Solubility of COH volatiles in graphite-saturated martian basalts

Stanley, B. D.; Hirschmann, M. M.

doi:10.1016/j.gca.2013.12.013

Cited by 62 publications

(94 citation statements)

References 88 publications

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“…Although values for both elements vary with experimental conditions and compositions, C partitions more strongly into metal than does N. Characteristic mass partition coefficients for C (D met=sil C ) are 10 2 -10 4 (8, 10, 45-47), compared with those for N (D met=sil N ) of ∼20 (9). The solubilities of C and N depend strongly on oxygen fugacity, with C more soluble than N in silicate melt under oxidizing conditions and the opposite under highly reducing conditions (41,46,47).…”

Section: C/n-forming Terrestrial Worldsmentioning

confidence: 99%

Tracing the ingredients for a habitable earth from interstellar space through planet formation

Bergin

Blake

Ciesla

et al. 2015

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

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176

175

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We use the C/N ratio as a monitor of the delivery of key ingredients of life to nascent terrestrial worlds. Total elemental C and N contents, and their ratio, are examined for the interstellar medium, comets, chondritic meteorites, and terrestrial planets; we include an updated estimate for the bulk silicate Earth (C/N = 49.0 ± 9.3). Using a kinetic model of disk chemistry, and the sublimation/condensation temperatures of primitive molecules, we suggest that organic ices and macromolecular (refractory or carbonaceous dust) organic material are the likely initial C and N carriers. Chemical reactions in the disk can produce nebular C/N ratios of ∼1-12, comparable to those of comets and the low end estimated for planetesimals. An increase of the C/N ratio is traced between volatile-rich pristine bodies and larger volatile-depleted objects subjected to thermal/accretional metamorphism. The C/N ratios of the dominant materials accreted to terrestrial planets should therefore be higher than those seen in carbonaceous chondrites or comets. During planetary formation, we explore scenarios leading to further volatile loss and associated C/N variations owing to core formation and atmospheric escape. Key processes include relative enrichment of nitrogen in the atmosphere and preferential sequestration of carbon by the core. The high C/N bulk silicate Earth ratio therefore is best satisfied by accretion of thermally processed objects followed by large-scale atmospheric loss. These two effects must be more profound if volatile sequestration in the core is effective. The stochastic nature of these processes hints that the surface/atmospheric abundances of biosphereessential materials will likely be variable.terrestrial worlds | elements | interstellar medium | comets | meteorites T he development of a habitable world and a stable biosphere requires the delivery of biogenic elements of which carbon and nitrogen are crucial. Carbon is the backbone for the chemistry of life and, in the form of CO 2 , combines with water to provide the greenhouse needed for a habitable Earth. Nitrogen is a key component of DNA, RNA, and proteins, while also present as the dominant constituent of our atmosphere. The processes that supply these crucial ingredients remain poorly understood. In interstellar space, C and N are abundant, but inherently volatile and so chiefly remain in the gas. Thus, the terrestrial planets, which accrete primarily from rocks and ices, are fed from C-and N-depleted materials and are carbon and nitrogen poor compared with the nebular disk from which they descend (1, 2). The carbon and nitrogen depletion of rocky bodies is a general phenomenon, observable not just in our solar system, but also in the polluted atmospheres of white dwarf stars, which trace the composition of disrupted planetesimals (3, 4). This volatile poor state of terrestrial planets is partially imparted from the starting materials. However, further differential loss of C and N can occur due to parent body processes such as thermal metamorphism, core s...

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Section: C/n-forming Terrestrial Worldsmentioning

confidence: 99%

Tracing the ingredients for a habitable earth from interstellar space through planet formation

Bergin

Blake

Ciesla

et al. 2015

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

Self Cite

176

175

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“…However, so far there are only a few studies that exclusively constrained the D metal/silicate C relevant for MO (Dasgupta and Walker, 2008;Zhang and Yin, 2012;Dasgupta et al, 2013a;Chi et al, 2014). Only Dasgupta et al (2013a), Stanley et al (2014), and Chi et al (2014) experimentally measured D metal/silicate C (100-5000) as a function of temperature (1350-2100 • C), pressure (1-5 GPa), oxygen fugacity (∼IW-0.4 to IW-1), silicate melt composition (NBO/T = 0.8-3.6), and alloy melt composition (Fe/Ni ratio).…”

Section: Introductionmentioning

confidence: 99%

“…However, all of these studies constructed alloy melt compositions that either had carbon as the only light element (Dasgupta et al, 2013a;Stanley et al, 2014;Chi et al, 2014) or had only a minor presence of sulfur (Dasgupta et al, 2013a). Further, these experiments did not extend to very reducing conditions (<IW-1.5) that may be relevant for early accretion of terrestrial planets such as Earth (e.g., Wood et al, 2006).…”

Section: Introductionmentioning

confidence: 99%

“…Understanding the dissolution mechanism of carbon in silicate melt is also of great importance in understanding carbon solubility in silicate melt and thus magma's storage and transport capacities of carbon (Holloway et al, 1992;Kadik et al, 2004;Mysen et al, 2011;Stanley et al, 2011Stanley et al, , 2014Ardia et al, 2013;Dasgupta et al, 2013a;Chi et al, 2014). The species of C-H-O volatiles in reduced silicate melt, which are mainly a multifunction of fugacities of H 2 O, H 2 , and O 2 , remain unclear, resulting in the carbon species degassed from reduced, solid planetary mantles such as those in Mars and the Moon remaining unclear and debated (Dasgupta, 2013;Wetzel et al, 2013;Stanley et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

“…The species of C-H-O volatiles in reduced silicate melt, which are mainly a multifunction of fugacities of H 2 O, H 2 , and O 2 , remain unclear, resulting in the carbon species degassed from reduced, solid planetary mantles such as those in Mars and the Moon remaining unclear and debated (Dasgupta, 2013;Wetzel et al, 2013;Stanley et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

Dasgupta

Tsuno

2015

Earth and Planetary Science Letters

104

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The origin of volatiles in the Earth's mantle

Hier‐Majumder

Hirschmann

2017

Geochem Geophys Geosyst

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The Earth's deep interior contains significant reservoirs of volatiles such as H, C, and N. Due to the incompatible nature of these volatile species, it has been difficult to reconcile their storage in the residual mantle immediately following crystallization of the terrestrial magma ocean (MO). As the magma ocean freezes, it is commonly assumed that very small amounts of melt are retained in the residual mantle, limiting the trapped volatile concentration in the primordial mantle. In this article, we show that inefficient melt drainage out of the freezing front can retain large amounts of volatiles hosted in the trapped melt in the residual mantle while creating a thick early atmosphere. Using a two‐phase flow model, we demonstrate that compaction within the moving freezing front is inefficient over time scales characteristic of magma ocean solidification. We employ a scaling relation between the trapped melt fraction, the rate of compaction, and the rate of freezing in our magma ocean evolution model. For cosmochemically plausible fractions of volatiles delivered during the later stages of accretion, our calculations suggest that up to 77% of total H2O and 12% of CO2 could have been trapped in the mantle during magma ocean crystallization. The assumption of a constant trapped melt fraction underestimates the mass of volatiles in the residual mantle by more than an order of magnitude.

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Solubility of COH volatiles in graphite-saturated martian basalts

Cited by 62 publications

References 88 publications

Tracing the ingredients for a habitable earth from interstellar space through planet formation

Tracing the ingredients for a habitable earth from interstellar space through planet formation

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

The origin of volatiles in the Earth's mantle

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