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Can Giant Planets Form by Direct Gravitational Instability?
Open accessAbstract
Gravitational instability has been invoked as a possible mechanism of the giant planet production in protoplanetary disks. Here we critically revise its viability by noting that to form planets directly, it is not enough for protoplanetary disks to be gravitationally unstable. They must also be able to cool efficiently (on a timescale comparable to the local disk orbital period) to allow the formation of the bound clumps by fragmentation. A combination of the dynamical and thermal constraints puts very stringent lower limits on the properties of disks capable of fragmenting into the self-gravitating objects: for the gravitational instability to form giant planets at 10 AU in the disk cooled by the radiation transfer, the gas temperature must exceed 10 3 K with a minimum disk mass of 0.7 M ☉ and a luminosity of 40 L ☉ . Although these requirements are relaxed in the more distant parts of the disk, masses of the bound objects formed as a result of instability are too large even at 100 AU (~10 M J ) to explain the characteristics of known extrasolar giant planets. Such protoplanetary disks (and planets formed in them) have very unusual observational properties, and this severely constrains the possibility of giant planet formation by direct gravitational instability.
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“More importantly, even if the gas were dense enough for disk fragmentation, at short orbital periods fragments would shear out before they could cool and contract.”
From Origins of Hot Jupiters (2018) · cites this paper as Rafikov 2005
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“As argued by Rafikov (2005), such high temperatures would unbind the gas from the star. Therefore we do not expect the conditions for gravitational instability close to the star.”
From Origins of Hot Jupiters (2018) · cites this paper as Rafikov 2005
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Cites
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Cited by
Sorted by citations
McKee, C., & Ostriker, E. (2007) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.45.051806.110602 · Cited by 1,826
Direct Imaging of Multiple Planets Orbiting the Star HR 8799
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Rapid growth of gas-giant cores by pebble accretion
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Gravitational Instabilities in Circumstellar Disks
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Metadata
- Authors
- Rafikov, R. R.
- Corresponding author
- Rafikov, Roman R.
- ORCID
- Rafikov, Roman R.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2005-01-31
- Volume
- 621
- Issue
- 1
- Pages
- L69-L72
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2064514018
- Cited by
- 433
- References
- 20
- Citations by year
- 2026: 11 · 2025: 17 · 2024: 10 · 2023: 8 · 2022: 12 · 2021: 19 · 2020: 17 · 2019: 22 · 2018: 44 · 2017: 15 · 2016: 39 · 2015: 17 · 2014: 14 · 2013: 19 · 2012: 26
- FWCI
- 10.85
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- giant planet formation, gravitational instability, protoplanetary disks, disk fragmentation, disk cooling, extrasolar giant planets, gas temperature
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