Models of giant planet formation with migration and disc evolution

Alibert, Y.; Mordasini, C.; Benz, W.; Winisdoerffer, C.

doi:10.1051/0004-6361:20042032

Cited by 685Astro and Planetary ScienceAstrophysics and Star Formation StudiesStellar, planetary, and galactic studies

The DOI matches its Crossref record; 52 of the 52 references it cites were found in a registry or an index.

Models of giant planet formation with migration and disc evolution

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Alibert, Y., Mordasini, C., Benz, W., Winisdoerffer, C.·2005·Astronomy & Astrophysics

DOI 10.1051/0004-6361:20042032

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Abstract

We present a new model of giant planet formation that extends the core-accretion model of Pollack et al. (1996, Icarus, 124, 62) to include migration, disc evolution and gap formation. We show that taking these effects into account can lead to much more rapid formation of giant planets, making it compatible with the typical disc lifetimes inferred from observations of young circumstellar discs. This speed up is due to the fact that migration prevents the severe depletion of the feeding zone as observed in in situ calculations. Hence, the growing planet is never isolated and it can reach cross-over mass on a much shorter timescale. To illustrate the range of planets that can form in our model, we describe a set of simulations in which we have varied some of the initial parameters and compare the final masses and semi-major axes with those inferred from observed extra-solar planets.

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A hot Jupiter that underwent disk migration may have an intermediate composition if it accreted gas along the way.
“A hot Jupiter that underwent disk migration may have an intermediate composition if it accreted gas along the way (e.g., Alibert et al. 2005).”
From Origins of Hot Jupiters (2018) · cites this paper as Alibert et al. 2005
The Introduction links close-in giant planets to inward disk migration, and §3.2 models a migrating giant that accretes both gas and planetesimals, with its heavy-element content depending partly on the accreted gas. But that illustrated planet ends at about 2.5 AU, not in a hot-Jupiter orbit, and the paper does not describe its composition as intermediate. (LLM, conf=0.82)
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Authors: Alibert, Y., Mordasini, C., Benz, W., & Winisdoerffer, C.
Affiliations: University of Bern (CH)
University of Leicester (GB)
ORCID: Alibert, Y.
Mordasini, C.
Benz, W.
Venue: Astronomy & Astrophysics
Publisher: EDP Sciences
Published: 2005-04
Volume: 434
Issue: 1
Pages: 343-353
ISSN: 0004-6361 (ISSN-L)
1432-0746
DOI: 10.1051/0004-6361:20042032
OpenAlex: W2134475956
Cited by: 685
References: 52
Citations by year: 2026: 20 · 2025: 19 · 2024: 23 · 2023: 20 · 2022: 27 · 2021: 32 · 2020: 37 · 2019: 38 · 2018: 36 · 2017: 34 · 2016: 34 · 2015: 30 · 2014: 37 · 2013: 26 · 2012: 39
FWCI: 23.64
Type: journal article
Language: en
Open access: bronze
doi.org
Locations: Astronomy and Astrophysics (publishedVersion)
arXiv (Cornell University) (submittedVersion)
Springer Link (Chiba Institute of Technology) (submittedVersion)
Bern Open Repository and Information System (University of Bern) (submittedVersion)
CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
arXiv (Cornell University)
Funders: National Science Foundation
Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung
Topics: Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Keywords: giant planet formation, core accretion, planet migration, protoplanetary disc evolution, gap formation, disc lifetime, semi-major axis, exoplanets, planetary mass

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Models of giant planet formation with migration and disc evolution

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