The lunar core can be a major reservoir for volatile elements S, Se, Te and Sb

Steenstra, E. S.; Lin, Yanhao; Dankers, D.; Rai, Nachiketa; Berndt, Jasper; Matveev, Sergei; Westrenen, W. van

doi:10.1038/s41598-017-15203-0

Cited by 31 publications

(57 citation statements)

References 51 publications

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“…at ∼88 PCS at a very high initial LMO S content of 300 ppm). However, in our view a bulk S content of the LMO, that is, similar to or exceeds the present‐day BSE is unlikely given that significant quantities of lunar mantle S should have partitioned into the lunar core, given the siderophile behavior of S under lunar‐relevant P‐T conditions (Steenstra et al., 2017b). As shown in Steenstra et al.…”

Section: Discussionmentioning

confidence: 68%

“…However, in our view a bulk S content of the LMO, that is, similar to or exceeds the present-day BSE is unlikely given that significant quantities of lunar mantle S should have partitioned into the lunar core, given the siderophile behavior of S under lunar-relevant P-T conditions (Steenstra et al, 2017b). As shown in Steenstra et al (2017b), core formation in the Moon is expected to have resulted in the S contents of the present-day bulk silicate Moon (∼75 ppm), consistent with previous estimates (e.g., Chen et al, 2015;Day and Walker, 2015). This is much lower than the amount of S required for achieving S-rich sulfide liquid saturation during intermediate or late LMO crystallization-it could only result in S-rich sulfide liquid saturation at >96 PCS, in the realm of urKREEP formation.…”

Section: The Fate Of S During Lunar Magma Ocean Crystallizationmentioning

confidence: 66%

“…The effects of uncertainties in the bulk (silicate) Moon S abundances on sulfide liquid saturation were assessed by exploring a range of bulk silicate Moon S abundances (25-1,000 ppm). This range encompasses the current estimates for the abundance of S in Earth's primitive mantle (235 ± 38 ppm; Wang et al, 2018), bulk Moon (94 ± 23 ppm; Steenstra et al, 2017a) and bulk silicate Moon (74.5 ± 4.5 ppm; Chen et al, 2015;Day and Walker, 2015;Hauri et al, 2015;Steenstra et al, 2017aSteenstra et al, , 2017b.…”

Section: Modeling Approachmentioning

confidence: 84%

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The Fate of Sulfur and Chalcophile Elements During Crystallization of the Lunar Magma Ocean

et al. 2020

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Section: Discussionmentioning

confidence: 68%

Section: The Fate Of S During Lunar Magma Ocean Crystallizationmentioning

confidence: 66%

Section: Modeling Approachmentioning

confidence: 84%

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The Fate of Sulfur and Chalcophile Elements During Crystallization of the Lunar Magma Ocean

et al. 2020

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“…At these conditions, a significant reduction in liquidus (and solidus) T is best accomplished by sulfur, with a steep gradient of the liquidus toward the eutectic composition, at least to 60 GPa (Buono & Walker, ). Based on this behavior and supported by geochemical arguments (Malavergne et al, ; McSween, ; Steenstra et al, ), it is not surprising that core models of the Moon, Mercury, and Mars largely rely on its presence (e.g., Helffrich, ; Laneuville et al, ; Rivoldini & Van Hoolst, ).…”

Section: Smaller Terrestrial Bodiesmentioning

confidence: 88%

Liquid Iron Equation of State to the Terapascal Regime From Ab Initio Simulations

Wagle

Steinle‐Neumann

2019

JGR Solid Earth

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We present a thermodynamic model for liquid iron, based on ab initio molecular dynamics simulations, which is applicable to 2 TPa and beyond 10000 K, conditions that are relevant in the cores of super-Earths. We combine ab initio results for V-T-P-E with a correction scheme to match experimental properties at ambient pressure, where ab initio results show poor agreement. We explore the performance of our thermodynamic potential and various previously published models for liquid iron over a wide range of conditions: (i) at ambient pressure as a function of temperature, (ii) along the melting curve of Fe to 40 GPa, relevant for the cores of smaller terrestrial bodies in our solar system, (iii) along isentropes in the Earth's outer core, and (iv) for the core of super-Earth Kepler-36b. The correction term significantly improves the agreement of computed properties with experiments and other thermodynamic models that are based on an assessment of the phase diagram at ambient and moderate pressure, showing how ab initio molecular dynamics simulations can be used at par with other thermodynamic techniques. For the Earth's core, densities from the various models are similar, but higher-order derivatives (acoustic velocities and Grüneisen parameter) show significant differences. Evaluated along a core-temperature profile in Kepler-36b, differences in density from various models are negligible, for core mass they do not exceed 2%, showing robust extrapolation of all equation of state models. Plain Language SummaryThe cores of the inner planets in our solar system and likely other planets outside of it (super-Earths) contain a partially liquid iron core that is critical in understanding magnetic field generation and their internal structure. In order to characterize their structure, the relation between density, pressure, and temperature (equation of state) must be known. As conditions in the interior of these planets are difficult to access in experiments, we perform computer simulations on the electronic structure of iron. However, results from such simulations have been shown to inadequately represent low-pressure data and we correct for this shortcoming. By combining simulation results and the correction scheme, we develop an equation of state that is applicable over a wide range of conditions. We compare our results to experimental data and previously published models and find that they generally agree at conditions of the Earth and continue to yield consistent results for super-Earths. This robust behavior can be used in analyzing their structure once relevant astronomical observations become available.

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“…tioning of trace elements (e.g. Steenstra et al 2017). The concentrations of S and HSEs in Earth's mantle prior to the Moon forming event are unknown but plausible values can be obtained from the model of Rubie et al (2016), namely ∼ 300 ppm S, 1.9 ppb Pt, 16 ppb Pd, 3.4 ppb Ru and 1.4 ppb Ir.…”

Section: A Reanalysis Of the Cataclysmic Scenariomentioning

confidence: 99%

The timeline of the lunar bombardment: Revisited

Morbidelli

Nesvorný²,

Laurenz

et al. 2018

Icarus

228

257

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The timeline of the lunar bombardment in the first Gy of Solar System history remains unclear. Basin-forming impacts (e.g. Imbrium, Orientale), occurred 3.9-3.7 Gy ago, i.e. 600-800 My after the formation of the Moon itself. Many other basins formed before Imbrium, but their exact ages are not precisely known. There is an intense debate between two possible interpretations of the data: in the cataclysm scenario there was a surge in the impact rate approximately at the time of Imbrium formation, while in the accretion tail scenario the lunar bombardment declined since the era of planet formation and the latest basins formed in its tail-end. Here, we revisit the work of that examined which scenario could be compatible with both the lunar crater record in the 3-4 Gy period and the abundance of highly siderophile elements (HSE) in the lunar mantle. We use updated numerical simulations of the fluxes of asteroids, comets and planetesimals leftover from the planet-formation process. Under the traditional assumption that the HSEs track the total amount of material accreted by the Moon since its formation, we conclude that only the cataclysm scenario can explain the data. The cataclysm should have started ∼ 3.95 Gy ago. However we also consider the possibility that HSEs are sequestered from the mantle of a planet during magma ocean crystallization, due to iron sulfide exsolution (O'Neil, 1991;. We show that this is likely true also for the Moon, if mantle overturn is taken into account. Based on the hypothesis that the lunar magma ocean crystallized about 100-150 My after Moon formation (Elkins-Tanton et al., 2011), and therefore that HSEs accumulated in the lunar mantle only after this timespan, we show that the bombardment in the 3-4 Gy period can be explained in the accretion tail scenario. This hypothesis would also explain why the Moon appears so depleted in HSEs relative to the Earth. We also extend our analysis of the cataclysm and accretion tail scenarios to the case of Mars. The accretion tail scenario requires a global resurfacing event on Mars ∼ 4.4Gy ago, possibly associated with the formation of the Borealis basin, and it arXiv:1801.03756v1 [astro-ph.EP] 11 Jan 2018 -2 -is consistent with the HSE budget of the planet. Moreover it implies that the Noachian and pre-Noachian terrains are ∼ 200 My older than usually considered.

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The lunar core can be a major reservoir for volatile elements S, Se, Te and Sb

Cited by 31 publications

References 51 publications

The Fate of Sulfur and Chalcophile Elements During Crystallization of the Lunar Magma Ocean

The Fate of Sulfur and Chalcophile Elements During Crystallization of the Lunar Magma Ocean

Liquid Iron Equation of State to the Terapascal Regime From Ab Initio Simulations

The timeline of the lunar bombardment: Revisited

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