Disk Surface Density Transitions as Protoplanet Traps

Masset, F.; Morbidelli, Alessandro; Crida, A.; Ferreira, J.

doi:10.1086/500967

Cited by 339 publications

(462 citation statements)

References 30 publications

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“…Thus when approaching the inner rim of such a disk, the inward migration can be stopped rapidly (Masset et al 2006). If the inner rim is located at a given radius of the disk (e.g.…”

Section: Sudden Termination Of Migrationmentioning

confidence: 99%

Stability and formation of the resonant system HD 73526

Sándor

Kley²,

Klagyivik

2007

A&A

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Context. Based on radial velocity measurements, it has been found that the two giant planets detected around the star HD 73526 are in 2:1 resonance. However, as our numerical integration shows, the derived orbital data for this system result in chaotic behavior of the giant planets, which is uncommon among the resonant extrasolar planetary systems. Aims. We present regular (non-chaotic) orbital solutions for the giant planets in the system HD 73526 and offer formation scenarios based on combining planetary migration and sudden perturbative effects such as planet-planet scattering or rapid dispersal of the protoplanetary disk. A comparison with the already-studied resonant system HD 128311, exhibiting similar behavior, is given. Methods. The new sets of orbital solutions were derived using the Systemic Console. The stability of these solutions was investigated using the Relative Lyapunov indicator, while the migration and scattering effects are studied by gravitational N-body simulations applying non-conservative forces. Additionally, hydrodynamic simulations of embedded planets in protoplanetary disks were performed to follow the capture into resonance. Results. For the system HD 73526 we demonstrate that the observational radial velocity data are consistent with a coplanar planetary system in a stable 2:1 resonance exhibiting apsidal corotation. We have shown that, similarly to the system HD 128311, the present dynamical state of HD 73526 could be the result of a mixed evolutionary process combining planetary migration and a perturbative event.

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“…Thus when approaching the inner rim of such a disk, the inward migration can be stopped rapidly (Masset et al 2006). If the inner rim is located at a given radius of the disk (e.g.…”

Section: Sudden Termination Of Migrationmentioning

confidence: 99%

Stability and formation of the resonant system HD 73526

Sándor

Kley²,

Klagyivik

2007

A&A

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“…1, while the lighter case is shown in the top panel. Surprisingly, the planets are not trapped at the dead zone inner edge as predicted by Masset et al (2006b). However, the orbital evolution of the same planet in the locally isothermal disk model, where the vortex cycle does not develop, is consistent with the trapping of planets at the dead zone inner edge.…”

Section: Planet Orbital Evolution At the Dead-active Zone Interfacementioning

confidence: 55%

“…The concept of a planet trap was introduced by Masset et al (2006b), where a disk location with a positive gradient in the surface density can trap a migrating planet because the vortensity related corotation torque is expected to have a large positive value in such a region. There are a number of hypothetical reasons why a planet trap may arise within a protoplanary disk, but an oft cited one is that regions between orbital radii 0.5 R 10 au are expected to host a dead zone where the effective disk viscosity is small due to poor coupling between the gas and magnetic fields (e.g.…”

Section: Introductionmentioning

confidence: 99%

Planet filtering at the inner edges of dead zones in protoplanetary disks

Faure

Nelson

2016

A&A

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Context. The interface between the dead zone and the inner active zone in a protoplanetary disk provides a promising region where the inward migration of planets may be halted owing to the existence of strong corotation torques. Recent work has indicated that this region may be prone to supporting a vortex cycle, during which vortices form at the dead-active zone interface and migrate into the active region before being destroyed, after which a new vortex forms and the cycle repeats. Aims. The aim of this paper is to examine the interaction between migrating planets and this vortex cycle, and to determine the conditions under which planets are able to remain trapped at the dead-active zone interface. Methods. We use the magnetohydrodynamics (MHD) codes PLUTO and RAMSES to perform 2D viscous disk simulations and 3D MHD simulations of protoplanetary disks containing migrating planets. A temperature switch is used to control the effective viscosity at the dead-active zone interface. Results. We find that both low mass and non-gap forming higher mass planets are able to escape from the planet trap at the inner edge of the dead zone as a result of their interaction with the migrating vortices, whereas intermediate mass planets remain trapped for the duration of simulation run times. Conclusions. Our results indicate that the vortex cycle causes the dead zone inner edge to act as an effective and mass-dependent planet filter, allowing some planets to pass through this region and others to remain there over long timescales.

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“…How to reduce the speed of type I migration is a key issue of present planet formation theory. Recent hydrodynamical simulation indicates that type I inward migration can be stopped near a boundary of a density maximum (Masset et al 2006). During the orbital decay of a protoplanet, the exchange of angular momentum between it and the fluid elements that perform U-turn at the end of the horseshoe streamlines generates a corotation torque on the protoplanet (Ward 1991, Masset 2002.…”

Section: Type I Migrationmentioning

confidence: 99%

Formation and tidal evolution of hot super-Earths in multiple planetary systems

Zhou

2010

EAS Publications Series

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Abstract. Hot super-Earths are exoplanets with masses ≤ 10M⊕ and orbital periods ≤ 20 days. Around 8 hot super-Earths have been discovered in the neighborhood of solar system. In this lecture, we review the mechanisms for the formation of hot super-Earths, dynamical effects that play important roles in sculpting the architecture of the multiple planetary systems. Two example systems (HD 40307 and GJ 436) are presented to show the formation and evolution of hot super-Earths or Neptunes.

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Disk Surface Density Transitions as Protoplanet Traps

Abstract: Astrophysical Journal, 642, pp. 478-487, http://dx.doi.org./10.1086/500967International audienc

Cited by 339 publications

References 30 publications

Stability and formation of the resonant system HD 73526

Stability and formation of the resonant system HD 73526

Planet filtering at the inner edges of dead zones in protoplanetary disks

Formation and tidal evolution of hot super-Earths in multiple planetary systems

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