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Internal structure and dynamics of the terrestrial planets

In the PSS team, we study the dynamic evolution of terrestrial planets. To do so, we rely on simple analytical approaches or on high performance computational fluid dynamics experiments to model the exchanges of heat and of chemical species between the different envelopes that may constitute planetary bodies: metallic core, silicate enveloppes, and atmosphere. Our investigations consist in characterising the dynamics of different systems of interest e.g., long-term solid state or short-term liquid state convection in planetary interiors fragmentation of iron drops or diapirs or volatile outgassing  in planetary magma oceans.  

Numerical modelling of two end-member scenarios for the evolution of Mars. Case of a homogeneous silicate mantle (left) where thermal convection is well-developed, leading to moderate present-day temperatures, contrary to a heterogeneous case (right) for which heat transfer is reduced, resulting in the presence of deep regions with extreme temperatures.