Calculated aqueous-solution-solid-solution relations in the low-temperature system CaO-MgO-FeO-CO2-H2O

Woods, Terri L.; Garrels, Robert M.

doi:10.1016/0016-7037(92)90288-t

Cited by 27 publications

(13 citation statements)

References 60 publications

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“…They contain about 26-71 mol% of the CaFe(CO 3 ) 2 component, which appears to be the maximum possible iron content for any temperature. Standard state Gibbs free energy of formation and enthalpy of end-member CaFe(CO 3 ) 2 were 116.86 kJ/mol and −17.47 kJ/mol, respectively, from Woods and Garrels (1992). The ankerite composition chosen for the present work was CaFe 0.6 Mg 0.4 (CO 3 ) 2 which correspond to a solid solution of 0.4 dolomite and 0.6 ankerite.…”

Section: Thermodynamic Datamentioning

confidence: 99%

On the potential of CO2–water–rock interactions for CO2 storage using a modified kinetic model

Pham

Lü

Aagaard

et al. 2011

International Journal of Greenhouse Gas Control

137

112

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a b s t r a c tDuring CO 2 storage, mineral trapping is the safest long-term storage mechanism, and it is therefore important to estimate the correct CO 2 portion trapped in secondary mineral phases. The storage potential for cold, quartz-rich reservoirs, hereafter termed Utsira-type reservoirs, were solved using the numerical code PHREEQC, using a rate model that took into account both nucleation and growth of secondary mineral phases. This represented a modification of earlier simulations where growth rates were calculated from dissolution rate data. Because growth rate and nucleation rate parameters were largely unknown for the secondary carbonates, we did a sensitivity study on the potential for carbonate growth on rate parameters.The simulations suggest that the total amount of CO 2 trapped as mineral carbonates is given by the amount of glauconite, chlorite, and smectite present in the reservoir prior to injection, as they were nearly completely dissolved. The fast dissolution of the silicates provided divalent cations for the growth of ankerite and siderite. The timing of precipitation and the secondary mineral assemblage were seen to be highly sensitive to the nucleation and growth rates. Moreover, at high nucleation rates, the secondary carbonates started to precipitate at fairly low supersaturations and formed rapidly after the dissolution of the primary minerals.Finally, a comparison of earlier simulations on the Utsira-type system with the present model and natural analogues, suggests that the earlier models have largely overestimated the growth potential of carbonates such as dolomite, magnesite and dawsonite.

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Section: Thermodynamic Datamentioning

confidence: 99%

On the potential of CO2–water–rock interactions for CO2 storage using a modified kinetic model

Pham

Lü

Aagaard

et al. 2011

International Journal of Greenhouse Gas Control

137

112

View full text Add to dashboard Cite

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“…Siderite has also been identified in extraterrestrial materials such as meteorites (Johnson and Prinz, 1993;Romanek et al, 1994;Treiman and Romanek, 1998) and interplanetary dust particles (Keller et al, 1994). The geochemical and isotopic information stored in siderite provide valuable insights into the environmental conditions of mineral formation and the processes by which carbonate minerals are modified over time Mozley, 1989;Pye et al, 1990;Woods and Garrels, 1992;Ohmoto et al, 2004).…”

Section: The Formation Of Sideritementioning

confidence: 99%

Inorganic synthesis of Fe–Ca–Mg carbonates at low temperature

Romanek¹,

Jiménez-López²,

Navarro³

et al. 2009

Geochimica et Cosmochimica Acta

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“…For example, Fe 2+ , tends to bind to CO 2− 3 to form the ion pair FeCO 0 3 (aq) in solution, which suppresses the level of free CO 2− 3 available and prevents the precipitation of other carbonates prior to siderite. Carbonate solid-solution equilibria (Woods and Garrels, 1992) determine the cationic composition of carbonates. The degree of cation substitution depends on the concentration ratios of cations in solution, e.g.…”

Section: Evaporation Modelsmentioning

confidence: 99%

Alteration Assemblages in Martian Meteorites: Implications for Near-Surface Processes

Bridges

Catling

Saxton

et al. 2001

Space Sciences Series of ISSI

128

201

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Abstract. The SNC (Shergotty-Nakhla-Chassigny) meteorites have recorded interactions between martian crustal fluids and the parent igneous rocks. The resultant secondary minerals -which comprise up to ~ 1 vol.% of the meteorites -provide information about the timing and nature of hydrous activity and atmospheric processes on Mars. We suggest that the most plausible models for secondary mineral formation involve the evaporation of low temperature o C) brines. This is consistent with the simple mineralogy of these assemblages -Fe-Mg-Ca carbonates, anhydrite, gypsum, halite, clays -and the chemical fractionation of Ca-to Mg-rich carbonate in ALH84001 'rosettes'. Longer-lived, and higher temperature, hydrothermal systems would have caused more silicate alteration than is seen and probably more complex mineral assemblages. Experimental and phase equilibria data on carbonate compositions similar to those present in the SNCs imply low temperatures of formation with cooling taking place over a short period of time (e.g. days). The ALH84001 carbonate also probably shows the effects of partial vapourisation and dehydration related to an impact event postdating the initial precipitation. This shock event may have led to the formation of sulphide and some magnetite in the Fe-rich outer parts of the rosettes.Radiometric dating (K-Ar, Rb-Sr) of the secondary mineral assemblages in one of the nakhlites (Lafayette) suggests that they formed between 0 and 670 Ma, and certainly long after the crystallisation of the host igneous rocks. Crystallisation of ALH84001 carbonate took place 0.5 Ga after the parent rock. These age ranges and the other research on these assemblages suggest that environmental conditions conducive to near-surface liquid water have been present on Mars periodically over the last ~1 Ga. This fluid activity cannot have been continuous over geological time because in that case much more silicate alteration would have taken place in the meteorite parent rocks and the soluble salts would probably not have been preserved.The secondary minerals could have been precipitated from brines with seawater-like composition, high bicarbonate contents and a weakly acidic nature. The co-existence of siderite (Fe-carbonate) and clays in the nakhlites suggests that the pCO 2 level in equilibrium with the parent brine may have been 50 mbar or more. The brines could have originated as flood waters which percolated through the top few hundred metres of the crust, releasing cations from the surrounding parent rocks. There is no spectroscopic or photographic evidence for extensive evaporite deposits on the current martian surface but some salt precipitation through solute concentration must have occurred as floodwaters associated with many of the martian channels ponded in low-lying areas. The high sulphur and chlorine concentrations of the martian soil have most likely resulted from aeolian redistribution of such aqueously-deposited salts and from reaction of the martian surface with volcanic acid volatiles. However, the SNC salt a...

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Calculated aqueous-solution-solid-solution relations in the low-temperature system CaO-MgO-FeO-CO2-H2O

Cited by 27 publications

References 60 publications

On the potential of CO2–water–rock interactions for CO2 storage using a modified kinetic model

On the potential of CO2–water–rock interactions for CO2 storage using a modified kinetic model

Inorganic synthesis of Fe–Ca–Mg carbonates at low temperature

Alteration Assemblages in Martian Meteorites: Implications for Near-Surface Processes

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