Origin of water and mantle–crust interactions on Mars inferred from hydrogen isotopes and volatile element abundances of olivine-hosted melt inclusions of primitive shergottites

Usui, Tomohiro; Alexander, Conel M. O'd.; Wang, Jingyuan; Simon, Justin I.; Jones, J. H.

doi:10.1016/j.epsl.2012.09.008

Cited by 161 publications

(221 citation statements)

References 62 publications

Supporting

Mentioning

202

Contrasting

Order By: Relevance

“…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%

“…Using early Mars as an example, we can estimate the atmospheric pressure of carbon species produced from the formation of an ancient (4.5 Ga) basaltic crust and compare this with previous calculations (29). Assuming a 50 km-thick (1.9 × 10 22 kg) crust initially melted at a depth of 1.2 GPa, a carbonsaturated oxidized melt (fO 2 > IW−0.55) would contain 665 ppm of dissolved C. If the Martian mantle was initially reduced at fO 2 < IW−0.55, the carbon concentration in the melt would be 293 ppm of C [70-400 ppm of C has been measured in Martian meteorite melt inclusions (10)]. Assuming an oxidized mantle will degas carbon as CO 2 , the formation of the crust will produce experiments (same color scheme as in Fig.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Degassing of reduced carbon from planetary basalts

Wetzel

Rutherford

Jacobsen

et al. 2013

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

View full text Add to dashboard Cite

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 ...

show abstract

mentioning

confidence: 99%

mentioning

confidence: 99%

Degassing of reduced carbon from planetary basalts

Wetzel

Rutherford

Jacobsen

et al. 2013

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

View full text Add to dashboard Cite

show abstract

“…The waterpoor, low-δD reservoir is likely derived from the igneous mineralogy of the rock (Chen et al 2015), which inherited an isotopic signature that reflects the martian mantle. While estimates for the martian mantle vary (e.g., Usui et al, 2012Usui et al, , 2015McCubbin et al 2016), Filiberto et al (2016) provide arguments for adopting δD = -100 ‰ and ≤ 200 ppm H 2 O for martian mantle sources. Our regression line yields 146 ppm H 2 O assuming δD = -100 ‰ (Fig.…”

Section: The Volatile Inventory Of Tissint Shock-produced Glassmentioning

confidence: 99%

Martian low-temperature alteration materials in shock-melt pockets in Tissint: Constraints on their preservation in shergottite meteorites

Kuchka

Herd

Walton

et al. 2017

Geochimica et Cosmochimica Acta

View full text Add to dashboard Cite

We apply an array of in situ analytical techniques, including electron and Raman microscopy, electron and ion probe microanalysis, and laser ablation mass spectrometry to the Tissint martian meteorite in order to find and elucidate a geochemical signature characteristic of low-temperature alteration at or near the martian surface. Tissint contains abundant shock-produced quench-crystallized melt pockets containing water in concentrations ranging from 73 to 1730 ppm; water content is positively correlated with Cl content. The isotopic composition of hydrogen in the shock-produced glass ranges from δD = 2559 to 4422 ‰. Water is derived from two distinct hydrogen reservoirs: the martian nearsurface (>500 ‰) and the martian mantle (-100 ‰). In one shock melt pocket comprising texturally homogeneous vesiculated glass, the concentration of H in the shock melt decreases while simultaneously becoming enriched in D, attributable to the preferential loss of H over D to the vesicle while the pocket was still molten. While igneous sulfides are pyrrhotite in composition (Fe 0.88-0.90 S), the iron to sulfur ratios of spherules in shock melt pockets are elevated, up to Fe 1.70 S, which we attribute to shock-oxidation of igneous pyrrhotite and the formation of hematite at high temperature. The D-and Cl-enrichment, and higher oxidation of the pockets (as indicated by hematite) support a scenario in which alteration products formed within fractures or void spaces within the rock; the signature of these alteration products is preserved within shock melt (now glass) which formed upon collapse of these fractures and voids during impact shock. Thermal modeling of Tissint shock melt pockets using the HEAT program demonstrates that the shock melt pockets with the greatest potential to preserve a signature of aqueous alteration are small, isolated from other regions of shock melt, vesicle-free, and glassy.3

show abstract

“…Water content can constrain the extent of oxidation [47] that may possibly affect the oxygen isotope compositions of the mantle minerals through isotopic exchange. Martian meteorites have shown the presence of water within Mars' interior [48][49][50][51][52][53][54][55]. However, Martian magmas may have suffered a partial loss of the volatiles by degassing upon eruption [56].…”

Section: Introductionmentioning

confidence: 99%

“…However, Martian magmas may have suffered a partial loss of the volatiles by degassing upon eruption [56]. To counter this uncertainty, several studies have been carried out to estimate the pre-eruptive water contents of Martian magmas on the basis of H-isotopes [53,54,57]. Furthermore, an experimental study [58] has suggested that at least 2 wt.…”

Section: Introductionmentioning

confidence: 99%

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

et al. 2018

View full text Add to dashboard Cite

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.

show abstract

Origin of water and mantle–crust interactions on Mars inferred from hydrogen isotopes and volatile element abundances of olivine-hosted melt inclusions of primitive shergottites

Cited by 161 publications

References 62 publications

Degassing of reduced carbon from planetary basalts

Degassing of reduced carbon from planetary basalts

Martian low-temperature alteration materials in shock-melt pockets in Tissint: Constraints on their preservation in shergottite meteorites

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

Contact Info

Product

Resources

About