Partitioning of carbon between Fe-rich alloy melt and silicate melt in a magma ocean – Implications for the abundance and origin of volatiles in Earth, Mars, and the Moon

Chi, H.; Dasgupta, Rajdeep; Duncan, M. S.; Shimizu, Nobumichi

doi:10.1016/j.gca.2014.04.046

Cited by 102 publications

(158 citation statements)

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“…The organics can derive in part from the dense ISM before stellar birth, but also can be created inside the gas-rich disk. Based on models and observations, disk chemistry and transport can imprint variable C/N ratios (1)(2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12) in ices comparable to those of comets and primitive meteorites. During the stages of planetesimal formation when bodies grow to large sizes (greater than tens of kilometers), impact processing and thermal metamorphism can lead to greater disparity in the C/N content of preplanetary material (Fig.…”

Section: Discussionmentioning

confidence: 99%

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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.

182

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: Discussionmentioning

confidence: 99%

“…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 segregation, planetary outgassing, and atmospheric loss (5)(6)(7)(8)(9)(10)(11).…”

mentioning

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.

182

175

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“…Such conditions are currently thought to be near the base of a deep magma ocean (e.g., Righter 2011;Wood 2008), near 3500-4000 K and 40-50 GPa, but our current experimental database extends only to near 3 GPa and <2000 C (Chi et al 2014;Dasgupta et al 2013). Second, there is some data at low P, but essentially no data > 7 GPa (Okuchi 1997) for H partitioning between metallic liquid and silicate melt; this is primarily due to the technical challenges offered by these chemical systems.…”

Section: Introductionmentioning

confidence: 94%

“…1 C, H 2 O, N, and S concentrations in the bulk silicate Earth, from Marty(2012)andPalme and O'Neill (2014). Calculated values are based on work ofChi et al (2014) andDasgupta et al (2013) for carbon,Kuramoto and Matsui (1996) for H 2 O,Roskosz et al (2013) for nitrogen, andBoujibar et al (2014) for sulfur. Bulk Earth values are from Marty…”

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confidence: 99%

Magma Ocean Depth and Oxygen Fugacity in the Early Earth—Implications for Biochemistry

Righter

2015

Orig Life Evol Biosph

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A large class of elements, referred to as the siderophile (iron-loving) elements, in the Earth's mantle can be explained by an early deep magma ocean on the early Earth in which the mantle equilibrated with metallic liquid (core liquid). This stage would have affected the distribution of some of the classic volatile elements that are also essential ingredients for life and biochemistry - H, C, S, and N. Estimates are made of the H, C, S, and N contents of Earth's early mantle after core formation, considering the effects of variable temperature, pressure, oxygen fugacity, and composition on their partitioning. Assessment is made of whether additional, exogenous, sources are required to explain the observed mantle concentrations, and areas are identified where additional data and experimentation would lead to an improved understanding of this phase of Earth's history.

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“…The mantle is thought to contain the Earth's largest carbon reservoir, whereas the total estimated carbon concentration of the Earth's core is still being debated (e.g., Chi et al 2014;Dasgupta et al 2013;Sleep and Zahnle 2001;McDonough 2003). The solubility of carbon in olivine and other major silicate-mantle minerals is extremely low (Shcheka et al 2006), and this implies that the carbon must occur in the form of carbonates, graphite, diamond, or in C-H-O fluids, etc.…”

Section: Introductionmentioning

confidence: 99%

Sintering polycrystalline olivine and polycrystalline clinopyroxene containing trace amount of graphite from natural crystals

Tsubokawa

Ishikawa

2017

Earth Planets Space

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Graphite-bearing polycrystalline olivine and polycrystalline clinopyroxene with submicron to micron grain size were successfully sintered from a single crystal of naturally occurring olivine ). The milled powders of both these crystals were sintered under argon gas flow at temperatures ranging from 1130 to 1350 °C for 2 h. As the sintering temperature increased, the average grain size of olivine increased from 0.2 to 1.4 µm and that of clinopyroxene increased from 0.1 to 2.4 µm. The porosity of sintered samples remained at an almost-constant volume of 2-5% for olivine and 3-4% for clinopyroxene. The samples sintered from powders milled with ethanol exhibited trace amount of graphite, identified via Raman spectroscopy analysis. As the sintering temperature increased, the intensity of the graphite Raman peak decreased, compared with both olivine and clinopyroxene peaks. The carbon content of the sintered samples was estimated to be a few hundred ppm. The in-plane size (L a ) of graphite in the sintered olivine was estimated to be <15 nm. Our experiments demonstrate new possibilities for preparing graphite-bearing silicatemantle mineral rocks, and this method might be useful in understanding the influence of the physical properties of graphite on grain-size-sensitive rheology or the seismic velocity of the Earth's mantle.

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Partitioning of carbon between Fe-rich alloy melt and silicate melt in a magma ocean – Implications for the abundance and origin of volatiles in Earth, Mars, and the Moon

Cited by 102 publications

References 103 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

Magma Ocean Depth and Oxygen Fugacity in the Early Earth—Implications for Biochemistry

Sintering polycrystalline olivine and polycrystalline clinopyroxene containing trace amount of graphite from natural crystals

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