et al 1998) to nearly 2 wt% (Dann et al 2001), although these results have been thought to be problematic (see Herd et al 2005 for discussion). Interestingly, secondary mineral inclusions of calcite and gypsum have been found in the shergottite EET A79001, and Gooding et al (1987) suggest that these minerals formed while the host material was on Mars.…”

Section: Discussionmentioning

confidence: 99%

Physical properties of Martian meteorites: Porosity and density measurements

Coulson

Beech

Nie

2007

Meteorit & Planetary Scien

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Abstract-Martian meteorites are fragments of the Martian crust. These samples represent igneous rocks, much like basalt. As such, many laboratory techniques designed for the study of Earth materials have been applied to these meteorites. Despite numerous studies of Martian meteorites, little data exists on their basic structural characteristics, such as porosity or density, information that is important in interpreting their origin, shock modification, and cosmic ray exposure history. Analysis of these meteorites provides both insight into the various lithologies present as well as the impact history of the planet's surface. We present new data relating to the physical characteristics of twelve Martian meteorites. Porosity was determined via a combination of scanning electron microscope (SEM) imagery/image analysis and helium pycnometry, coupled with a modified Archimedean method for bulk density measurements. Our results show a range in porosity and density values and that porosity tends to increase toward the edge of the sample. Preliminary interpretation of the data demonstrates good agreement between porosity measured at 100× and 300× magnification for the shergottite group, while others exhibit more variability. In comparison with the limited existing data for Martian meteorites we find fairly good agreement, although our porosity values typically lie at the low end of published values. Surprisingly, despite the increased data set, there is little by way of correlation between either porosity or density with parameters such as shock effect or terrestrial residency. Further data collection on additional meteorite samples is required before more definitive statements can be made concerning the validity of these observations.

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“…It has been reported that the fraction of Fe 3ϩ (or Fe 2ϩ ) ions to the total iron ions determined by Mössbauer spectroscopy and wet-chemical techniques are the same within these uncertainties. [17][18][19] The Doppler velocity scale for the measurements was calibrated at room temperature using the spectrum of a-Fe foil. concentrations and the increase of CaO concentration were observed during melting for the samples of series 1-3, probably owing to the vaporization of SiF 4 and HF.…”

Section: Measurementsmentioning

confidence: 99%

“…as a function of the value of (mol%CaO)/(mol%SiO 2 ) for the samples of series 4, 5 and 6. The values of (mol%CaO)/(mol%SiO 2 ) were obtained from the analyzed chemical compositions shown in Table 1 23) have proposed the following redox equilibrium model of iron ions involving the anionic structural units. …”

Section: Figmentioning

confidence: 99%

Effect of Fluorine on Silicate Network for CaO-CaF2-SiO2 and CaO-CaF2-SiO2-FeOx Glasses.

et al. 2002

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The chemical state of fluorine and the effect of fluorine addition on the degree of polymerization of silicate network have been investigated for the CaO-SiO 2 -CaF 2 and CaO-SiO 2 -CaF 2 -FeO x glasses using the Xray photoelectron spectroscopy (XPS) and Mössbauer spectroscopy measurements. The F1s XPS spectra indicate that the fluorine is dominantly coordinated with calcium rather than silicon. The O1s XPS spectra for the CaO-SiO 2 -CaF 2 glasses and the values of Fe 2ϩ /Fe 3ϩ obtained by Mössbauer spectra for the CaO-SiO 2 -CaF 2 -FeO x glasses indicate that CaF 2 addition does not depolymerize the silicate network for both systems.KEY WORDS: chemical state of fluorine; polymerization; silicate network; X-ray photoelectron spectroscopy; Mössbauer spectroscopy.

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The role of H₂O in Martian magmatic systems

Cited by 69 publications

References 17 publications

Infrared Emission Spectra of CaF2-CaO-SiO2 Melt.

Infrared Emission Spectra of CaF2-CaO-SiO2 Melt.

Physical properties of Martian meteorites: Porosity and density measurements

Effect of Fluorine on Silicate Network for CaO-CaF2-SiO2 and CaO-CaF2-SiO2-FeOx Glasses.

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The role of H2O in Martian magmatic systems

Cited by 69 publications

References 17 publications

Infrared Emission Spectra of CaF2-CaO-SiO2 Melt.

Infrared Emission Spectra of CaF2-CaO-SiO2 Melt.

Physical properties of Martian meteorites: Porosity and density measurements

Effect of Fluorine on Silicate Network for CaO-CaF2-SiO2 and CaO-CaF2-SiO2-FeOx Glasses.

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The role of H₂O in Martian magmatic systems