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  Rocky super-Earths or waterworlds: the interplay of planet migration, pebble accretion, and disc evolution

Bitsch, B., Raymond, S. N., & Izidoro, A. (2019). Rocky super-Earths or waterworlds: the interplay of planet migration, pebble accretion, and disc evolution. Astronomy and Astrophysics, 624.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-D411-8 Version Permalink: http://hdl.handle.net/21.11116/0000-0005-D412-7
Genre: Journal Article

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 Creators:
Bitsch, Bertram1, Author
Raymond, Sean N.1, Author
Izidoro, Andre1, Author
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1Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners, ou_2421692              

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Free keywords: accretion accretion disks planets and satellites: formation planets and satellites: composition planet-disk interactions Astrophysics - Earth and Planetary Astrophysics
 Abstract: Recent observations have found a valley in the size distribution of close-in super-Earths that is interpreted as a signpost that close-in super-Earths are mostly rocky in composition. However, new models predict that planetesimals should first form at the water ice line such that close-in planets are expected to have a significant water ice component. Here we investigate the water contents of super-Earths by studying the interplay between pebble accretion, planet migration and disc evolution. Planets' compositions are determined by their position relative to different condensation fronts (ice lines) throughout their growth. Migration plays a key role. Assuming that planetesimals start at or exterior to the water ice line (r > rH2O), inward migration causes planets to leave the source region of icy pebbles and therefore to have lower final water contents than in discs with either outward migration or no migration. The water ice line itself moves inward as the disc evolves, and delivers water as it sweeps across planets that formed dry. The relative speed and direction of planet migration and inward drift of the water ice line is thus central in determining planets' water contents. If planet formation starts at the water ice line, this implies that hot close-in super-Earths (r < 0.3 AU) with water contents of a few percent are a signpost of inward planet migration during the early gas phase. Hot super-Earths with larger water ice contents on the other hand, experienced outward migration at the water ice line and only migrated inwards after their formation was complete either because they become too massive to be contained in the region of outward migration or in chains of resonant planets. Measuring the water ice content of hot super-Earths may thus constrain their migration history.

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 Dates: 2019
 Publication Status: Published in print
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Title: Astronomy and Astrophysics
Source Genre: Journal
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Pages: - Volume / Issue: 624 Sequence Number: - Start / End Page: - Identifier: -