A Reduced Organic Carbon Component in Martian Basalts

Steele, A.; McCubbin, F. M.; Fries, M.; Kater, L.; Boctor, N. Z.; Fogel, Marilyn L.; Conrad, Pamela G.; Glamoclija, M.; Spencer, Maegan K.; Morrow, Amy L.; Hammond, Michelle; Zare, Richard N.; Vicenzi, Edward P.; Siljeström, Sandra; Bowden, R.; Herd, Christopher D. K.; Mysen, Bjørn O.; Shirey, S. B.; Amundsen, H. E. F.; Treiman, Allan H.; Bullock, E. S.; Jull, A. J. T.

doi:10.1126/science.1220715

Cited by 188 publications

(220 citation statements)

References 66 publications

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“…Melt trapping in the olivine of DaG 476 has been reported at ~1275 °C followed by ascent and cooling that assisted crystallization of abiotic macromolecular carbon, spinel, and pyroxene in the melt inclusions of DaG 476 [82]. Our temperature estimation (~1200 °C) using pyroxene-olivine oxygen isotope thermometer for DaG 476 show a close resemblance.…”

Section: Petrogenetic Relationshipsupporting

confidence: 59%

“…The mantle melting zone shows temperature stratification (i.e., increase with increasing depth) that range from ~1400 °C to ~1700 °C [82]. Melt trapping in the olivine of DaG 476 has been reported at ~1275 °C followed by ascent and cooling that assisted crystallization of abiotic macromolecular carbon, spinel, and pyroxene in the melt inclusions of DaG 476 [82].…”

Section: Petrogenetic Relationshipmentioning

confidence: 99%

“…We calculated the f Di and f Fo values at temperatures between 600 • C and 1700 • C with a stepwise increment of 100 degrees. We selected higher temperatures for our calculations given the fact that oxygen isotope fractionation between these minerals have been studied experimentally at 600-1300 • C [81], and extrapolated to the typical temperature range of mantle melting zone (i.e.,~1400-1700 • C; [82]). The squared and cubed terms in the expressions (Equations (1) and (2)) are found to be negligibly low and has been ignored to get a simplified expression (Equation (3)).…”

Section: Oxygen Isotope Thermometrymentioning

confidence: 99%

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Oxygen Isotope Thermometry of DaG 476 and SaU 008 Martian Meteorites: Implications for Their Origin

et al. 2018

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Abstract:We report the equilibration temperatures derived from the oxygen isotope thermometry of pyroxene-olivine pair from the Dar al Ghani (DaG) 476 (1200 +105/−90 • C) and Sayh al Uhaymir (SaU) 008 (1430 +220/−155 • C) meteorites showing a difference of over 200 • C at the face values. Regardless of the large associated uncertainties, contrasting geochemical and isotopic characteristics such as oxygen fugacities, hydrogen isotopic compositions (referred to as the D/H ratios), olivine abundances, presence of merrillite and/or apatite, and their chlorine contents between the two meteorites are observed in the literature. These opposing features lend support to the idea that the relative difference observed in the estimated temperatures is probably real and significant, thus providing insights into the Martian mantle magmatism. Based on our temperature estimation and previous magmatic models, we propose that SaU 008 could have been originated from a deeper depleted mantle source. However, DaG 476 may have been produced by the partial melting of the entrained pockets of the depleted mantle similar to that of the SaU 008's source at a relatively shallower depth. Both meteorites erupted as a relatively thick lava flow or a shallow intrusion at approximately the same time followed by a launch initiated by a single meteoritic impact 1.1 million years (Ma) ago.

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Section: Petrogenetic Relationshipsupporting

confidence: 59%

Section: Petrogenetic Relationshipmentioning

confidence: 99%

Section: Oxygen Isotope Thermometrymentioning

confidence: 99%

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Oxygen Isotope Thermometry of DaG 476 and SaU 008 Martian Meteorites: Implications for Their Origin

et al. 2018

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“…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)(10)(11)(12), and Mercury (13) is a strong incentive to improve our understanding of C-O-H speciation and solubility in planetary basaltic magmas.…”

mentioning

confidence: 99%

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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“…The simplest conclusion is that the Earth's upper mantle was significantly more reduced in the beginning. Growing evidence indicates that magmatic carbon on Mars (17,18) and the Moon (19) has a carbon isotopic Bell et al describe two sizable graphite inclusions within a 4.1 billion-y-old zircon from the Jack Hills.…”

mentioning

confidence: 99%

Penciling in details of the Hadean

House¹

2015

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

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A Reduced Organic Carbon Component in Martian Basalts

Cited by 188 publications

References 66 publications

Oxygen Isotope Thermometry of DaG 476 and SaU 008 Martian Meteorites: Implications for Their Origin

Oxygen Isotope Thermometry of DaG 476 and SaU 008 Martian Meteorites: Implications for Their Origin

Degassing of reduced carbon from planetary basalts

Penciling in details of the Hadean

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