Laboratory Studies of Mantle Convection

Davaille, Anne; Limare, Angela

doi:10.1016/b978-044452748-6.00116-4

Cited by 23 publications

(26 citation statements)

References 396 publications

(566 reference statements)

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“…An exponent n = 1 ∕ 3 in equation means that heat loss is governed solely by local instabilities of the upper thermal boundary layer (TBL) and does not depend explicitly on the magma ocean thickness. It has been observed in experiments with constant viscosity for 10 6 < Ra < 10 10 with constant C 0 varying between 0.05 and 0.18 (see Siggia [] and Davaille and Limare [] for a review). On the other hand, the appearance of a large‐scale circulation connecting the top TBL to the bottom of the layer, either due to turbulent motions in confined boxes (for 10 8 < Ra < 10 14 , see Castaing [] and Grossmann and Lohse []) or due to large viscosity variations [e.g., Solomatov and Moresi , ; Androvandi et al , ] would give an exponent lower than 1 ∕ 3.…”

Section: The Modelmentioning

confidence: 92%

Thermal evolution of an early magma ocean in interaction with the atmosphere

et al. 2013

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[1] The thermal evolution of magma oceans produced by collision with giant impactors late in accretion is expected to depend on the composition and structure of the atmosphere through the greenhouse effect of CO 2 and H 2 O released from the magma during its crystallization. In order to constrain the various cooling timescales of the system, we developed a 1-D parameterized convection model of a magma ocean coupled with a 1-D radiative-convective model of the atmosphere. We conducted a parametric study and described the influences of the initial volatile inventories, the initial depth of the magma ocean, and the Sun-planet distance. Our results suggest that a steam atmosphere delays the end of the magma ocean phase by typically 1 Myr. Water vapor condenses to an ocean after 0.1, 1.5, and 10 Myr for, respectively, Mars, Earth, and Venus. This time would be virtually infinite for an Earth-sized planet located at less than 0.66 AU from the Sun. Using a more accurate calculation of opacities, we show that Venus is much closer to this threshold distance than in previous models. So there are conditions such as no water ocean is formed on Venus. Moreover, for Mars and Earth, water ocean formation timescales are shorter than typical time gaps between major impacts. This implies that successive water oceans may have developed during accretion, making easier the loss of their atmospheres by impact erosion. On the other hand, Venus could have remained in the magma ocean stage for most of its accretion.

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Section: The Modelmentioning

confidence: 92%

Thermal evolution of an early magma ocean in interaction with the atmosphere

et al. 2013

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“…Fluid dynamical modeling using laboratory experiments, theoretical arguments, and numerical simulations (for recent reviews, see Ribe et al . [], Ito and van Keken [], and Davaille and Limare [2007]) demonstrates that the physical characteristics of hotspots in many cases can be explained by plumes rising from the deep mantle, although shallow mantle origins have also been suggested [ King and Ritsema , ]. Seismological evidence for low velocity regions below hotspots have also been used to argue for the existence of plumes [ Montelli et al ., ; Wolfe et al ., ], although it is likely that application of standard tomographic techniques is limited due to the effects of wave front healing that may render plumes invisible in the deeper mantle [ Hwang et al ., ].…”

Section: Introductionmentioning

confidence: 99%

Dynamics of a laminar plume in a cavity: The influence of boundaries on the steady state stem structure

Keken

Davaille

Vatteville

2013

Geochem Geophys Geosyst

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[1] The steady state structure of thermal plumes rising from a small heater is studied in high Prandtl number fluids. We show good agreement between laboratory experiments and numerical simulations. We study the effect of the boundaries on the plume development by numerically simulating the plume rise in very large geometries. The thermal structure of the plume axis is similar for all box sizes considered, but the velocity structure changes strongly as box sizes are increased. We show that the effect of the side boundaries becomes unimportant for large aspect ratio, but that the free-slip top boundary has a strong influence on the velocity structure under all conditions. We show that the use of an outflow boundary condition significantly reduces the influence of the top boundary. Under these conditions we recover to good precision the theoretical predictions for plumes rising in an semi-infinite half-space. The strong influence of the boundaries in high Prandtl number fluids is important in the interpretation of laboratory experiments and numerical simulation for the dynamics of the Earth's mantle.Components: 9,800 words, 15 figures.

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“…When γ ≥ 10 4 , the "stagnant lid" regime prevails whereby convective motions develop below a stagnant viscous sublayer located at the surface, forming a "plate" (e.g., ref. [164] for a review). …”

Section: Convection In Planetary Mantlesmentioning

confidence: 99%

Drying colloidal systems: Laboratory models for a wide range of applications

et al. 2018

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Abstract. The drying of complex fluids provides a powerful insight into phenomena that take place on time and length scales not normally accessible. An important feature of complex fluids, colloidal dispersions and polymer solutions is their high sensitivity to weak external actions. Thus, the drying of complex fluids involves a large number of physical and chemical processes. The scope of this review is the capacity to tune such systems to reproduce and explore specific properties in a physics laboratory. A wide variety of systems are presented, ranging from functional coatings, food science, cosmetology, medical diagnostics and forensics to geophysics and art.

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Laboratory Studies of Mantle Convection

Cited by 23 publications

References 396 publications

Thermal evolution of an early magma ocean in interaction with the atmosphere

Thermal evolution of an early magma ocean in interaction with the atmosphere

Dynamics of a laminar plume in a cavity: The influence of boundaries on the steady state stem structure

Drying colloidal systems: Laboratory models for a wide range of applications

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