This is the second paper in a two-part series examining the fluid dynamics of crystal settling and flotation in the lunar magma ocean. In the first paper, we develop a direct numerical method for resolving the hydrodynamic interactions between crystals and their feedback on the flow field in magmatic liquid. In this paper, we use this computational technique to test the leading model for the formation of the earliest crust on the Moon. The anorthositic lithology of the lunar crust is thought to have been formed by the flotation of buoyant plagioclase crystals at a time when the lunar mantle was still wholly or largely molten. This model is appealing from an observational point of view, but its fluid dynamical validity is not obvious, because (1) plagioclase probably started crystallizing very late (i.e., when the magma ocean was already 80% solidified) and (2) a significant portion of the shallow lunar crust consists of almost pure plagioclase (>90 vol. %), requiring very efficient plagioclase segregation. The goal of this study is to better understand the fluid dynamical conditions that hinder or facilitate crystal settling or flotation. Our approach complements earlier studies by explicitly linking the petrological and fluid dynamical evolution and by focusing on the effect of increasing crystal fraction. We find that crystal settling was probably possible throughout the entire solidification history of the lunar magma ocean as long as crystal sizes were sufficiently large (r>1 mm) and crystal fraction sufficiently low (<13%).
ASJC Scopus subject areas
- Geochemistry and Petrology
- Earth and Planetary Sciences (miscellaneous)
- Space and Planetary Science