Impact melt pools: the aftermath of planetary-scale impacts

At the end of the planetary formation stage, collisions of leftover planetesimals onto planetary bodies are very common. While small impacts are known to form impact craters and basins on the planetary surface, the biggest and most energetic impacts can be disruptive. However, the consequence of moderately energetic impacts have not been as widely observed and studied, even though impactors of such sizes are expected to be common in the first few million years of planetary formation. My research interests focus on modelling the interior dynamics and surface features of terrestrial planets in our Solar System. Previously, I have run mantle convection models to demonstrate how such an intermediate planetary-scale impact may form the Crustal Dichotomy of Mars. Now, I would like to extend my study to understand in details how magma convection and solidification within the original impact melt pool can influence the differentiation into crust and residue in the first place.My proposed project aims to apply a state-of-the-art magma dynamics model to study the evolution of impact melt ponds from fully molten state to completely solid, consisting of three work packages. The first work package includes the testing of parameters and setups suitable for post-impact conditions. The second work package focuses on modelling known impact basins on the Moon. The advantage of using known impact basins as testing grounds will allow me to compare model results to plentiful of space mission data, which will be useful to constrain the models. Finally, the third work package first examines impact basins of Mars, and then extend to larger systems to address questions regarding the Martian Dichotomy formation.Aiming to serve as a bridge between the planetary impact and magma dynamics fields, results from this proposed project will help unravel the mystery of the biggest impact structures, and provide insight to the earliest part planetary history.