Thermal and chemical evolution of the terrestrial magma ocean

Abe, Yutaka

doi:10.1016/s0031-9201(96)03229-3

Cited by 291 publications

(252 citation statements)

References 29 publications

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“…5 Log of resulting water ocean depth in meters produced by a collapsed degassed atmosphere of a planet of given mass and initial bulk mantle water content. Water contents far less than 1 mass% would likely produce near-planetary water oceans within tens of millions of years of the last accretionary impact have passed the critical point of water and cooled into the liquid water stability field (Abe 1997;Elkins-Tanton 2008).…”

Section: Resultsmentioning

confidence: 99%

Formation of early water oceans on rocky planets

Elkins-Tanton

2010

Astrophys Space Sci

103

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Terrestrial planets, with silicate mantles and metallic cores, are likely to obtain water and carbon compounds during accretion. Here I examine the conditions that allow early formation of a surface water ocean (simultaneous with cooling to clement surface conditions), and the timeline of degassing the planetary interior into the atmosphere. The greatest fraction of a planet's initial volatile budget is degassed into the atmosphere during the end of magma ocean solidification, leaving only a small fraction of the original volatiles to be released into the atmosphere through later volcanism. Rocky planets that accrete with water in their bulk mantle have two mechanisms for producing an early water ocean: First, if they accrete with at least 1 to 3 mass% of water in their bulk composition, liquid water may be extruded onto the planetary surface at the end of magma ocean solidification. Second, at initial water contents as low as 0.01 mass% or lower, during solidification a massive supercritical fluid and steam atmosphere is produced that collapses into a water ocean upon cooling. The low water contents required for this process indicate that rocky super-Earth exoplanets may be expected to commonly produce water oceans within tens to hundreds of millions of years of their last major accretionary impact, through collapse of their atmosphere.

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Section: Resultsmentioning

confidence: 99%

Formation of early water oceans on rocky planets

Elkins-Tanton

2010

Astrophys Space Sci

103

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“…U nderstanding the structural response of silicate melts to pressure and composition is crucial in earth and planetary sciences, as the differentiation of chemical species within planetary interiors is primarily controlled by melting and crystallization processes, which are intimately linked to evolution histories and thermal states of the planets [1][2][3] . Quenching of pressurized oxide melts may also produce new materials, such as densified glasses with novel and tailored properties [4][5][6] .…”

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confidence: 99%

Atomistic insight into viscosity and density of silicate melts under pressure

et al. 2014

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A defining characteristic of silicate melts is the degree of polymerization (tetrahedral connectivity), which dictates viscosity and affects compressibility. While viscosity of depolymerized silicate melts increases with pressure consistent with the free-volume theory, isothermal viscosity of polymerized melts decreases with pressure up to B3-5 GPa, above which it turns over to normal (positive) pressure dependence. Here we show that the viscosity turnover in polymerized liquids corresponds to the tetrahedral packing limit, below which the structure is compressed through tightening of the inter-tetrahedral bond angle, resulting in high compressibility, continual breakup of tetrahedral connectivity and viscosity decrease with increasing pressure. Above the turnover pressure, silicon and aluminium coordination increases to allow further packing, with increasing viscosity and density. These structural responses prescribe the distribution of melt viscosity and density with depth and play an important role in magma transport in terrestrial planetary interiors.

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“…the core-mantle boundary, are accounted for by constant temperature jumps according to Earth-like values. A mixing length formulation (Sasaki & Nakazawa 1986, Abe 1997) is adopted to calculate the radial distribution of temperature within the upper mantle and to simulate a lithospheric structure within the uppermost part. The basic idea behind this concept is that internally generated heat is primarily transfered by vertical motion of fluid parcels which, after migrating for size-dependent characteristic length scales, will entirely loose their individuality.…”

Section: Introduction and Methodsologymentioning

confidence: 99%

Interior structure models of terrestrial exoplanets and application to CoRoT-7 b

et al. 2009

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Abstract. In this study, we model the internal structure of CoRoT-7 b, considered as a typical extrasolar terrestrial planet, using mass and energy balance constraints. Our results suggest that the deep interior is predominantly composed of dry silicate rock, similar to the Earth's Moon. A central iron core, if present, would be relatively small and less massive (<15 wt.% of the planet's total mass) as compared to the Earth's (core mass fraction 32.6 wt.%). Furthermore, a partly molten near-surface magma ocean could be maintained, provided surface temperatures were high enough and the rock component mainly composed of Earth-like mineral phase assemblages.

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Thermal and chemical evolution of the terrestrial magma ocean

Cited by 291 publications

References 29 publications

Formation of early water oceans on rocky planets

Formation of early water oceans on rocky planets

Atomistic insight into viscosity and density of silicate melts under pressure

Interior structure models of terrestrial exoplanets and application to CoRoT-7 b

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