A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion

Paardekooper, Sijme-Jan; Baruteau, Clément; Kley, W.

doi:10.1111/j.1365-2966.2010.17442.x

Cited by 504 publications

(955 citation statements)

References 33 publications

(74 reference statements)

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“…Since these first calculations, type I migration has been studied in great detail, and new formulations for type I migration rates are now available (Paardekooper et al 2010(Paardekooper et al , 2011. We use in our model an analytic description of type I migration that reproduces the results of Paardekooper et al (2011). A detailed description of this model is presented in Dittkrist et al (in prep.…”

Section: Orbital Evolution: Disc-planet Interactionmentioning

confidence: 99%

“…At ∼8 M ⊕ the protoplanet undergoes inward migration in the adiabatic saturated regime 5 (see Paardekooper et al 2010Paardekooper et al , 2011Mordasini et al 2010;Dittkrist et al). This timescale turns 5 The regime is called adiabatic when the local cooling timescale in the disc is longer than the time it takes for a parcel of gas to make a U-turn on the horseshoe orbit close to the planet in the corotation region.…”

Section: Planet Formation With Migrationmentioning

confidence: 99%

“…For low-mass planets, which are not massive enough to open a gap in the protoplanetary disc, migration occurs in type I (Ward 1997;Tanaka et al 2002;Paardekooper et al 2010Paardekooper et al , 2011. For higher mass planets, migration is again subdivided into two modes: disc-dominated type II migration, when the local disc mass is larger than the planetary mass (the migration rate is then simply given by the viscous evolution of the protoplanetary disc), and planet-dominated type II migration in the opposite case (see M09).…”

Section: Orbital Evolution: Disc-planet Interactionmentioning

confidence: 99%

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Planet formation models: the interplay with the planetesimal disc

Fortier

Alibert

Carron

et al. 2012

A&A

124

196

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Context. According to the sequential accretion model (or core-nucleated accretion model), giant planet formation is based first on the formation of a solid core which, when massive enough, can gravitationally bind gas from the nebula to form the envelope. The most critical part of the model is the formation time of the core: to trigger the accretion of gas, the core has to grow up to several Earth masses before the gas component of the protoplanetary disc dissipates. Aims. We calculate planetary formation models including a detailed description of the dynamics of the planetesimal disc, taking into account both gas drag and excitation of forming planets. Methods. We computed the formation of planets, considering the oligarchic regime for the growth of the solid core. Embryos growing in the disc stir their neighbour planetesimals, exciting their relative velocities, which makes accretion more difficult. Here we introduce a more realistic treatment for the evolution of planetesimals' relative velocities, which directly impact on the formation timescale. For this, we computed the excitation state of planetesimals, as a result of stirring by forming planets, and gas-solid interactions. Results. We find that the formation of giant planets is favoured by the accretion of small planetesimals, as their random velocities are more easily damped by the gas drag of the nebula. Moreover, the capture radius of a protoplanet with a (tiny) envelope is also larger for small planetesimals. However, planets migrate as a result of disc-planet angular momentum exchange, with important consequences for their survival: due to the slow growth of a protoplanet in the oligarchic regime, rapid inward type I migration has important implications on intermediate-mass planets that have not yet started their runaway accretion phase of gas. Most of these planets are lost in the central star. Surviving planets have masses either below 10 M ⊕ or above several Jupiter masses. Conclusions. To form giant planets before the dissipation of the disc, small planetesimals (∼0.1 km) have to be the major contributors of the solid accretion process. However, the combination of oligarchic growth and fast inward migration leads to the absence of intermediate-mass planets. Other processes must therefore be at work to explain the population of extrasolar planets that are presently known.

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Section: Orbital Evolution: Disc-planet Interactionmentioning

confidence: 99%

Section: Planet Formation With Migrationmentioning

confidence: 99%

Section: Orbital Evolution: Disc-planet Interactionmentioning

confidence: 99%

See 1 more Smart Citation

Planet formation models: the interplay with the planetesimal disc

Fortier

Alibert

Carron

et al. 2012

A&A

124

196

View full text Add to dashboard Cite

show abstract

“…In this scenario, the solid core of the planet needs to form and initiate gas accretion at quite large radius from the star. This may occur if planetary cores can migrate outward because of the strong influence of corotation torques, as considered by [39] and [20]. Rapid gas accretion leading to a gap-opening planet is likely to require the formation of a massive core out at 15 au.…”

Section: Scenariomentioning

confidence: 99%

The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

2014

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Over the last twenty years, the search for extrasolar planets has revealed the rich diversity of outcomes from the formation and evolution of planetary systems. In order to fully understand how these extrasolar planets came to be, however, the orbital and physical data we possess are not enough, and they need to be complemented with information about the composition of the exoplanets. Ground-based and space-based observations provided the first data on the atmospheric composition of a few extrasolar planets, but a larger and more detailed sample is required before we can fully take advantage of it. The primary goal of a dedicated space mission like the Exoplanet Characterization Observatory (EChO) proposal is to fill this gap and to expand the limited data we possess by performing a systematic survey of extrasolar planets. The full exploitation of the data that space-based and ground-based facilities will provide in the near future, however, requires knowledge about the sources and sinks of the chemical species and molecules that will be observed. Luckily, the study of the past history of the Solar System provides several indications about the effects of processes like migration, late accretion and secular impacts, and on the time they occur in the life of planetary systems. In this work we will review what is

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“…However, Rein (2012) has assumed that the smooth migration is always inward, which is only true for classic type I (and type II) migration. Recent improvements in the analysis of the corotation and horseshoe torques (plus the differential Linblad torque) have shown that type I migration can be outward in some regions of certain disk models, and that there are locations in the disk where the total torque vanishes and the migration is stalled (e.g., Paardekooper et al 2011;Kretke & Lin 2012). This more complex migration behavior means that it is possible for a pair of planets to undergo both convergent and divergent migration, as the disk accretion rate decreases with time and the disk depletes.…”

Section: Discussionmentioning

confidence: 99%

Evidence for Solid Planets from Kepler's Near-Resonance Systems

2012

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Abstract. The multiple-planet systems discovered by the Kepler mission show an excess of planet pairs with period ratios just wide of exact commensurability for first-order resonances like 2:1 and 3:2. In principle, these planet pairs could be in resonance if their orbital eccentricities are sufficiently small, because the width of first-order resonances diverges in the limit of vanishingly small eccentricity. We consider a widely-held scenario in which pairs of planets were captured into first-order resonances by migration due to planet-disk interactions, and subsequently became detached from the resonances, due to tidal dissipation in the planets. In the context of this scenario, we find a constraint on the ratio of the planet's tidal dissipation function and Love number that implies that some of the Kepler planets are likely solid. However, tides are not strong enough to move many of the planet pairs to the observed separations, suggesting that additional processes are at play.

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A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion

Cited by 504 publications

References 33 publications

Planet formation models: the interplay with the planetesimal disc

Planet formation models: the interplay with the planetesimal disc

The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

Evidence for Solid Planets from Kepler's Near-Resonance Systems

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