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Water Partitioning in Planetary Embryos and Protoplanets with Magma Oceans

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Masahiro Ikoma, Linda Elkins-Tanton, Keiko Hamano, Jenny Suckale

Earth and Planetary Astrophysics · Submitted 24 Apr 2018

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim Significant amounts of water are partitioned into magma oceans, provided the planetary building blocks are water-rich enough.

how it is stated · asserted 0.61 read the record →

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arXiv ID1804.09294 (version 1)
Pith IDVTDJSQJK, Pith's permanent record of this paper and its review
CitationJenny Suckale, Keiko Hamano, Linda Elkins-Tanton, Masahiro Ikoma. "Water Partitioning in Planetary Embryos and Protoplanets with Magma Oceans." arXiv:1804.09294 (2018). https://pith.science/paper/VTDJSQJK
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The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,571 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.52 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.03 · compares with prior results 0.06 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

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.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 The water content of magma oceans is widely accepted as a key factor that determines whether a terrestrial planet is habitable. background 1.00 0.03 0.05 asserted 1.00
s1 Water ocean mass is determined as a result not only of water delivery and loss, but also of water partitioning among several reservoirs. background 1.00 0.08 0.10 asserted 1.00
s2 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. contribution 0.99 0.17 0.09 asserted 0.70
s3 Magma oceans are readily formed in planetary embryos and protoplanets in their accretion phase. background 1.00 0.07 0.04 asserted 0.95
s4 Significant amounts of water are partitioned into magma oceans, provided the planetary building blocks are water-rich enough. result 0.61 0.13 0.19 asserted 0.61
s5 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. gap 0.98 0.06 0.12 asserted 0.69
s6 Constraints from both solar-system explorations and exoplanet observations and also from laboratory experiments are needed to resolve these issues. future work 0.99 0.04 0.10 asserted 0.96

What kind of paper the classifier reports this is: review 1.00 · evidence from literature 0.99.

What was examined, and what was not

sources read
  • arXiv listing abstract v1
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

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.

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