Type I Planetary Migration in a Self‐Gravitating Disk

Baruteau, Clément; Masset, F.

doi:10.1086/529487

Cited by 142 publications

(175 citation statements)

References 22 publications

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“…In self-gravitating discs, the torque acting on an embedded planet can differ by a factor of two compared to non selfgravitating discs, as shown by Baruteau & Masset (2008b). These authors also state that self-gravity has no effect on the corotation torque in the linear regime, but our 3D simulations are in the non-linear regime.…”

Section: Convective Zonesupporting

confidence: 50%

Range of outward migration and influence of the disc’s mass on the migration of giant planet cores

Bitsch

Kley

2011

A&A

106

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Context. The migration of planets plays an important role in the early planet-formation process. An important problem has been that standard migration theories predict very rapid inward migration, which poses problems for population synthesis models. However, it has been shown recently that low-mass planets (20-30 M Earth ) that are still embedded in the protoplanetary disc can migrate outwards under certain conditions. Simulations have been performed mostly for planets at given radii for a particular disc model. Aims. Here, we plan to extend previous work and consider different masses of the disc to quantify the influence of the physical disc conditions on planetary migration. The migration behaviour of the planets will be analysed for a variety of positions in the disc. Methods. We perform three-dimensional (3D) radiation hydrodynamical simulations of embedded planets in protoplanetary discs. We use the explicit-implicit 3D hydrodynamical code NIRVANA that includes full tensor viscosity, and implicit radiation transport. For planets on circular orbits at various locations we measure the radial dependence of the torques for three different planetary masses. Results. For all considered planet masses (20-30 M Earth ) in this study we find outward migration within a limited radial range of the disc, typically from about 0.5 up to 1.5-2.5 a Jup . Inside and outside this interval, migration is inward and given by the Lindblad value for large radii. Interestingly, the fastest outward migration occurs at a radius of about a Jup for different disc and planet masses. Because outward migration stops at a certain location in the disc, there exists a zero-torque distance for planetary embryos, where they can continue to grow without moving too fast. For higher disc masses (M disc > 0.02 M ) convection ensues, which changes the structure of the disc and therefore the torque on the planet as well. Conclusions. Outward migration stops at different points in the disc for different planetary masses, resulting in a quite extended region where the formation of larger cores might be easier. In higher mass discs, convection changes the disc's structure resulting in fluctuations in the surface density, which influence the torque acting on the planet, and therefore its migration rate. Because convection is a 3D effect, 2D simulations of massive discs with embedded planets should be handled with care.

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Section: Convective Zonesupporting

confidence: 50%

Range of outward migration and influence of the disc’s mass on the migration of giant planet cores

Bitsch

Kley

2011

A&A

106

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“…In the case of a self-gravitating disc the corresponding accelerations are directly added to the righthand side of Eq. (2) (Baruteau & Masset 2008). The components of T, the viscous stress tensor, are given as…”

Section: Codementioning

confidence: 99%

Planet-vortex interaction: How a vortex can shepherd a planetary embryo

Ataiee

Dullemond

Kley

et al. 2014

A&A

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Context. Anti-cyclonic vortices are considered to be a favourable places for trapping dust and forming planetary embryos. On the other hand, they are massive blobs that can interact gravitationally with the planets in the disc. Aims. We aim to study how a vortex interacts gravitationally with a planet that migrates towards the vortex or with a planet that is created inside the vortex. Methods. We performed hydrodynamical simulations of a viscous locally isothermal disc using GFARGO and FARGO-ADSG. We set a stationary Gaussian pressure bump in the disc so that a large vortex is formed and maintained as a result of Rossby wave instability (RWI). After the vortex is established, we implanted a low-mass planet ([5, 1, 0.5] × 10 −6 M ) in the outer disc or inside the vortex and allowed it to migrate. We also examined the effect of vortex strength on the planet migration by doubling the height of the bump and checked the validity of the final result in the presence of self-gravity. Results. We noticed that regardless of the planet's initial position, the planet is finally locked to the RWI-created vortex in a 1:1 resonance or its migration is stopped at a larger orbital distance, in case of a stronger vortex. For the model with the weaker vortex (our standard model), we studied the effect of different parameters such as background viscosity, background surface density, mass of the planet, and different planet positions. In these models, while the trapping time and locking angle of the planet vary for different parameters, the main result, which is the planet-vortex locking, remains valid. We discovered that even a planet with a mass less than 5 × 10 −7 M comes out from the vortex and is locked to it at the same orbital distance. For a stronger vortex, both in non-selfgravitating and self-gravitating models, the planet migration is stopped far away from the radial position of the vortex. This effect can make the vortices a suitable place for continual planet formation under the condition that they save their shape during the planetary growth.

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“…Since we are not interested in the evolution of the binary star system but only in the structure of the disk under the binary perturbation after the tidal truncation of the disk, we fix the orbital parameters of the companion star. In the latest release of FARGO a Poisson equation solver based on the Fourier method has been implemented (Baruteau & Masset 2008) allowing us to properly model the disk self-gravitation (hereinafter SG). The impact of SG on the disk evolution is relevant when modelling highly perturbed massive disks.…”

Section: The Hydrodynamical Modelmentioning

confidence: 99%

“…In a first step, we focus on the influence of the binary eccentricity using for all other parameters mean standard values which are expected from observations. For the simulations, we use the latest release of the hydrodynamical code FARGO (Masset 2000) which now includes disk self-gravitation (Baruteau & Masset 2008). Comparison with former simulations allows the investigation of its influence on the formation of structures in the disk, on its eccentricity and orientation.…”

Section: Introductionmentioning

confidence: 99%

On the eccentricity of self-gravitating circumstellar disks in eccentric binary systems

Marzari¹,

Scholl

Thébault

2009

A&A

Self Cite

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Aims. We study the evolution of circumstellar massive disks around the primary star of a binary system focusing on the computation of disk eccentricity. In particular, we concentrate on its dependence on the binary eccentricity. Self-gravitation is included in our numerical simulations. Our standard model assumes a semimajor axis for the binary of 30 AU, the most probable value according to the present binary statistics. Methods. Two-dimensional hydrodynamical computations are performed with FARGO. Besides the dynamical standard method to determine disk eccentricities, we apply a morphological method which may allow a better comparison with observations. Results. Self-gravitation leads to disks that, on average, have low eccentricity. Moreover, the orientation of the disk computed with the standard dynamical method always librates instead of circulating as in simulations without self-gravitation. The disk eccentricity decreases with the binary eccentricity, a result found also in models without self-gravitation. Conclusions. Disk self-gravitation appears to be an important factor in determining the evolution of a massive disk in a binary system. High eccentricity binaries are not necessarily a hostile environment for planetary accretion.

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Type I Planetary Migration in a Self‐Gravitating Disk

Cited by 142 publications

References 22 publications

Range of outward migration and influence of the disc’s mass on the migration of giant planet cores

Range of outward migration and influence of the disc’s mass on the migration of giant planet cores

Planet-vortex interaction: How a vortex can shepherd a planetary embryo

On the eccentricity of self-gravitating circumstellar disks in eccentric binary systems

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