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The water content of magma oceans is widely accepted as a key factor thatdetermines whether a terrestrial planet is habitable. Water ocean mass isdetermined as a result not only of water delivery and loss, but also of waterpartitioning among several reservoirs. Here we review our current understandingof water partitioning among the atmosphere, magma ocean, and solid mantle ofaccreting planetary embryos and protoplanets just after giant collisions. Magmaoceans are readily formed in planetary embryos and protoplanets in theiraccretion phase. Significant amounts of water are partitioned into magmaoceans, provided the planetary building blocks are water-rich enough.Particularly important but still quite uncertain issues are how much water theplanetary building blocks contain initially and how water goes out of thesolidifying mantle and is finally degassed to the atmosphere. Constraints fromboth solar-system explorations and exoplanet observations and also fromlaboratory experiments are needed to resolve these issues.

Water Partitioning in Planetary Embryos and Protoplanets with Magma Oceans