The DOI matches its Crossref record; 1 of the 1 references it cites were found in a registry or an index.
Giant Planet Formation by Gravitational Instability
Abstract
The recent discoveries of extrasolar giant planets, coupled with refined models of the compositions of Jupiter and Saturn, prompt a reexamination of theories of giant planet formation. An alternative to the favored core accretion hypothesis is examined here; gravitational instability in the outer solar nebula leading to giant planet formation. Three-dimensional hydrodynamic calculations of protoplanetary disks show that giant gaseous protoplanets can form with locally isothermal or adiabatic disk thermodynamics. Gravitational instability appears to be capable of forming giant planets with modest cores of ice and rock faster than the core accretion mechanism can.
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“An alternative planet formation model that has been hypothesized is that of gravitational instability (Zel'Dovich, 1970; Boss, 1997).”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Boss, 1997
Citations
Cites
A Jupiter-mass companion to a solar-type star
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Flagged first, then by citations
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Cited by
Sorted by citations
Direct Imaging of Multiple Planets Orbiting the Star HR 8799
Marois, C., Macintosh, B., Barman, T., Zuckerman, B., Song, I., Patience, J. L., Lafreniére, D., & Doyon, R. (2008) · Science · doi:10.1126/science.1166585 · Cited by 1,711
Rapid planetesimal formation in turbulent circumstellar disks
Johansen, A., Oishi, J., Low, M.-M. M., Klahr, H., Henning, T., & Youdin, A. (2007) · Nature · doi:10.1038/nature06086 · Cited by 991
Rauer, H., Catala, C., Aerts, C., Appourchaux, T. P., Benz, W., Brandeker, A., Christensen-Dalsgaard, J., Deleuil, M., Gizon, L., Goupil, M. J., et al. (2014) · Experimental Astronomy · doi:10.1007/s10686-014-9383-4 · Cited by 1,390
Nonlinear Outcome of Gravitational Instability in Cooling, Gaseous Disks
Gammie, C. (2001) · The Astrophysical Journal · doi:10.1086/320631 · Cited by 828
“Numerical experiments with fluid disks often assume a fixed temperature profile or a fixed entropy profile (Boss 1997, 1998; Nelson et al. 1998).”
BackgroundThe Occurrence and Architecture of Exoplanetary Systems
Winn, J. N., & Fabrycky, D. C. (2015) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082214-122246 · Cited by 926
“The only other theory that is occasionally discussed is gravitational instability, in which the gaseous disk collapses directly into giant planets (Boss 1997).”
Background
Metadata
- Authors
- Boss, A. P.
- Affiliations
- Carnegie Institution for Science (US)
- Corresponding author
- Boss, Alan P.
- ORCID
- Boss, Alan P.
- Venue
- Science
- Published
- 1997-06-20
- Volume
- 276
- Issue
- 5320
- Pages
- 1836-1839
- ISSN
- 0036-8075 (ISSN-L)
- 1095-9203
- OpenAlex
- W2084110269
- Cited by
- 1,124
- References
- 0
- Citations by year
- 2026: 44 · 2025: 61 · 2024: 79 · 2023: 49 · 2022: 51 · 2021: 59 · 2020: 63 · 2019: 41 · 2018: 36 · 2017: 39 · 2016: 60 · 2015: 37 · 2014: 40 · 2013: 44 · 2012: 40
- FWCI
- 13.33
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Science (publishedVersion)
- 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, gravitational instability, core accretion, protoplanetary disks, exoplanets, Jupiter, Saturn, isothermal disk, three-dimensional fluid dynamics, ice cores
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