Halting Planet Migration in the Evacuated Centers of Protoplanetary Disks

Kuchner, Marc J.; Lecar, M.

doi:10.1086/342370

Cited by 55 publications

(69 citation statements)

References 38 publications

(48 reference statements)

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“…They found that all bodies migrated until reaching a point slightly exterior to the cavity edge, where they were effectively trapped in a stable configuration in almost circular orbits. Although this result appears different from that predicted by Kuchner & Lecar (2002), each is valid, as we shall see, for a different range of planetary masses.…”

Section: Introductioncontrasting

confidence: 96%

“…Since it is unclear whether in-situ formation occurs, the current orbital and physical characteristics of these planets provide important constraints on their past evolution and formation process. Several mechanisms have been proposed to explain the pile-up of hot planets with a three-day orbital period, including a truncation of the gaseous disk by the star (Lin et al 1996;Kuchner & Lecar 2002), planetary scattering combined with Kozai resonance and tidal circularization (Nagasawa et al 2008), planetary evaporation (Davis & Wheatly 2009), and tidal interactions with the parent star (Jackson et al 2009). …”

Section: Introductionmentioning

confidence: 99%

“…In particular, Kuchner & Lecar (2002) suggested that a giant planet in circular orbit could halt its migration when its orbital period was half that of the inner edge of the disk. In this configuration, all the planet's circular Lindblad resonances would lie in the inner cavity (IC) and no further interchange of angular momentum would take place.…”

Section: Introductionmentioning

confidence: 99%

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The mass-period distribution of close-in exoplanets

Benítez-Llambay

Masset

Beaugé

2011

A&A

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Context. The lower limit to the distribution of orbital periods P for the current population of close-in exoplanets shows a distinctive discontinuity located at approximately one Jovian mass. Most smaller planets have orbital periods longer than P ∼ 2.5 days, while higher masses are found down to P ∼ 1 day. Aims. We analyze whether this observed mass-period distribution could be explained in terms of the combined effects of stellar tides and the interactions of planets with an inner cavity in the gaseous disk. Methods. We performed a series of hydrodynamical simulations of the evolution of single-planet systems in a gaseous disk with an inner cavity mimicking the inner boundary of the disk. The subsequent tidal evolution is analyzed assuming that orbital eccentricities are small and stellar tides are dominant. Results. We find that most of the close-in exoplanet population is consistent with an inner edge of the protoplanetary disk being located at approximately P > ∼ 2 days for solar-type stars, in addition to orbital decay having been caused by stellar tides with a specific tidal parameter on the order of Q * 10 7 . The data is broadly consistent with planets more massive than one Jupiter mass undergoing type II migration, crossing the gap, and finally halting at the interior 2/1 mean-motion resonance with the disk edge. Smaller planets do not open a gap in the disk and remain trapped in the cavity edge. CoRoT-7b appears detached from the remaining exoplanet population, apparently requiring additional evolutionary effects to explain its current mass and semimajor axis.

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Section: Introductioncontrasting

confidence: 96%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The mass-period distribution of close-in exoplanets

Benítez-Llambay

Masset

Beaugé

2011

A&A

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“…Some effects that may be influencing the observed sizes include additional sources of luminosity (Hillenbrand et al 1992;Hartmann et al 1993), photoevaporation (Hollenbach et al 1994;Danchi et al 2001), turbulent accretion (Kuchner & Lecar 2002), or more complicated emission morphology (scattered light, viewing angles, disk plus envelope combinations, etc. ; Miroshnichenko et al 1999).…”

Section: Other Important Effectsmentioning

confidence: 99%

On the Interferometric Sizes of Young Stellar Objects

Monnier

Millan-Gabet

2002

ApJ

228

240

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Long-baseline optical interferometers can now detect and resolve hot dust emission thought to arise at the inner edge of circumstellar disks around young stellar objects (YSOs). We argue that the near-infrared sizes being measured are closely related to the radius at which dust is sublimated by the stellar radiation field. We consider how realistic dust optical properties and gas opacity dramatically affect the predicted location of this dust destruction radius, an exercise routinely done in other contexts but so far neglected in the analysis of near-infrared sizes of YSOs. We also present the accumulated literature of near-infrared YSO sizes in the form of a size-luminosity diagram and compare with theoretical expectations. We find evidence that large (e1.0 lm) dust grains predominate in the inner disks of T Tauri and Herbig Ae/Be stars, under the assumption that the innermost gaseous disks are optically thin at visible wavelengths.

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“…The inward migration of a planet could be stopped near the star as a result of tidal interaction with the host star, or through the evacuation of the inner disk by some processes such as interactions with stellar magnetosphere (Lin, Bodenheimer & Richardson 1996), magnetorotational instability (Kuchner & Lecar 2002), photoevaporation by irradiation from the central star (Matsuyama, Johnstone and Murray 2003), etc. The negligible Planet system dynamics 33 eccentricity of all extra-solar planets with periods less than 6 days can be accounted for by tidal dissipation induced by their host stars.…”

Section: Problems On Planet Migrationmentioning

confidence: 99%

Dynamical evolution of extrasolar planetary systems

Zhou

Sun

2004

Proc. IAU

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Abstract. To date, more than 130 extrasolar planets around main sequence stars are revealed mainly by the Doppler radial velocity measurements. Due to the observational biases, most of the detected planets are moving in orbits close to the host stars, with some in highly eccentric orbits. Dynamical processes during the late stage of planet formation are important to account for the present orbital properties. These processes include: planet migrations and resonance trappings caused by gravitational interactions between protostellar disk and planets, dynamical scattering due to interactions between planets, etc. In this paper, we review the major effects of these dynamical processes on the orbital characteristics of the planet systems.

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Halting Planet Migration in the Evacuated Centers of Protoplanetary Disks

Cited by 55 publications

References 38 publications

The mass-period distribution of close-in exoplanets

The mass-period distribution of close-in exoplanets

On the Interferometric Sizes of Young Stellar Objects

Dynamical evolution of extrasolar planetary systems

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