Liquids are the most dynamic phases present in planetary interiors. As the primary means of transporting both heat and mass, liquids are the major players in a wide of earth and planetary science questions: what controls volcanic eruptions dynamics? How do planets evolve during differentiation? How does the presences of melts produce or modify geophysical observables (e.g. low velocity zones, high electrical conductivity)? How are volatiles and incompatible elements stored during planetary formation? How is stress accommodated in shear zones and at the LAB? What is the temperature profile of the core? And many others.

The aim of this session is to evaluate recent data from all relevant fields – experimental, computational, geochemical, geophysical, etc. – with implications for understanding the role of liquids in planetary interiors spanning processes relevant from crust to core and from formation to present-day structures.