The origin, history and role of water in the evolution of the inner Solar System

Russell, S. S.; Ballentine, C. J.; Grady, M. M.

doi:10.1098/rsta.2017.0108

Cited by 5 publications

(3 citation statements)

References 21 publications

(23 reference statements)

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“…Indeed, noble gases clearly show that there is a solar component in the Earth's mantle (e.g. [112]). …”

Section: Minor Contributors To Volatile Budgetsmentioning

confidence: 99%

The origin of inner Solar System water

Alexander¹

2017

Phil. Trans. R. Soc. A.

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Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt (‘classical’ model) or in the outer Solar System (5–15 AU in the Grand Tack model). To test these models, at present the H isotopes of water are the most promising indicators of formation location because they should have become increasingly D-rich with distance from the Sun. The estimated initial H isotopic compositions of water accreted by the CI, CM, CR and Tagish Lake carbonaceous chondrites were much more D-poor than measured outer Solar System objects. A similar pattern is seen for N isotopes. The D-poor compositions reflect incomplete re-equilibration with H 2 in the inner Solar System, which is also consistent with the O isotopes of chondritic water. On balance, it seems that the carbonaceous chondrites and their water did not form very far out in the disc, almost certainly not beyond the orbit of Saturn when its moons formed (approx. 3–7 AU in the Grand Tack model) and possibly close to where they are found today. This article is part of the themed issue ‘The origin, history and role of water in the evolution of the inner Solar System’.

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“…Indeed, noble gases clearly show that there is a solar component in the Earth's mantle (e.g. [112]). …”

Section: Minor Contributors To Volatile Budgetsmentioning

confidence: 99%

The origin of inner Solar System water

Alexander¹

2017

Phil. Trans. R. Soc. A.

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“…Recent models of ingassing of nebular hydrogen into the magma ocean show that only 1% of water entered the planet in this way (Wu et al 2018). The current general consensus is that the Earth acquired its water inventory largely via accretion of chondritic materials (Russell et al 2017). Also, experiments of metal-silicate partitioning require the presence of a hydrous magma ocean to account for the characteristics of certain trace-elements of the Earth (e.g.…”

Section: Introductionmentioning

confidence: 99%

Evolution and Spectral Response of a Steam Atmosphere for Early Earth with a Coupled Climate–Interior Model

Katyal

Nikolaou

Godolt

et al. 2019

ApJ

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The evolution of Earth's early atmosphere and the emergence of habitable conditions on our planet are intricately coupled with the development and duration of the magma ocean phase during the early Hadean period (4 to 4.5 Ga). In this paper, we deal with the evolution of the steam atmosphere during the magma ocean period. We obtain the outgoing longwave radiation using a line-by-line radiative transfer code GARLIC. Our study suggests that an atmosphere consisting of pure H 2 O, built as a result of outgassing extends the magma ocean lifetime to several million years. The thermal emission as a function of solidification timescale of magma ocean is shown. We study the effect of thermal dissociation of H 2 O at higher temperatures by applying atmospheric chemical equilibrium which results in the formation of H 2 and O 2 during the early phase of the magma ocean. A 1-6% reduction in the OLR is seen. We also obtain the effective height of the atmosphere by calculating the transmission spectra for the whole duration of the magma ocean. An atmosphere of depth 100 km is seen for pure water atmospheres. The effect of thermal dissociation on the effective height of the atmosphere is also shown. Due to the difference in the absorption behavior at different altitudes, the spectral features of H 2 and O 2 are seen at different altitudes of the atmosphere. Therefore, these species along with H 2 O have a significant contribution to the transmission spectra and could be useful for placing observational constraints upon magma ocean exoplanets.

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“…It was demonstrated that the structure and dynamics of the water–olivine interface are strongly affected by the surrounding conditions such as water fugacity and temperatures. Our collective understanding of the structure, dynamics, and vibrational behavior of water on forsterite sets the stage for interrogating more complex mineral–water interactions such as the uptake, stability, and storage of water on interstellar particles as they agglomerate and evolve into larger entities, ultimately leading to protoplanet formation. − Understanding interfacial water behavior in this context provides the foundation for addressing the origin and evolution of water on Earth starting from deep time. Further, this detailed knowledge of water on forsterite acts as the stepping stone to explore surface reactivity involving dissolution and alteration to new phases, such as serpentine, relevant to subaerial weathering and subsurface systems.…”

Section: Discussionmentioning

confidence: 99%

Vibrational Behavior of Water Adsorbed on Forsterite (Mg₂SiO₄) Surfaces

Liu

Gautam

Daemen

et al. 2020

ACS Earth Space Chem.

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The dynamics of water on or in a mineral substrate plays an important role in interfacial processes. This is because the structure and dynamics of interfacial water deviate from those of bulk water due to the change of interactions between surface water molecules and the interactions between the surface water and the substrate. This work presents a study of the vibrational behavior of water on a forsterite (Mg- end member of olivine) surface using inelastic neutron scattering (INS) and molecular dynamics (MD) simulations as complementary tools. The synthetic nano-forsterite used (dominated by the (010) crystal face), i.e., “dry” sample, inherently has a partial hydration/hydroxylation layer on the surface, as shown by previous studies and TGA. In the INS experiments, three water loadings (0.5, 1, and 2 monolayers) were added to the nano-forsterite surfaces. For samples with lower water loadings, i.e., dry and 0.5 monolayers, the INS spectra exhibited a red shift (lower frequency) of the water libration band and strengthening (blue shift, higher frequency) of the O–H stretching modes, implying weakening of the hydrogen bonding acting on the water molecules. In the simulations, we modeled the forsterite (010) surface and titrated it with two water loadings representing the lower and higher experimental water loadings. The lower loading in the simulation is equivalent to the dry and 0.5 monolayer samples in the experiment, thus suggesting weak hydrogen bonding between water molecules. The higher-loading simulation emulates the multilayer adsorption experiment. This produced a more significant shift of the vibrational bands, implying increased hydrogen-bonding strength and disorder between water molecules. The MD simulations complement the INS study by providing a detailed interfacial structure, and the combination of the two approaches provides a fundamental understanding of how the presence of the olivine surface impacts the vibrational behavior of water under different degrees of hydrationa phenomenon widely associated with terrestrial and extraterrestrial surfaces and near-surface processes.

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The origin, history and role of water in the evolution of the inner Solar System

Abstract: One contribution of 9 to a Theo Murphy meeting issue 'The origin, history and role of water in the evolution of the inner Solar System'.

Cited by 5 publications

References 21 publications

The origin of inner Solar System water

The origin of inner Solar System water

Evolution and Spectral Response of a Steam Atmosphere for Early Earth with a Coupled Climate–Interior Model

Vibrational Behavior of Water Adsorbed on Forsterite (Mg₂SiO₄) Surfaces

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The origin, history and role of water in the evolution of the inner Solar System

Abstract: One contribution of 9 to a Theo Murphy meeting issue 'The origin, history and role of water in the evolution of the inner Solar System'.

Cited by 5 publications

References 21 publications

The origin of inner Solar System water

The origin of inner Solar System water

Evolution and Spectral Response of a Steam Atmosphere for Early Earth with a Coupled Climate–Interior Model

Vibrational Behavior of Water Adsorbed on Forsterite (Mg2SiO4) Surfaces

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Vibrational Behavior of Water Adsorbed on Forsterite (Mg₂SiO₄) Surfaces