Habitable Zones & Global Climate

Water Partitioning in Planetary Embryos and Protoplanets with Magma Oceans

By Keith Cowing
Press Release
April 25, 2018
Filed under
Water Partitioning in Planetary Embryos and Protoplanets with Magma Oceans
Protoplanet with Magma Oceans

The water content of magma oceans is widely accepted as a key factor that determines whether a terrestrial planet is habitable. Water ocean mass is determined as a result not only of water delivery and loss, but also of water partitioning among several reservoirs.

Here we review our current understanding of water partitioning among the atmosphere, magma ocean, and solid mantle of accreting planetary embryos and protoplanets just after giant collisions. Magma oceans are readily formed in planetary embryos and protoplanets in their accretion phase. Significant amounts of water are partitioned into magma oceans, provided the planetary building blocks are water-rich enough. Particularly important but still quite uncertain issues are how much water the planetary building blocks contain initially and how water goes out of the solidifying mantle and is finally degassed to the atmosphere. Constraints from both solar-system explorations and exoplanet observations and also from laboratory experiments are needed to resolve these issues.

Masahiro Ikoma, Linda Elkins-Tanton, Keiko Hamano, Jenny Suckale
(Submitted on 24 Apr 2018)

Comments: Accepted for publication in Space Science Reviews
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:1804.09294 [astro-ph.EP] (or arXiv:1804.09294v1 [astro-ph.EP] for this version)
Submission history
From: Masahiro Ikoma
[v1] Tue, 24 Apr 2018 23:37:15 GMT (2607kb)

Explorers Club Fellow, ex-NASA Space Station Payload manager/space biologist, Away Teams, Journalist, Lapsed climber, Synaesthete, Na’Vi-Jedi-Freman-Buddhist-mix, ASL, Devon Island and Everest Base Camp veteran, (he/him) πŸ––πŸ»