How does disk gravity really influence type-I migration?

Huré, Jean-Marc

doi:10.1051/0004-6361:200500099

Cited by 29 publications

(39 citation statements)

References 12 publications

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“…15 shows the semi-major axis of the planet for the SG model. Although the migration is slower than the Height2 model because of the disc self-gravity (Pierens & Huré 2005), …”

Section: Strength Of the Vortexmentioning

confidence: 86%

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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“…15 shows the semi-major axis of the planet for the SG model. Although the migration is slower than the Height2 model because of the disc self-gravity (Pierens & Huré 2005), …”

Section: Strength Of the Vortexmentioning

confidence: 86%

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

Ataiee

Dullemond

Kley

et al. 2014

A&A

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“…The inclusion of the disk self-gravity in our calculations confirms that the disk gravity accelerates type I migration. We solve the contradiction between the statements of Nelson & Benz (2003a, 2003b and Pierens & Huré (2005) regarding the impact of the disk self-gravity on the migration rate. The increase of the differ-ential Lindblad torque due to the disk gravity is typically 1 order of magnitude smaller than the spurious one induced by a planet freely migrating in a nonYself-gravitating disk.…”

Section: Discussionmentioning

confidence: 99%

Type I Planetary Migration in a Self‐Gravitating Disk

Baruteau

Masset

2008

ApJ

142

167

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We investigate the tidal interaction between a low-mass planet and a self-gravitating protoplanetary disk by means of two-dimensional hydrodynamic simulations. We first show that considering a planet as freely migrating in a disk without self-gravity leads to a significant overestimate of the migration rate. The overestimate can reach a factor of 2 for a disk having 3 times the surface density of the minimum mass solar nebula. Unbiased drift rates may be obtained only by considering a planet and a disk orbiting within the same gravitational potential. In the second part, the disk self-gravity is taken into account. We confirm that the disk gravity enhances the differential Lindblad torque with respect to the situation where neither the planet nor the disk feels the disk gravity. This enhancement only depends on the Toomre parameter at the planet location. It is typically 1 order of magnitude smaller than the spurious one induced by assuming a planet migrating in a disk without self-gravity. We confirm that the torque enhancement due to the disk gravity can be entirely accounted for by a shift of Lindblad resonances and can be reproduced by the use of an anisotropic pressure tensor. We do not find any significant impact of the disk gravity on the corotation torque.

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“…Consequently, the 2 migration terms may be inaccurate. The PPD ←→ PPD effects, which is the influence of the gas selfgravity on the differential Lindblad torque, has been studied for low-mass planets by Nelson & Benz (2003), Pierens & Huré (2005), and more recently by Baruteau & Masset (2008b,c). They confirmed that the type I migration is slightly accelerated by the disc selfgravity.…”

Section: Gravitational Interactionsmentioning

confidence: 99%

The dynamical role of the circumplanetary disc in planetary migration

Crida¹,

Baruteau

Kley³

et al. 2009

A&A

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Context. Numerical simulations of planets embedded in protoplanetary gaseous discs are a precious tool for studying the planetary migration; however, some approximations have to be made. Most often, the selfgravity of the gas is neglected. In that case, it is not clear in the literature how the material inside the Roche lobe of the planet should be taken into account. Aims. Here, we want to address this issue by studying the influence of various methods so far used by different authors on the migration rate. Methods. We performed high-resolution numerical simulations of giant planets embedded in discs. We compared the migration rates with and without gas selfgravity, testing various ways of taking the circum-planetary disc (CPD) into account. Results. Different methods lead to significantly different migration rates. Adding the mass of the CPD to the perturbing mass of the planet accelerates the migration. Excluding a part of the Hill sphere is a very touchy parameter that may lead to an artificial suppression of the type III, runaway migration. In fact, the CPD is smaller than the Hill sphere. We recommend excluding no more than a 0.6 Hill radius and using a smooth filter. Alternatively, the CPD can be given the acceleration felt by the planet from the rest of the protoplanetary disc. Conclusions. The gas inside the Roche lobe of the planet should be very carefully taken into account in numerical simulations without any selfgravity of the gas. The entire Hill sphere should not be excluded. The method used should be explicitly given. However, no method is equivalent to computing the full selfgravity of the gas.

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How does disk gravity really influence type-I migration?

Cited by 29 publications

References 12 publications

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

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

Type I Planetary Migration in a Self‐Gravitating Disk

The dynamical role of the circumplanetary disc in planetary migration

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