Magma Oceans and Primordial Mantle Differentiation

Solomatov, V. S.

doi:10.1016/b978-044452748-6.00141-3

Cited by 146 publications

(255 citation statements)

References 226 publications

Supporting

Mentioning

246

Contrasting

Unclassified

Order By: Relevance

“…Hartmann & Davis 1975) evolved with substantial debate on an impact-triggered origin of the Earth-Moon system (for an overview, see Canup & Righter (2000)) that continues to the present day (Stevenson 2007(Stevenson , 2008. Recently, the possibility of more energetic collisions has led to possible extension of the magma ocean depth through high-temperature impactor core implantation (Canup 2004;Rubie et al 2007;Solomatov 2007) and early tidal heating. The late stage Mars-like impact scenario (Halliday & Wood 2007) suggests that final equilibration in the Earth is likely to have taken place under mid-mantle pressures or greater and at higher temperatures.…”

Section: High-pressure Experiments and The Planetary Contextmentioning

confidence: 99%

Partitioning experiments in the laser-heated diamond anvil cell: volatile content in the Earth's core

Jephcoat

Bouhifd

Porcelli

2008

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

The present state of the Earth evolved from energetic events that were determined early in the history of the Solar System. A key process in reconciling this state and the observable mantle composition with models of the original formation relies on understanding the planetary processing that has taken place over the past 4.5 Ga. Planetary size plays a key role and ultimately determines the pressure and temperature conditions at which the materials of the early solar nebular segregated. We summarize recent developments with the laser-heated diamond anvil cell that have made possible extension of the conventional pressure limit for partitioning experiments as well as the study of volatile trace elements. In particular, we discuss liquid-liquid, metal-silicate (M-Sil) partitioning results for several elements in a synthetic chondritic mixture, spanning a wide range of atomic number-helium to iodine. We examine the role of the core as a possible host of both siderophile and trace elements and the implications that early segregation processes at deep magma ocean conditions have for current mantle signatures, both compositional and isotopic. The results provide some of the first experimental evidence that the core is the obvious replacement for the long-sought, deep mantle reservoir. If so, they also indicate the need to understand the detailed nature and scale of core-mantle exchange processes, from atomic to macroscopic, throughout the age of the Earth to the present day.

show abstract

Section: High-pressure Experiments and The Planetary Contextmentioning

confidence: 99%

Partitioning experiments in the laser-heated diamond anvil cell: volatile content in the Earth's core

Jephcoat

Bouhifd

Porcelli

2008

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

show abstract

“…This theory is applicable because the boundary layer was thin compared with the convecting region (e.g. [36][37][38]). We present basic scaling relationships for the thickness of the boundary layer, its rate of sinking and the convective heat flow, following Sleep [39].…”

Section: Physics Of Convection Within the Nascent Earthmentioning

confidence: 99%

“…For example, Stockstill-Cahill [46] computed 0.02 Pa s at 1950 K liquidus for mercurian peridotitic komatiite. Solomatov [38] assumed 0.1 Pa s in his calculations. We will assume that η liq = 0.01 Pa s. The values of the other parameters in (4.7) are well constrained and apply to both liquid and solid mantle; we let ρ be 3300 kg m −3 ; k be 2.5 W m −1 K −1 ; C be 1.25 × 10 3 J kg −1 K −1 ; g be 9.8 m s −2 ; and α be 3 × 10 −5 K −1 .…”

Section: (B) Qualitative Thermal Historymentioning

confidence: 99%

“…The appropriate multiplicative constant A in (4.7) for convection beneath a free surface (here, the atmosphere) is approximately 0.089 if we assume that the convection is mildly turbulent [38]. We retain T ηL to be 100 K and round η liq to the value of 0.01 Pa s. The predicted heat flow q v in (4.1) for mildly turbulent flow is then 5.6 × 10 4 W m −2 .…”

Section: (D) Fully Molten Mantle Convectionmentioning

confidence: 99%

See 1 more Smart Citation

Terrestrial aftermath of the Moon-forming impact

Sleep

Zahnle

Lupu

2014

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

Much of the Earth's mantle was melted in the Moon-forming impact. Gases that were not partially soluble in the melt, such as water and CO 2 , formed a thick, deep atmosphere surrounding the post-impact Earth. This atmosphere was opaque to thermal radiation, allowing heat to escape to space only at the runaway greenhouse threshold of approximately 100 W m −2 . The duration of this runaway greenhouse stage was limited to approximately 10 Myr by the internal energy and tidal heating, ending with a partially crystalline uppermost mantle and a solid deep mantle. At this point, the crust was able to cool efficiently and solidified at the surface. After the condensation of the water ocean, approximately 100 bar of CO 2 remained in the atmosphere, creating a solar-heated greenhouse, while the surface cooled to approximately 500 K. Almost all this CO 2 had to be sequestered by subduction into the mantle by 3.8 Ga, when the geological record indicates the presence of life and hence a habitable environment. The deep CO 2 sequestration into the mantle could be explained by a rapid subduction of the old oceanic crust, such that the top of the crust would remain cold and retain its CO 2 . Kinematically, these episodes would be required to have both fast subduction (and hence seafloor spreading) and old crust. Hadean oceanic crust that formed from hot mantle would have been thicker than modern crust, and therefore only old crust underlain by cool mantle lithosphere could subduct. Once subduction started, the basaltic crust would turn into dense eclogite, increasing the rate of subduction. The rapid subduction would stop when the young partially frozen crust from the rapidly spreading ridge entered the subduction zone.

show abstract

“…The mantle of the post-giant impact Earth will cool very fast at first 12 , limited only by the black-body radiation that can escape from the top of the transient (initially silicate vapour) atmosphere. The thermal structure of the mantle is expected to be close to isentropic because that is the state of neutral buoyancy and therefore the state preferred by convection, provided that viscosity is low.…”

Section: Mantle Differentiationmentioning

confidence: 99%

A planetary perspective on the deep Earth

Stevenson

2008

Nature

View full text Add to dashboard Cite

Earth is an engine, tending to obliterate some of the evidence of events that are distant in time, but a memory is retained in its chemistry, its isotopes, the presence of the Moon, perhaps also in geophysical observables such as the temperature of the core and the nature of the mantle immediately above the core, and maybe even in the existence of plate tectonics and life. The remarkable growth in the study and understanding of Earth has happened in parallel with a spectacular era of planetary exploration, relevant astronomical discoveries and computational and theoretical advances, all of which help us to place Earth and its interior in a perspective that integrates the Earth sciences with extraterrestrial studies and basic sciences such as condensed-matter physics. However, progress on the biggest challenges in understanding the deep Earth continues to rely mainly on looking down rather than looking up. A planetary perspectiveEarth is a planet -one of many. There is nothing particularly remarkable about our home, except perhaps that it is suitable for life like us -arguably a tautology. It happens to be the largest of its type in the Solar System, but as there are only three others of the terrestrial type (Mercury, Venus and Mars) this is not particularly significant. Among planets in general, it is small.In the past decade, we have seen an astonishing explosion in our catalogue of planets outside the Solar System to about 250 so far (see the Extrasolar Planets Encyclopaedia, http://exoplanet.eu/ catalog.php). These are mostly planets that we suspect are like Jupiter, very different from Earth. But as time goes on and detection methods improve, we can expect to find bodies that are Earth-like at least to the extent of being made predominantly of rock and iron, the primary constituents of our planet. Some would claim we might already be finding such bodies 1 , initially those that are more massive than Earth.If planets were like atoms or molecules, or even crystals, we could speak of their characteristics (their DNA, so to speak) in a very compact way, just as a handbook might list the properties of a material. Planets are richer, more complex and more resistant to reductionist thinking. Genetics is the science of heredity and variation in biological systems. By analogy, we can speak of the genetics of a planet such as Earth, while also acknowledging that environment has a role in its evolution and its current state.Cosmologists are familiar with thinking about time logarithmically: a lot happened in a very short period of time back near the Big Bang. To some extent, it helps to think about planet formation in a similar way (Fig. 1). The events that defined Earth's formation and the initial conditions for its subsequent evolution are squeezed into an epoch that may have already been over within 100 million years of the formation of the Solar System. In this epoch more happened inside Earth and more energy was dissipated from within the planet than throughout all of subsequent geological time. We have no direct ...

show abstract

Magma Oceans and Primordial Mantle Differentiation

Cited by 146 publications

References 226 publications

Partitioning experiments in the laser-heated diamond anvil cell: volatile content in the Earth's core

Partitioning experiments in the laser-heated diamond anvil cell: volatile content in the Earth's core

Terrestrial aftermath of the Moon-forming impact

A planetary perspective on the deep Earth

Contact Info

Product

Resources

About