Stirring the magma ocean with changing buoyancy and viscosity of various silicate melts
The currently accepted model of the Earth formation and evolution involves a stage of condensation from the protolunar disk or synestia into a global magma ocean. This ocean was constituted primarily from silicate melts; temperatures were considerably higher than today, while pressures considerably lower.
Variations of the composition of the magma ocean occurring from chemical heterogeneities or induced by crystallization could have considerably altered the convection pattern. Here we want to study the properties of Fe-rich melts as segregated in the last stages of the crystallization of the magma ocean.
For the first time, we will try to understand the behaviour of light elements trapped in the basal magma ocean, not only on relative buoyancy of the melt but also on its viscosity.
Structure of liquids; transport, convection and turbulence of melts; thermodynamics; petrology; use of supercomputing centres; use of python/Linux/Unix.