The effects of sulfur, silicon, water, and oxygen fugacity on carbon solubility and partitioning in Fe-rich alloy and silicate melt systems at 3 GPa and 1600 °C: Implications for core–mantle differentiation and degassing of magma oceans and reduced planetary mantles

Li, Yuan; Dasgupta, Rajdeep; Tsuno, K.

doi:10.1016/j.epsl.2015.01.017

Cited by 72 publications

(120 citation statements)

References 89 publications

(170 reference statements)

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“…Compositions of the quenched silicate and metallic melts from our five diamond anvil cell experiments and our 15 multianvil press experiments are reported in (Chi et al, 2014;Dasgupta et al, 2013;Li et al, 2015), so its absence in the silicate indicates that the carbon was in the system during the high P-T experiments and was not introduced as a contaminant during analyses. The light element content of the metal increases with increasing temperature and pressure, reaching 11.3 wt% O, 8.8 wt% Si, and 0.9 wt% C at 100 GPa and 5700 K (Table A.2).…”

Section: Resultsmentioning

confidence: 95%

High pressure metal–silicate partitioning of Ni, Co, V, Cr, Si, and O

Fischer

Nakajima

Campbell

et al. 2015

Geochimica et Cosmochimica Acta

199

263

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High pressure metal-silicate partitioning of Ni, Co, V, Cr, Si, and O, Geochimica et Cosmochimica Acta (2015), doi: http://dx.High pressure metal-silicate partitioning of Ni, Co, V, Cr, Si, and O AbstractThe distributions of major and minor elements in Earth's core and mantle were primarily established by high pressure, high temperature metal-silicate partitioning during core segregation. The partitioning behaviors of moderately siderophile elements can be used to constrain the pressure-temperature conditions of core formation and the 2 core's composition. We performed experiments to study the partitioning of Ni, Co, V, Cr, Si, and O between silicate melt and Fe-rich metallic melt in a multianvil press and diamond anvil cell, up to 100 GPa and 5700 K. Combining our new results with data from 18 previous studies, we parameterized the effects of pressure, temperature, and metallic melt composition on partitioning. Ni and Co partitioning are insensitive to composition. At low pressures, these elements become less siderophile with increasing temperature, with this trend reversing above ~45 GPa. V and Cr partitioning are much more sensitive to metallic melt composition and less sensitive to pressure. Partitioning of Si and O are insensitive to pressure, but with strong and moderate temperature dependences, respectively. Our new parameterizations of Ni and Co partitioning suggest that the Earth's distributions of these elements can be matched by single-stage coremantle equilibration at 54 ± 5 GPa and 3300-3400 K. These conditions would result in 8.5 ± 1.4 wt% Si and 1.6 ± 0.3 wt% O in the core, compatible with the core's measured density. However, this single-stage model matches the Earth's V and Cr distributions less well. We also incorporated our parameterizations into models of multi-stage core formation over evolving pressure-temperature-oxygen fugacity conditions, reproducing the Earth's Ni and Co distributions while simultaneously producing a core whose light element composition is consistent with its density.

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Section: Resultsmentioning

confidence: 95%

High pressure metal–silicate partitioning of Ni, Co, V, Cr, Si, and O

Fischer

Nakajima

Campbell

et al. 2015

Geochimica et Cosmochimica Acta

199

263

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“…After each 3–5 analytical spots on the sample glass, one or two analyses were performed on the standard glass (ALV 519‐4‐1) for checking the possible deviation and accuracy during the analysis. Similar to the study of Li et al [], during the analytical session, no considerable deviation was observed and the calculated CO 2 content (166 ± 5 ppm) of the standard glass (ALV519‐4‐1) was in good agreement with its nominal value (165 ppm).…”

Section: Methodsmentioning

confidence: 99%

“…The solubility and speciation of carbon in silicate melt, which are mainly controlled by pressure, temperature, melt composition, and fugacities of H 2 O, H 2 , and O 2 , have been studied extensively at conditions corresponding to the Earth's present mantle and crust [e.g., Duncan and Dasgupta , ; Holloway et al , ; Mysen et al , ; Ni and Keppler , ]. However, both the solubility and speciation of carbon in reduced mafic silicate melt, which are more relevant for the reduced silicate mantles of Mars, Mercury, and the Moon, are poorly constrained and are topics of active investigation and debate [ Armstrong et al , ; Chi et al , ; Dasgupta et al , ; Kadik et al , ; Li et al , ; Stanley et al , ; Stanley et al , ; Wetzel et al , ; Yoshioka et al , ; Li et al , ]. At the Earth's present upper mantle conditions, carbon in mafic silicate melts is dissolved mainly as carbonates [ Duncan and Dasgupta , ; Holloway et al , ; Mysen et al , ; Ni and Keppler , ].…”

Section: Introductionmentioning

confidence: 99%

“…In this study, in order to further constrain the carbon speciation and solubility in reduced planetary mantle melts, we first present new experimental results on carbon solubility and speciation in Martian basalts at relevant P ‐ T ‐ f O 2 conditions. Then, combing with recent data sets of carbon solubility in reduced, different mafic melts [ Armstrong et al , ; Chi et al , ; Dasgupta et al , ; Li et al , ; Stanley et al , ; Wetzel et al , ; Li et al , ; Duncan and Dasgupta , ], we develop an empirical model that can be used to predict carbon solubility in mantle melts of Mars, Mercury, and the Moon.…”

Section: Introductionmentioning

confidence: 99%

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Carbon contents in reduced basalts at graphite saturation: Implications for the degassing of Mars, Mercury, and the Moon

Dasgupta

Tsuno

2017

JGR Planets

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Carbon contents in reduced Martian basalts at graphite saturation were experimentally studied at 1400–1550°C, 1–2 GPa, and logfO2 of IW − 0.4 to IW + 1.5 (IW denotes the Fe‐FeO buffer). The results show that carbon solubility in Martian basalts, determined by secondary ion mass spectrometry, is 20 to 1400 ppm, increasing with increasing fO2. Raman and Fourier transform infrared spectroscopic measurements on the quenched silicate glasses show that the dominant carbon species in Martian basalts is carbonate (CO32−). The experimental data generated here were combined with literature data on similar graphite‐saturated carbon solubility for mafic‐ultramafic compositions to develop an empirical model that can be used to predict carbon content of graphite‐saturated reduced basalts at vapor‐absent conditions: leftAtIW+1.7≥logfnormalO2≥IW−1:logCppm=−3702±534/T−194±49P/T−0.0034±0.043logXH2O+0.61±0.07NBO/T+0.55±0.02ΔIW+3.5±0.3R2=0.89 leftAtIW−5.3≤logfnormalO2≤IW−1:logCppm=0.96±0.19logXH2O−0.25±0.04ΔIW+2.83±0.34R2=0.6 in which T is temperature in K, P is pressure in GPa, XH2O is mole fraction of water in basalts, ΔIW is the oxygen fugacity relative to the IW buffer, and NBO/T = 2 total O/T − 4 (T = Si + Ti + Al + Cr + P). This model was applied to predict carbon content in graphite‐saturated mantle melts of the Mercury, Mars, and the Moon. The results show that graphite may be consumed during the production and extraction of some Martian basalts, and CO2 released by volcanism on Mars cannot be an efficient greenhouse gas in the early Mars. The lunar mantle carbon may be one of the main propellant driving the fire‐fountain eruption on the Moon; however, the Mercurian mantle carbon may not be an important propellant for the explosive eruption on Mercury.

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“…Although compositional variability was observed in some experiments, a single, homogeneous, metallic melt is observed in most experiments. The sulfur content of the metal melt is low and decreases continuously with f O 2 from ∼2.2 wt.% at IW-3.5 to 0 wt.% at IW-9, leading ing a lower concentration of dissolved carbon (Li et al, 2015). The sulfide phase observed in the majority of our experiments is dominated by Fe (54-69 wt.%) and S (27-39 wt.%), with minor Ti (0.0-4.5 wt.%), Mn (0.0-2.3 wt.%), Mg (0.0-4.1 wt.%), Ca (0.0-2.8 wt.%), Cr (0.1-3.2 wt.%) and Ni (0.0-3.0 wt.%), and has a Fe/S ratio close to 1 (Fe 0.91 S 1.09 to Fe 1.13 S 0.87 ; average Fe 1.0 S 1.0 ).…”

Section: Major Element Compositions Of the Experiments And Sulfur Conmentioning

confidence: 99%

Sulfur solubility in reduced mafic silicate melts: Implications for the speciation and distribution of sulfur on Mercury

Namur

Charlier

Holtz

et al. 2016

Earth and Planetary Science Letters

107

160

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Chemical data from the MESSENGER spacecraft revealed that surface rocks on Mercury are unusually enriched in sulfur compared to samples from other terrestrial planets. In order to understand the speciation and distribution of sulfur on Mercury, we performed high temperature (1200-1750 • C), lowto high-pressure (1 bar to 4 GPa) experiments on compositions representative of Mercurian lavas and on the silicate composition of an enstatite chondrite. We equilibrated silicate melts with sulfide and metallic melts under highly reducing conditions (IW-1.5 to IW-9.4; IW = iron-wüstite oxygen fugacity buffer). Under these oxygen fugacity conditions, sulfur dissolves in the silicate melt as S 2− and forms complexes with Fe 2+ , Mg 2+ and Ca 2+ . The sulfur concentration in silicate melts at sulfide saturation (SCSS) increases with increasing reducing conditions (from <1 wt.% S at IW-2 to >10 wt.% S at IW-8) and with increasing temperature. Metallic melts have a low sulfur content which decreases from 3 wt.% at IW-2 to 0 wt.% at IW-9. We developed an empirical parameterization to predict SCSS in Mercurian magmas as a function of oxygen fugacity ( f O 2 ), temperature, pressure and silicate melt composition. SCSS being not strictly a redox reaction, our expression is fully valid for magmatic systems containing a metal phase. Using physical constraints of the Mercurian mantle and magmas as well as our experimental results, we suggest that basalts on Mercury were free of sulfide globules when they erupted. The high sulfur contents revealed by MESSENGER result from the high sulfur solubility in silicate melt at reducing conditions. We make the realistic assumption that the oxygen fugacity of mantle rocks was set during equilibration of the magma ocean with the core and/or that the mantle contains a minor metal phase and combine our parameterization of SCSS with chemical data from MESSENGER to constrain the oxygen fugacity of Mercury's interior to IW-5.4 ± 0.4. We also calculate that the mantle of Mercury contains 7-11 wt.% S and that the metallic core of the planet has little sulfur (<1.5 wt.% S). The external part of the Mercurian core is likely to be made up of a thin (<90 km) FeS layer.

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The effects of sulfur, silicon, water, and oxygen fugacity on carbon solubility and partitioning in Fe-rich alloy and silicate melt systems at 3 GPa and 1600 °C: Implications for core–mantle differentiation and degassing of magma oceans and reduced planetary mantles

Cited by 72 publications

References 89 publications

High pressure metal–silicate partitioning of Ni, Co, V, Cr, Si, and O

High pressure metal–silicate partitioning of Ni, Co, V, Cr, Si, and O

Carbon contents in reduced basalts at graphite saturation: Implications for the degassing of Mars, Mercury, and the Moon

Sulfur solubility in reduced mafic silicate melts: Implications for the speciation and distribution of sulfur on Mercury

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