The DOI matches its Crossref record; 42 of the 42 references it cites were found in a registry or an index.
THE TWO MODES OF GAS GIANT PLANET FORMATION
Open accessAbstract
I argue for two modes of gas giant planet formation and discuss the conditions under which each mode operates. Gas giant planets at disk radii r >100 AU are likely to form in situ by disk instability, while core accretion plus gas capture remains the dominant formation mechanism for r < 100 AU. During the mass accretion phase, mass loading can push disks toward fragmentation conditions at large r . Massive, extended disks can fragment into clumps of a few to tens of Jupiter masses. This is confirmed by radiation hydrodynamics simulations. The two modes of gas giant formation should lead to a bimodal distribution of gas giant semimajor axes. Because core accretion is expected to be less efficient in low-metallicity systems, the ratio of gas giants at large r to planets at small r should increase with decreasing metallicity.
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Cites
On the Gravitational Stability of a Disk of Stars
Toomre, A. (1964) · The Astrophysical Journal · doi:10.1086/147861 · Cited by 3,349 · cited 1×
“In order for gravitational instabilities (GIs) to form gas giants directly, the Toomre (1964) Q = csκ/πGΣ, where cs is the sound speed, κ is the epicyclic frequency, and Σ is the surface density, must approach unity and the local cooling time must be . the local orbit period (Gammie 2001; Rice et…”
BackgroundFormation of the Giant Planets by Concurrent Accretion of Solids and Gas
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Valenti, J. A., & Fischer, D. A. (2005) · The Astrophysical Journal Supplement Series · doi:10.1086/430500 · Cited by 1,460
Giant Planet Formation by Gravitational Instability
Boss, A. P. (1997) · Science · doi:10.1126/science.276.5320.1836 · Cited by 1,124 · cited 1×
“Both core accretion plus gas capture (e.g., Pollack et al. 1996) and direct formation by disk instability (Cameron 1978; Boss 1997) can form gas giant planets in principle.”
BackgroundNonlinear Outcome of Gravitational Instability in Cooling, Gaseous Disks
Gammie, C. F. (2001) · The Astrophysical Journal · doi:10.1086/320631 · Cited by 1,012
Truelove, J. K., Klein, R. I., McKee, C. F., Holliman II, J. H., Howell, L. H., & Greenough, J. A. (1997) · The Astrophysical Journal · doi:10.1086/310975 · Cited by 961
Using FU Orionis outbursts to constrain self-regulated protostellar disk models
Bell, K. R., & Lin, D. N. C. (1994) · The Astrophysical Journal · doi:10.1086/174206 · Cited by 881
Optical Images of an Exosolar Planet 25 Light-Years from Earth
Kalas, P., Graham, J. R., Chiang, E., Fitzgerald, M. P., Clampin, M., Kite, E. S., Stapelfeldt, K., Marois, C., & Krist, J. (2008) · Science · doi:10.1126/science.1166609 · Cited by 840
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Accretion Disks around Young Objects. III. Grain Growth
D’Alessio, P., Calvet, N., & Hartmann, L. (2001) · The Astrophysical Journal · doi:10.1086/320655 · Cited by 544
Cited by
Dynamics of Protoplanetary Disks
Armitage, P. J. (2011) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081710-102521 · Cited by 517
Caselli, P., & Ceccarelli, C. (2012) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-012-0056-x · Cited by 489
A torque formula for non-isothermal type I planetary migration - I. Unsaturated horseshoe drag
Paardekooper, S.-J., Baruteau, C., Crida, A., & Kley, W. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15782.x · Cited by 448
Perryman, M. (2018) · Cambridge University Press eBooks · doi:10.1017/9781108304160 · Cited by 340
LkCa 15: A YOUNG EXOPLANET CAUGHT AT FORMATION?
Kraus, A. L., & Ireland, M. J. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/745/1/5 · Cited by 320
Metadata
- Authors
- Boley, A. C.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2009-03-23
- Volume
- 695
- Issue
- 1
- Pages
- L53-L57
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2047276734
- Cited by
- 277
- References
- 42
- FWCI
- 16.62
- Type
- journal article
- Language
- en
- Open access
- bronze
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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).
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