Formation of the Giant Planets

Mizuno, Hiroshi

doi:10.1143/ptp.64.544

Cited by 749 publications

(355 citation statements)

References 9 publications

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“…core nucleated accretion) of giant planet formation (Mizuno, 1980;Bodenheimer & Pollack, 1986;Pollack et al, 1996) involves the formation of a giant planet by capture of nebula gas by a solid core. These stages are as follows (Bodenheimer et al, 2000):…”

Section: Core Accretion-gas Capture Modelmentioning

confidence: 99%

Young Jupiters are faint: new models of the early evolution of giant planets

Fortney¹,

Marley

Hubickyj

et al. 2005

Astron Nachr

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Abstract.Here we show preliminary calculations of the cooling and contraction of a 2 MJ planet. These calculations, which are being extended to 1-10 MJ, differ from other published "cooling tracks" in that they include a core accretion-gas capture formation scenario, the leading theory for the formation of gas giant planets. We find that the initial post-accretionary intrinsic luminosity of the planet is ∼3 times less than previously published models which use arbitrary initial conditions. These differences last a few tens of millions of years. Young giant planets are intrinsically fainter than has been previously appreciated. We also discuss how uncertainties in atmospheric chemistry and the duration of the formation time of giant planets lead to challenges in deriving planetary physical properties from comparison with tabulated model values.

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Section: Core Accretion-gas Capture Modelmentioning

confidence: 99%

Young Jupiters are faint: new models of the early evolution of giant planets

Fortney¹,

Marley

Hubickyj

et al. 2005

Astron Nachr

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“…A massive gas atmosphere builds up around the rocky core if it reaches a critical mass of about 10 M ⊕ (e.g., Mizuno 1980). The CA model's main theoretical difficulty is in the very beginning of the growth: it is not clear how metresized rocks would stick together while colliding at high speeds, subject to high radial drifts into the parent star (Weidenschilling 1977(Weidenschilling , 1980, although gas-dust dynamical instabilities are suggested to help (e.g., Youdin & Goodman 2005;Johansen et al 2007).…”

Section: Introductionmentioning

confidence: 99%

A new view on planet formation

Nayakshin¹

2010

Proc. IAU

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Abstract. The standard picture of planet formation posits that giant gas planets are over-grown rocky planets massive enough to attract enormous gas atmospheres. It has been shown recently that the opposite point of view is physically plausible: the rocky terrestrial planets are former giant planet embryos dried of their gas "to the bone" by the influences of the parent star. Here we provide a brief overview of this "Tidal Downsizing" hypothesis in the context of the Solar System structure.

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“…At first glance, this seems like an extraordinarily high critical core mass compared to the canonical value of 10 M ⊕ derived by Mizuno (1980) and the 15 M ⊕ quoted by Papaloizou & Nelson (2005). However, critical core mass is really a function of orbital radius and solid/ gas ratio.…”

Section: Simulation Results and Discussionmentioning

confidence: 64%

DISCOVERING THE GROWTH HISTORIES OF EXOPLANETS: THE SATURN ANALOG HD 149026b

Dodson-Robinson

Bodenheimer

2009

ApJ

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The transiting "hot Saturn" HD 149026b, which has the highest mean density of any confirmed planet in the NeptuneJupiter mass range, has challenged theories of planet formation since its discovery in 2005. Previous investigations could not explain the origin of the planet's 45-110 Earth-mass solid core without invoking catastrophes such as gas giant collisions or heavy planetesimal bombardment launched by neighboring planets. Here we show that HD 149026b's large core can be successfully explained by the standard core accretion theory of planet formation. The keys to our reconstruction of HD 149026b are (1) applying a model of the solar nebula to describe the protoplanet nursery, (2) placing the planet initially on a long-period orbit at Saturn's heliocentric distance of 9.5 AU, and (3) adjusting the solid mass in the HD 149026 disk to twice that of the solar nebula in accordance with the star's heavy element enrichment. We show that the planet's migration into its current orbit at 0.042 AU is consistent with our formation model. Our study of HD 149026b demonstrates that it is possible to discover the growth history of any planet with a well-defined core mass that orbits a solar-type star.

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Formation of the Giant Planets

Cited by 749 publications

References 9 publications

Young Jupiters are faint: new models of the early evolution of giant planets

Young Jupiters are faint: new models of the early evolution of giant planets

A new view on planet formation

DISCOVERING THE GROWTH HISTORIES OF EXOPLANETS: THE SATURN ANALOG HD 149026b

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