Dry or water world? How the water contents of inner sub-Neptunes constrain giant planet formation and the location of the water ice line

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Volume 649 (May 2021)

A&A, 649 (2021) L5

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Table 1.

Predictions of the water content of sub-Neptunes from our model if the system formed via scenario A or scenario B (Fig. 1) and depending on the α value for the ice line position (always using Σ_g = 1000 g cm⁻²).

Name	α = 0.01	α = 0.001	α = 10⁻⁴
K-68b	Wet	Wet	Dry
K-48b	Wet	Wet	Dry
K-48c	Wet	Wet	Dry
K-48d	Wet	Wet	Dry
K-94b	Wet	Wet	Dry
π-Men-c	Wet	Dry	Dry
WASP-47d	Wet	Wet	Dry
K-454b	Wet	Wet	Dry
K-289b	Wet	Wet	Wet
K-289c	Wet	Wet	Wet
HD-86226c	Wet	Dry	Dry
HAT-P-11b	Wet	Dry	Dry
K-88b	Wet	Dry	Dry

Notes. We only list the planets that have a mean density lower than pure rock (Fig. 2). The exact water content of the inner planet then depends on if the sub-Neptune is formed via scenario B or C (see Appendix B). Bold values mark the most interesting results that could be found observationally.

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