Sequestration of Martian CO2 by mineral carbonation

Tomkinson, T.; Lee, Martin; Mark, Darren F.; Smith, C. L.

doi:10.1038/ncomms3662

Cited by 55 publications

(93 citation statements)

References 36 publications

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“…The presence of secondary minerals within the mesostasis gives it a light brown colour when viewed using plane polarised transmitted light. Meunier et al (2012) interpreted the phyllosilicate-rich mesostasis to be a precipitate from late-stage magmatic fluids, whereas Tomkinson et al (2013a) concluded that phyllosilicate and siderite had formed by the water-mediated replacement of plagioclase feldspar.…”

Section: Mineralogy Of Lafayettementioning

confidence: 97%

“…Areas of mesostasis are $100 to 600 lm across (Fig. 1a) and are dominated either by plagioclase feldspar (Ab 62.6 An 31.8 Or 5.6 ; Bunch and Reid, 1975; Table 1) or phyllosilicate that is often intergrown with siderite (Tomkinson et al, 2013a). The presence of secondary minerals within the mesostasis gives it a light brown colour when viewed using plane polarised transmitted light.…”

Section: Mineralogy Of Lafayettementioning

confidence: 98%

“…If replacement were centripetal (i.e., from the vein axis outwards, and thus from the margin of the unaltered reactant mineral towards its interior), as is typical for serpentinisation of terrestrial olivine (e.g., Delvigne et al, 1979;Velbel, 1984Velbel, , 1993Velbel, , 2012, the first formed minerals will be on the vein axis. Our initial study of aqueous alteration of Lafayette focused on the origin of siderite within grains of olivine and the intercumulate mesostasis as revealed by SEM imaging (Tomkinson et al, 2013a). Here we have built on this earlier work by investigating the mineralogy and nanoscale microstructure of iddingsite veins in augite and olivine grains using a suite of high resolution electron imaging and diffraction techniques.…”

Section: Introductionmentioning

confidence: 97%

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Formation of iddingsite veins in the martian crust by centripetal replacement of olivine: Evidence from the nakhlite meteorite Lafayette

Lee

Tomkinson

Hallis

et al. 2015

Geochimica et Cosmochimica Acta

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The Lafayette meteorite is an olivine clinopyroxenite that crystallized on Mars $1300 million years ago within a lava flow or shallow sill. Liquid water entered this igneous rock $700 million years later to produce a suite of secondary minerals, collectively called 'iddingsite', that occur as veins within grains of augite and olivine. The deuterium/hydrogen ratio of water within these secondary minerals shows that the aqueous solutions were sourced from one or more near-surface reservoirs. Several petrographically distinct types of veins can be recognised by differences in their width, shape, and crystallographic orientation. Augite and olivine both contain veins of a very fine grained hydrous Fe-and Mg-rich silicate that are $1-2 lm in width and lack any preferred crystallographic orientation. These narrow veins formed by cementation of pore spaces that had been opened by fracturing and probably in response to shock. The subset of olivine-hosted veins whose axes lie parallel to (0 0 1) have serrated walls, and formed by widening of the narrow veins by interface coupled dissolution-precipitation. Widening started by replacement of the walls of the narrow precursor veins by Fe-Mg silicate, and a crystallographic control on the trajectory of the dissolution-precipitation front created micrometre-scale {1 1 1} serrations. The walls of many of the finely serrated veins were subsequently replaced by siderite, and the solutions responsible for carbonation of olivine also partially recrystallized the Fe-Mg silicate. Smectite was the last mineral to form and grew by replacement of siderite. This mineralization sequence shows that Lafayette was exposed to two discrete pulses of aqueous solutions, the first of which formed the Fe-Mg silicate, and the second mediated replacement of vein walls by siderite and smectite. The similarity in size, shape and crystallographic orientation of iddingsite veins in the Lafayette meteorite and in terrestrial basalts demonstrates a common microstructural control on water-mineral interaction between Mars and Earth, and indicates that prior shock deformation was not a prerequisite for aqueous alteration of the martian crust.

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Section: Mineralogy Of Lafayettementioning

confidence: 97%

Section: Mineralogy Of Lafayettementioning

confidence: 98%

Section: Introductionmentioning

confidence: 97%

See 1 more Smart Citation

Formation of iddingsite veins in the martian crust by centripetal replacement of olivine: Evidence from the nakhlite meteorite Lafayette

Lee

Tomkinson

Hallis

et al. 2015

Geochimica et Cosmochimica Acta

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“…Tomkinson et al [40] showed that olivine and a plagioclase feldspar-rich mesostasis in the meteorite have been replaced by carbonate over geological timescales. The susceptibility of olivine to replacement was enhanced by the presence of smectite veins along which CO 2 -rich fluids gained access to grain interiors.…”

Section: +mentioning

confidence: 98%

Mineralization of Carbon Dioxide: A Literature Review

et al. 2015

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Research on carbon capture and storage has been focused on CO 2 storage in geologic formations, with many potential risks. An alternative to conventional geologic storage is carbon mineralization, where CO 2 is reacted with metal cations to form carbonate minerals. Mineralization methods can be broadly divided into two categories: in situ and ex situ. In situ mineralization, or mineral trapping, is a component of underground geologic sequestration, in which a portion of the injected CO 2 reacts with alkaline rock present in the target formation to form solid carbonate species. In ex situ mineralization, the carbonation reaction occurs above ground, within a separate reactor or industrial process. This literature review is meant to provide an update on the current status of research on CO 2 mineralization.

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“…The example used in the discussion by Edwards and Ehlmann of the possibility of deep diffuse carbonate alteration-rather than precipitation of carbonate in discrete rock deposits like those analyzedwas selected based on measurements of carbonate in dust, in-situ mission data, and meteorites. That is, a 1 km global crustal layer of 1 vol.% carbonate-bearing materials, similar to the abundances in the Nakhaliteclass Lafayette meteorite (Changela and Bridges, 2010;Nyquist et al, 2001;Tomkinson et al, 2013;Wright et al, 1992), if formed from waters in contact with the atmosphere, would lead to sequestration of ~500 mbar CO 2 .…”

mentioning

confidence: 99%