Chemical fractionation in the silicate vapor atmosphere of the Earth

Pahlevan, Kaveh; Stevenson, D. J.; Eiler, John M.

doi:10.1016/j.epsl.2010.10.036

Cited by 66 publications

(77 citation statements)

References 53 publications

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“…Recent theoretical studies show that too much silicate vapor would prevent the formation of moon after a giant impact [e.g., 3]. However, the presence of silicate vapor may help the equilibration of oxygen isotope [4] and the chemical fractionation of Mg# ,Mg/(Fe+Mg) [24], between the Earth and the Moon. Thus, there should be an intermediate successful range of the degree of vaporization for the giant impact hypothesis.…”

Section: Resultsmentioning

confidence: 99%

Time-resolved spectroscopic observations of shockinduced silicate ionization

Kurosawa¹,

Kadono²,

Sugita³

et al. 2012

AIP Conference Proceedings

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Section: Resultsmentioning

confidence: 99%

Time-resolved spectroscopic observations of shockinduced silicate ionization

Kurosawa¹,

Kadono²,

Sugita³

et al. 2012

AIP Conference Proceedings

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“…This would argue for a source of fresh material, which would have had to be produced within the last 0.1 Myr to be consistent with SiO recondensation. Recently, Pahlevan et al (2011) showed that silicate constituents (Si, Fe, Mg and O) can be produced in the form of gas during hypervelocity collisions. Therefore, one can speculate that the origin of atomic oxygen detected with Herschel could be the violent event proposed by Lisse et al (2009) to explain the shape of the Spitzer/IRS spectrum.…”

Section: Recent Release During a Catastrophic Eventmentioning

confidence: 99%

HD 172555: detection of 63μm [OI] emission in a debris disc

Rivière-Marichalar

Barrado

Augereau

et al. 2012

A&A

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Context. HD 172555 is a young A7 star belonging to the β Pictoris moving group that harbours a debris disc. The Spitzer/IRS spectrum of the source showed mid-IR features such as silicates and glassy silica species, indicating the presence of a warm dust component with small grains, which places HD 172555 among the small group of debris discs with such properties. The IRS spectrum also shows a possible emission of SiO gas. Aims. We aim to study the dust distribution in the circumstellar disc of HD 172555 and to asses the presence of gas in the debris disc. Methods. As part of the GASPS open time key programme, we obtained Herschel/PACS photometric and spectroscopic observations of the source. We analysed PACS observations of HD 172555 and modelled the spectral energy distribution with a modified blackbody and the gas emission with a two-level population model with no collisional de-excitation. Results. We report for the first time the detection of [OI] atomic gas emission at 63.18 μm in the HD 172555 circumstellar disc. We detect excesses due to circumstellar dust toward HD 172555 in the three photometric bands of PACS (70, 100, and 160 μm). We derive a large dust particle mass of (4.8 ± 0.6) × 10 −4 M ⊕ and an atomic oxygen mass of 2.5 × 10 −2 R 2 M ⊕ , where R in AU is the separation between the star and the inner disc. Thus, most of the detected mass of the disc is in the gaseous phase.

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“…The similarity in abundances of refractory elements implies that processes in the protolunar disc did not lead to relative fractionation of refractory elements or to a general enrichment during condensation and partial crystallization of the disc before the Moon accreted from it. Chemical models of disc processes [59][60][61] need to account for the approximate similarity with terrestrial abundances of refractory elements.…”

Section: Implications For Lunar Originmentioning

confidence: 99%

Lunar bulk chemical composition: a post-Gravity Recovery and Interior Laboratory reassessment

Taylor

Wieczorek

2014

Phil. Trans. R. Soc. A.

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New estimates of the thickness of the lunar highlands crust based on data from the Gravity Recovery and Interior Laboratory mission, allow us to reassess the abundances of refractory elements in the Moon. Previous estimates of the Moon fall into two distinct groups: earthlike and a 50% enrichment in the Moon compared with the Earth. Revised crustal thicknesses and compositional information from remote sensing and lunar samples indicate that the crust contributes 1.13–1.85 wt% Al 2 O 3 to the bulk Moon abundance. Mare basalt Al 2 O 3 concentrations (8–10 wt%) and Al 2 O 3 partitioning behaviour between melt and pyroxene during partial melting indicate mantle Al 2 O 3 concentration in the range 1.3–3.1 wt%, depending on the relative amounts of pyroxene and olivine. Using crustal and mantle mass fractions, we show that that the Moon and the Earth most likely have the same (within 20%) concentrations of refractory elements. This allows us to use correlations between pairs of refractory and volatile elements to confirm that lunar abundances of moderately volatile elements such as K, Rb and Cs are depleted by 75% in the Moon compared with the Earth and that highly volatile elements, such as Tl and Cd, are depleted by 99%. The earthlike refractory abundances and depleted volatile abundances are strong constraints on lunar formation processes.

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Chemical fractionation in the silicate vapor atmosphere of the Earth

Cited by 66 publications

References 53 publications

Time-resolved spectroscopic observations of shockinduced silicate ionization

Time-resolved spectroscopic observations of shockinduced silicate ionization

HD 172555: detection of 63μm [OI] emission in a debris disc

Lunar bulk chemical composition: a post-Gravity Recovery and Interior Laboratory reassessment

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