| Issue |
A&A
Volume 668, December 2022
|
|
|---|---|---|
| Article Number | A170 | |
| Number of page(s) | 15 | |
| Section | Planets and planetary systems | |
| DOI | https://doi.org/10.1051/0004-6361/202244864 | |
| Published online | 21 December 2022 | |
Rapid formation of massive planetary cores in a pressure bump
1
University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München,
Scheinerstr. 1,
81679
Munich, Germany
e-mail: ch.lau@physik.uni-muenchen.de
2
Max Planck Institute for Solar System Research,
Justus-von-Liebig-Weg 3,
37077
Göttingen, Germany
3
Exzellenzcluster ORIGINS,
Boltzmannstr. 2,
85748
Garching, Germany
4
Institut für Theoretische Astrophysik, Zentrum für Astronomie, Heidelberg University,
Albert Ueberle Str. 2,
69120
Heidelberg, Germany
Received:
1
September
2022
Accepted:
8
November
2022
Context. Models of planetary core growth by either planetesimal or pebble accretion are traditionally disconnected from the models of dust evolution and formation of the first gravitationally bound planetesimals. State-of-the-art models typically start with massive planetary cores already present.
Aims. We aim to study the formation and growth of planetary cores in a pressure bump, motivated by the annular structures observed in protoplanetary disks, starting with submicron-sized dust grains.
Methods. We connect the models of dust coagulation and drift, planetesimal formation in the streaming instability, gravitational interactions between planetesimals, pebble accretion, and planet migration into one uniform framework.
Results. We find that planetesimals forming early at the massive end of the size distribution grow quickly, predominantly by pebble accretion. These few massive bodies grow on timescales of ~100 000 yr and stir the planetesimals that form later, preventing the emergence of further planetary cores. Additionally, a migration trap occurs, allowing for retention of the growing cores.
Conclusions. Pressure bumps are favourable locations for the emergence and rapid growth of planetary cores by pebble accretion as the dust density and grain size are increased and the pebble accretion onset mass is reduced compared to a smooth-disc model.
Key words: accretion, accretion disks / planets and satellites: formation / protoplanetary disks / methods: numerical
© Tommy Chi Ho Lau et al. 2022
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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