Dataset Information

Redox control on nitrogen isotope fractionation during planetary core formation.

ABSTRACT: The present-day nitrogen isotopic compositions of Earth's surficial (15N-enriched) and deep reservoirs (15N-depleted) differ significantly. This distribution can neither be explained by modern mantle degassing nor recycling via subduction zones. As the effect of planetary differentiation on the behavior of N isotopes is poorly understood, we experimentally determined N-isotopic fractionations during metal-silicate partitioning (analogous to planetary core formation) over a large range of oxygen fugacities (?IW -3.1 < logfO2 < ?IW -0.5, where ?IW is the logarithmic difference between experimental oxygen fugacity [fO2] conditions and that imposed by the coexistence of iron and wüstite) at 1 GPa and 1,400 °C. We developed an in situ analytical method to measure the N-elemental and -isotopic compositions of experimental run products composed of Fe-C-N metal alloys and basaltic melts. Our results show substantial N-isotopic fractionations between metal alloys and silicate glasses, i.e., from -257 ± 22‰ to -49 ± 1‰ over 3 log units of fO2 These large fractionations under reduced conditions can be explained by the large difference between N bonding in metal alloys (Fe-N) and in silicate glasses (as molecular N2 and NH complexes). We show that the ?15N value of the silicate mantle could have increased by ?20‰ during core formation due to N segregation into the core.

SUBMITTER: Dalou C

PROVIDER: S-EPMC6642344 | biostudies-literature | 2019 Jul

REPOSITORIES: biostudies-literature

ACCESS DATA

Publications

Redox control on nitrogen isotope fractionation during planetary core formation.

Dalou Celia C Füri Evelyn E Deligny Cécile C Piani Laurette L Caumon Marie-Camille MC Laumonier Mickael M Boulliung Julien J Edén Mattias M

Proceedings of the National Academy of Sciences of the United States of America 20190701 29

The present-day nitrogen isotopic compositions of Earth's surficial (<sup>15</sup>N-enriched) and deep reservoirs (<sup>15</sup>N-depleted) differ significantly. This distribution can neither be explained by modern mantle degassing nor recycling via subduction zones. As the effect of planetary differentiation on the behavior of N isotopes is poorly understood, we experimentally determined N-isotopic fractionations during metal-silicate partitioning (analogous to planetary core formation) over a ...[more]

PMID: 31262822

Similar Datasets

Project description:Silicon and Mg in differentiated rocky bodies exhibit heavy isotope enrichments that have been attributed to evaporation of partially or entirely molten planetesimals. We evaluate the mechanisms of planetesimal evaporation in the early solar system and the conditions that controled attendant isotope fractionations. Energy balance at the surface of a body accreted within ~1 Myr of CAI formation and heated from within by 26Al decay results in internal temperatures exceeding the silicate solidus, producing a transient magma ocean with a thin surface boundary layer of order < 1 meter that would be subject to foundering. Bodies that are massive enough to form magma oceans by radioisotope decay (? 0.1% M ?) can retain hot rock vapor even in the absence of ambient nebular gas. We find that a steady-state rock vapor forms within minutes to hours and results from a balance between rates of magma evaporation and atmospheric escape. Vapor pressure buildup adjacent to the surfaces of the evaporating magmas would have inevitably led to an approach to equilibrium isotope partitioning between the vapor phase and the silicate melt. Numerical simulations of this near-equilibrium evaporation process for a body with a radius of ~ 700 km yield a steady-state far-field vapor pressure of 10-8 bar and a vapor pressure at the surface of 10-4 bar, corresponding to 95% saturation. Approaches to equilibrium isotope fractionation between vapor and melt should have been the norm during planet formation due to the formation of steady-state rock vapor atmospheres and/or the presence of protostellar gas. We model the Si and Mg isotopic composition of bulk Earth as a consequence of accretion of planetesimals that evaporated subject to the conditions described above. The results show that the best fit to bulk Earth is for a carbonaceous chondrite-like source material with about 12% loss of Mg and 15% loss of Si resulting from near-equilibrium evaporation into the solar protostellar disk of H2 on timescales of 104 to 105 years.

Project description:The naturally occurring nitrogen (N) isotopes, 15N and 14N, exhibit different reaction rates during many microbial N transformation processes, which results in N isotope fractionation. Such isotope effects are critical parameters for interpreting natural stable isotope abundances as proxies for biological process rates in the environment across scales. The kinetic isotope effect of ammonia oxidation (AO) to nitrite (NO2 -), performed by ammonia-oxidizing archaea (AOA) and ammonia-oxidizing bacteria (AOB), is generally ascribed to the enzyme ammonia monooxygenase (AMO), which catalyzes the first step in this process. However, the kinetic isotope effect of AMO, or ? A M O , has been typically determined based on isotope kinetics during product formation (cumulative product, NO2 -) alone, which may have overestimated ? A M O due to possible accumulation of chemical intermediates and alternative sinks of ammonia/ammonium (NH3/NH4 +). Here, we analyzed 15N isotope fractionation during archaeal ammonia oxidation based on both isotopic changes in residual substrate (RS, NH4 +) and cumulative product (CP, NO2 -) pools in pure cultures of the soil strain Nitrososphaera viennensis EN76 and in highly enriched cultures of the marine strain Nitrosopumilus adriaticus NF5, under non-limiting substrate conditions. We obtained ? A M O values of 31.9-33.1‰ for both strains based on RS (?15NH4 +) and showed that estimates based on CP (?15NO2 -) give larger isotope fractionation factors by 6-8‰. Complementary analyses showed that, at the end of the growth period, microbial biomass was 15N-enriched (10.1‰), whereas nitrous oxide (N2O) was highly 15N depleted (-38.1‰) relative to the initial substrate. Although we did not determine the isotope effect of NH4 + assimilation (biomass formation) and N2O production by AOA, our results nevertheless show that the discrepancy between ? A M O estimates based on RS and CP might have derived from the incorporation of 15N-enriched residual NH4 + after AMO reaction into microbial biomass and that N2O production did not affect isotope fractionation estimates significantly.

Dataset Information

Redox control on nitrogen isotope fractionation during planetary core formation.

Publications

Redox control on nitrogen isotope fractionation during planetary core formation.

Similar Datasets

OmicsDI is part of the ELIXIR infrastructure

Tweets