Journal ArticleDOI
Calculations of the accretion and evolution of giant planets: The effects of solid cores
TLDR
In this paper, the evolution of the giant planets is calculated under the general hypothesis that the solid cores formed first, by accretion of small particles, and that these cores later gravitationally attracted their gaseous envelopes from the solar nebula.About:
This article is published in Icarus.The article was published on 1986-09-01. It has received 503 citations till now. The article focuses on the topics: Planetary core & Accretion (astrophysics).read more
Citations
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Journal ArticleDOI
Formation of the Giant Planets by Concurrent Accretion of Solids and Gas
James B. Pollack,Olenka Hubickyj,Peter Bodenheimer,Jack J. Lissauer,Morris Podolak,Yuval Greenzweig +5 more
TL;DR: In this article, the authors presented a self-consistent, interactive simulation of the formation of the giant planets, in which for the first time both the gas and planetesimal accretion rates were calculated in a selfconsistent and interactive fashion.
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Orbital migration of the planetary companion of 51 Pegasi to its present location
TL;DR: In this paper, the authors show that if the companion is indeed a gas-giant planet, it is extremely unlikely to have formed at its present location, and suggest instead that the planet probably formed by gradual accretion of solids and capture of gas at a much larger distance from the star (∼5 AU), and that it subsequently migrated inwards through interactions with the remnants of the circumstellar disk.
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Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets
Shigeru Ida,D. N. C. Lin +1 more
TL;DR: In this article, the authors examine the accretion of cores of giant planets from planetesimals, gas accretion onto the cores, and their orbital migration and show that the mass and semimajor axis distributions generated in their simulations for the gas giants are consistent with those of the known extrasolar planets.
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Models of giant planet formation with migration and disc evolution
TL;DR: In this article, the authors 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.
References
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Journal ArticleDOI
Formation of the Giant Planets
TL;DR: In this paper, the structure of a gaseous envelope surrounding a protoplanet has been investigated in connection with the formation of the giant planets, and the most remarkable result is that a common relation between the core mass and the total mass holds irrespectively of the regions in the solar nebula.
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Tidal torques on accretion discs in binary systems with extreme mass ratios.
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Timescales for planetary accretion and the structure of the protoplanetary disk
TL;DR: In this article, a self-consistent scenario for all stages of planetary accretion which satisfies observational constraints is proposed. But it is not a selfconsistent model for all phases of planetary formation.
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Some dynamical aspects of the accretion of Uranus and Neptune: The exchange of orbital angular momentum with planetesimals
J.A. Fernández,Wing-Huen Ip +1 more
TL;DR: In this paper, the final stage of the accretion of Uranus and Neptune is numerically investigated and two possible effects that may have contributed to the formation of the two outer Jovian planets are incorporated in the model.
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Physics of the Primitive Solar Accretion Disk
TL;DR: The theory of viscous accretion disks developed by Lynden-Bell and Pringle (1974) has been applied to the evolution of the primitive solar nebula as mentioned in this paper, and it was concluded that the late stages of evolution would be dominated by the effects of mass loss from the expansion of a hot disk corona into space.