Giant planet formation in radially structured protoplanetary discs
Open accessAbstract
Our recent N-body simulations of planetary system formation, incorporating models for the main physical processes thought to be important during the building of planets (i.e. gas disc evolution, migration, planetesimal/boulder accretion, gas accretion on to cores, etc.), have been successful in reproducing some of the broad features of the observed exoplanet population (e.g. compact systems of low-mass planets, hot Jupiters), but fail completely to form any surviving cold Jupiters. The primary reason for this failure is rapid inward migration of growing protoplanets during the gas accretion phase, resulting in the delivery of these bodies on to orbits close to the star. Here, we present the results of simulations that examine the formation of gas giant planets in protoplanetary discs that are radially structured due to spatial and temporal variations in the effective viscous stresses, and show that such a model results in the formation of a population of cold gas giants. Furthermore, when combined with models for disc photoevaporation and a central magnetospheric cavity, the simulations reproduce the well-known hot-Jupiter/cold-Jupiter dichotomy in the observed period distribution of giant exoplanets, with a period valley between 10 and 100 d.
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Disk migration can deliver hot Jupiters at the observed relative rate for plausible migration parameters.
“Disk migration ( § 2.2) can deliver hot Jupiters at the observed relative rate for plausible migration parameters.”
From Origins of Hot Jupiters (2018) · cites this paper as Coleman & Nelson (2016)
Section 3.2.1 (p. 11) says early-forming giants migrate inward and become hot Jupiters, and §2.2.2 (p. 3) says the modeled migration rates are in reasonable agreement with hydrodynamic calculations. But §3.3.1 (p. 12) says the simulated period distribution compares reasonably with observations while producing a higher fraction of hot Jupiters. The paper therefore supports delivery by plausible disk migration, but not an exact match to the observed relative rate. (LLM, conf=0.85)
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Cites
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Dawson, R. I., & Johnson, J. A. (2018) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081817-051853 · Cited by 622 · see citing works
- Authors
- Coleman, G. A. L., & Nelson, R. P.
- Affiliations
- Queen Mary University of London (GB)
- Corresponding author
- Coleman, Gavin A. L.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2016-05-17
- Volume
- 460
- Issue
- 3
- Pages
- 2779-2795
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2336088992
- Cited by
- 79
- References
- 3
- Citations by year
- 2026: 3 · 2025: 7 · 2024: 7 · 2023: 7 · 2022: 5 · 2021: 7 · 2020: 9 · 2019: 12 · 2018: 14 · 2017: 6 · 2016: 2
- FWCI
- 5.42
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- HighWire Press Open Archive (submittedVersion)
- Queen Mary Research Online (Queen Mary University of London) (submittedVersion)
- arXiv (Cornell University)
- Funders
- Engineering and Physical Sciences Research Council (EP/K000128/1, EP/K000233/1)
- Science and Technology Facilities Council (ST/M001202/1)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- giant planet formation, cold Jupiters, hot Jupiters, planet migration, gas accretion, planetesimal accretion, magnetospheric cavity, N-body simulations
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