Fluid Dynamics of a Terrestrial Magma Ocean

By V. Solomatov. 2000

231 citations recorded by the source corpus.

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Citations in the corpus

The lunar magma ocean: Reconciling the solidification process with lunar petrology and geochronology (2011, background): “This unstable density gradient is created in three ways: by temperature, fractionation of magnesium and iron, and late solidification of dense iron, chromium, and titanium-bearing oxides (Hess and Parmentier, 1995; Solomatov, 2000 and references therein).”
Melting and mixing states of the Earth’s mantle after the Moon-forming impact (2015, background): “…of a compositionally distinct basal magma ocean could have been accomplished in less than 106 yr compared to the likely time between giant impacts plausibly ∼ 107 years (without an atmosphere, the majority of the mantle could have crystallized as short as 103 years, Solomatov 2000).”
Simulations of a late lunar-forming impact (2004, background): “…isen-tropic temperature proﬁle, dT/dP = αT/ρC p , where α is the coefﬁcient of thermal expansion and C p is the spe-ciﬁc heat at constant pressure (e.g., Solomatov, 2000, and values therein), and a constant average density ρ , so that P(r) = 2 πGρ 2 (R − r) 2 / 3, where R is the object radius…”
Evidence for multiple magma ocean outgassing and atmospheric loss episodes from mantle noble gases (2013, background): “Regions in the deep mantle could escape melting because the distribution of energy during a giant impact is heterogeneous (Solomatov, 2000).”
Origin and evolution of the atmospheres of early Venus, Earth and Mars (2018, background): “Silicate liquids have a low viscosity in the range between ≈ 0.01−1 Pa s at the conditions typical of magma oceans (e.g. Karki and Stixrude 2010), which are thus expected to undergo turbulent convection and to cool and crystallize rapidly (e.g. Abe 1997; Solomatov 2000).”
Heterogeneous accretion, composition and core–mantle differentiation of the Earth (2011, background): “A series of magma oceans is likely if the crystallisation time for the bulk of a deepmagma ocean is short, i.e. on the order of 103 years (Solomatov, 2000).”
Thermal and Magmatic Evolution of the Moon (2006, background): “However, if surface recycling was inefficient, thereby slowing convection beneath the lunar crust, the crystallization time would be longer (Solomatov and Moresi 1996; Solomatov 2000).”
Thermal Properties of Rocks and Density of Fluids (2014, background): “…have existed for about 1–10 million years (Spohn and Schubert 1991), while others argue that it could have remained for 100–200 million years (Abe 1997; Pollack 1997), and could have persisted for even a few hundred million years in the case of a thick early atmosphere (Abe 1997; Solomatov 2000).”
Magma ocean fractional crystallization and cumulate overturn in terrestrial planets: Implications for Mars (2003, background): “The ability of crystals to accumulate at the bottom depends on a competition between settling and entrainment (Martin and Nokes 1989; Tonks and Melosh 1990; Solomatov and Stevenson 1993a, b; Solomatov 2000).”
Possible formation of ancient crust on Mars through magma ocean processes (2005, background): “A gravitationally unstable stratigraphy will overturn via Rayleigh-Taylor instabilities to a stable profile with intrinsically densest materials at the bottom, on timescales that depend on the rate of thermally activated creep [Solomatov, 2000; Elkins-Tanton et al., 2003a].”
Thermodynamics of silicate liquids in the deep Earth (Invited) (2009, unknown): “Crystallization of an initially molten mantle begins at mid-mantle depths, rather than at the base of the mantle as found in many previous analyses that did not take into account the increase of γwith compression (Miller et al., 1991b; Solomatov, 2000; Walter and Tronnes, 2004).”
Linked magma ocean solidification and atmospheric growth for Earth and Mars (2008, background): “A gravitationally unstable stratigraphy will overturn via Rayleigh–Taylor instabilities to a stable profile with intrinsically densest materials at the bottom, on timescales that depend on the rate of thermallyactivated creep (Solomatov, 2000; Elkins-Tanton et al., 2003).”
The timeline of the lunar bombardment: Revisited (2018, background): “a ocean crystallization because the upper late-crystallizing mantle layer was enriched in Fe/Mg and contained late-crystallizing dense oxide phases such as FeTiO3 ilmenite (Hess and Parmentier, 1995; Solomatov, 2000; Elkins-Tanton et al., 2011). The unstable density structure caused mantle overturn ”
Differentiated Planetesimals and the Parent Bodies of Chondrites (2013, background): “Heat flux from the convecting magma ocean is proportional to Rayleigh number to the one-third power, and in the soft convective regime, convective velocity is proportional to heat flux to the one-third power (Solomatov 2000).”