CO2 solubility in Martian basalts and Martian atmospheric evolution

Stanley, B. D.; Hirschmann, M. M.; Withers, A. C.

doi:10.1016/j.gca.2011.07.027

Cited by 69 publications

(89 citation statements)

References 118 publications

(206 reference statements)

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“…This transition in dissolved carbon species occurs at much more reducing conditions in our basaltic composition than previously observed for a simplified silicate system (15). The observation that carbonate is dissolved in haplobasaltic melts and synthetic Martian basalts down to IW+1 (20,21) is consistent with the fO 2 range we observe (Fig. 4).…”

supporting

confidence: 91%

“…The oxidized glasses equilibrated at fO 2 > IW−0.55 follow a separate trend for carbon solubility: C (ppm) = 0.5605 * P (MPa) (r 2 = 0.9163). Previous work (21,29) indicates that carbonate solubility decreases significantly with decreasing fO 2 , but our results show that more carbon is dissolved at reduced conditions than is suggested by previous work. The two different carbon solubility-pressure trends appear to result from a difference in carbon speciation.…”

contrasting

confidence: 77%

“…Therefore, carbon speciation is a function of melt composition as well as fO 2 . This study reports evidence for CO, dissolved as Fe (CO) 5 , in basaltic glass, which results in higher carbon solubility for Fe-bearing planetary basalts under reduced conditions than previously reported CO (19) and CO 2 (21,29) solubilities.…”

mentioning

confidence: 40%

“…However, under more oxidizing conditions in basaltic melt compositions, carbon is dissolved as carbonate (17)(18)(19), and the transition in speciation from methane to carbonate has long been debated as either occurring at more reducing conditions than IW+1 (20,21) or at more oxidizing conditions (15). Another study (22) shows that a significant amount of C 4+ (carbonate) can be incorporated at extremely low fO 2 (IW−4.5) if Fe and alkalis are present in the melt.…”

mentioning

confidence: 99%

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Degassing of reduced carbon from planetary basalts

Wetzel

Rutherford

Jacobsen

et al. 2013

Proc. Natl. Acad. Sci. U.S.A.

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Degassing of planetary interiors through surface volcanism plays an important role in the evolution of planetary bodies and atmospheres. On Earth, carbon dioxide and water are the primary volatile species in magmas. However, little is known about the speciation and degassing of carbon in magmas formed on other planets (i.e., Moon, Mars, Mercury), where the mantle oxidation state [oxygen fugacity (fO 2 )] is different from that of the Earth. Using experiments on a lunar basalt composition, we confirm that carbon dissolves as carbonate at an fO 2 higher than -0.55 relative to the iron wustite oxygen buffer (IW-0.55), whereas at a lower fO 2 , we discover that carbon is present mainly as iron pentacarbonyl and in smaller amounts as methane in the melt. The transition of carbon speciation in mantle-derived melts at fO 2 less than IW-0.55 is associated with a decrease in carbon solubility by a factor of 2. Thus, the fO 2 controls carbon speciation and solubility in mantle-derived melts even more than previous data indicate, and the degassing of reduced carbon from Fe-rich basalts on planetary bodies would produce methane-bearing, CO-rich early atmospheres with a strong greenhouse potential.hydrogen | iron carbonyl | magmatic volatiles | experimental petrology M agmas formed through igneous processes on parent bodies in the early solar system span 12 log units in oxidation state, from 6.3 log units of oxygen fugacity (fO 2 ) below the iron wustite oxygen buffer (IW) to 6 log units above the IW (IW−6.3 to IW+6) (1-4). Over the wide range of basalt fO 2 observed in these planetary bodies, thermodynamic data for the C-O-H gas system indicate that there are significant changes in gas phase speciation (5). These differences should be reflected in how volatiles are dissolved in magmas, but carbon speciation experiments for basaltic systems are limited, particularly at low fO 2 . The developing evidence for volatiles in magmas erupted on the Moon (6, 7) as well as on Earth (3,8), Mars (9-12), and Mercury (13) is a strong incentive to improve our understanding of C-O-H speciation and solubility in planetary basaltic magmas.Previous experimental studies on the speciation of carbon in Fe-free silicate systems under reducing conditions or at fO 2 < IW show carbon is dissolved as methane (14-16). However, under more oxidizing conditions in basaltic melt compositions, carbon is dissolved as carbonate (17)(18)(19), and the transition in speciation from methane to carbonate has long been debated as either occurring at more reducing conditions than IW+1 (20, 21) or at more oxidizing conditions (15). Another study (22) shows that a significant amount of C 4+ (carbonate) can be incorporated at extremely low fO 2 (IW−4.5) if Fe and alkalis are present in the melt. Additional experiments on Fe-bearing basalt are clearly required to resolve the conflicts in existing data. The results are important in understanding the residence time of carbon in the mantle and the rate of carbon degassing during the early evolution of terrestrial planets ...

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supporting

confidence: 91%

contrasting

confidence: 77%

mentioning

confidence: 40%

mentioning

confidence: 99%

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Degassing of reduced carbon from planetary basalts

Wetzel

Rutherford

Jacobsen

et al. 2013

Proc. Natl. Acad. Sci. U.S.A.

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“…Crustal production modeling suggests that a total 0.5-1 bar of CO 2 have been outgassed, mostly during the Noachian (Grott et al 2011). Finally, modeling using CO 2 contents of martian magmas based on the martian meteorites also predicts between 0 and 1.2 bars of CO 2 outgassing in the past 4.5 Ga (Stanley et al 2011). Thus, up to ∼1.2 bar of magmatic CO 2 has been released to the atmosphere throughout martian history.…”

Section: Co 2 Budget Of Marsmentioning

confidence: 84%

Geochemistry of Carbonates on Mars: Implications for Climate History and Nature of Aqueous Environments

Niles¹,

Catling²,

Berger³

et al. 2012

Quantifying the Martian Geochemical Reservoirs

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Ongoing research on martian meteorites and a new set of observations of carbonate minerals provided by an unprecedented series of robotic missions to Mars in the past 15 years help define new constraints on the history of martian climate with important cross- cutting themes including: the CO 2 budget of Mars, the role of Mg-, Fe-rich fluids on Mars, and the interplay between carbonate formation and acidity.Carbonate minerals have now been identified in a wide range of localities on Mars as well as in several martian meteorites. The martian meteorites contain carbonates in low abundances (<1 vol.%) and with a wide range of chemistries. Carbonates have also been identified by remote sensing instruments on orbiting spacecraft in several surface locations as well as in low concentrations (2-5 wt.%) in the martian dust. The Spirit rover also identified an outcrop with 16 to 34 wt.% carbonate material in the Columbia Hills of Gusev Crater that strongly resembled the composition of carbonate found in martian meteorite ALH 84001. Finally, the Phoenix lander identified concentrations of 3-6 wt.% carbonate in the soils of the northern plains.The carbonates discovered to date do not clearly indicate the past presence of a dense Noachian atmosphere, but instead suggest localized hydrothermal aqueous environments with limited water availability that existed primarily in the early to mid-Noachian followed by low levels of carbonate formation from thin films of transient water from the late Noachian to the present. The prevalence of carbonate along with evidence for active carbonate precipitation suggests that a global acidic chemistry is unlikely and a more complex relationship between acidity and carbonate formation is present.

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The eruptibility of magmas at Tharsis and Syrtis Major on Mars

Black

Manga

2016

JGR Planets

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Magnetic and geologic data indicate that the ratio of intrusive to extrusive magmatism (the I/E ratio) is higher in the Tharsis and Syrtis Major volcanic provinces on Mars relative to most volcanic centers on Earth. The fraction of magmas that erupt helps to determine the effects of magmatism on crustal structure and the flux of magmatic gases to the atmosphere and also influences estimates of melt production inferred from the history of surface volcanism. We consider several possible controls on the prevalence of intrusive magmatism at Tharsis and Syrtis Major, including melt production rates, lithospheric properties, regional stresses and strain rates, and magmatic volatile budgets. The Curie temperature is the minimum crustal temperature required for thermal demagnetization, implying that if the primary magnetic mineral is magnetite or hematite, the crust was warm during the intrusive magmatism reflected in Tharsis and Syrtis Major I/E ratios. When wall rocks are warm, thermally activated creep relaxes stresses from magma replenishment and regional tectonics, and eruptibility depends on buoyancy overpressure. We develop a new one‐dimensional model for the development of buoyancy in a viscous regime that accounts for cooling, crystallization, volatile exsolution, bubble coalescence and rise, fluid egress, and compaction of country rock. Under these conditions, we find that initial water and CO2 contents typically <1.5 wt % can explain the observed range of intrusive/extrusive ratios. Our results support the hypothesis that warm crust and a relatively sparse volatile budget encouraged the development of large intrusive complexes beneath Tharsis and Syrtis Major.

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CO2 solubility in Martian basalts and Martian atmospheric evolution

Cited by 69 publications

References 118 publications

Degassing of reduced carbon from planetary basalts

Degassing of reduced carbon from planetary basalts

Geochemistry of Carbonates on Mars: Implications for Climate History and Nature of Aqueous Environments

The eruptibility of magmas at Tharsis and Syrtis Major on Mars

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