Formation and long-term evolution of 3D vortices in protoplanetary discs

Méheut, H.; Keppens, Rony; Casse, Fabien; Benz, W.

doi:10.1051/0004-6361/201118500

Cited by 78 publications

(91 citation statements)

References 44 publications

(69 reference statements)

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“…In more realistic models, the vortex could migrate (Paardekooper et al 2010b), move in the disc (Regály et al 2013), or even be threatened by decay (e.g. Meheut et al 2012a). It is very interesting to explore whether a moving vortex in a more realistic disc is able to "lay a planet system" or not.…”

Section: Discussionmentioning

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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Section: Discussionmentioning

confidence: 99%

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

Ataiee

Dullemond

Kley

et al. 2014

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“…To simulate the growth of the RWI in the gas disk, we used the numerical methods presented in Meheut et al (2012a), which we briefly summarise here. The governing equations are solved in cylindrical coordinates (r, φ, z), centred on the star, and read as…”

Section: Methodsmentioning

confidence: 99%

“…Another proposed formation mechanism for the vortices is the Rossby wave instability (RWI). This is a linear instability that grows A&A 545, A134 (2012) in the region of a pressure extremum, which avoids vortex migration (Meheut et al 2012a). This instability was first studied in 2D both analytically (Lovelace et al 1999) and numerically (Li et al 2001;.…”

Section: Introductionmentioning

confidence: 99%

Dust-trapping Rossby vortices in protoplanetary disks

Méheut¹,

Méliani²,

Varnière³

et al. 2012

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110

108

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Context. One of the most challenging steps in planet formation theory is the one leading to the formation of planetesimals of kilometre size. A promising scenario involves the existence of vortices able to concentrate a large amount of dust and grains in their centres. Up to now this scenario has mostly been studied in 2D razor thin disks. A 3D study including, simultaneously, the formation and resulting dust concentration of the vortices with vertical settling, is still missing. Aims. The Rossby wave instability self-consistently forms 3D vortices, which have the unique quality of presenting a large-scale vertical velocity in their centre. Here we aim to study how this newly discovered effect can alter the dynamic evolution of the dust. Methods. We performed global 3D simulations of the RWI in a radially and vertically stratified disk using the code MPI-AMRVAC. After the growth phase of the instability, the gas and solid phases are modelled by a bi-fluid approach, where the dust is considered as a fluid without pressure. Both the drag force of the gas on the dust and the back reaction of the dust on the gas are included. Multiple grain sizes from 1 mm to 5 cm are used with a constant density distribution. Results. We obtain in a short timescale a high concentration of the largest grains in the vortices. Indeed, in 3 rotations the dust-to-gas density ratio grows from 10 −2 to unity leading to a concentration of mass up to that of Mars in one vortex. The presence of the radial drift is also at the origin of a dust pile-up at the radius of the vortices. Lastly, the vertical velocity of the gas in the vortex causes the sedimentation process to be reversed, the mm size dust is lifted and higher concentrations are obtained in the upper layer than in the midplane. Conclusions. The Rossby wave instability is a promising mechanism for planetesimal formation, and the results presented here can be of particular interest in the context of future observations of protoplanetary disks.

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“…As an example, at 35 AU, for H/r = 0.07, a Stokes number of 0.2, and a gas density contrast of ρ max g /ρ min g = 2, the time scale is 3 × 10 5 years, but could be as short as 10 2 orbits for optimal conditions. Any gas structure therefore has to be long-lived to cause strong asymmetries in the dust, making the asymmetries caused by a planet or longlived vortices the best candidates (Meheut et al 2012). If such an accumulation is formed and the gas asymmetry disappears, it still takes t diff to "remove" it, which at 35 AU is of the order of Myrs.…”

Section: Analytical Modelmentioning

confidence: 99%

Lopsided dust rings in transition disks

Birnstiel

Dullemond

Pinilla

2013

A&A

157

169

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Context. Particle trapping in local or global pressure maxima in protoplanetary disks is one of the new paradigms in the theory of the first stages of planet formation. However, finding observational evidence for this effect is not easy. Recent work suggests that the large ring-shaped outer disks observed in transition disk sources may in fact be lopsided and constitute large banana-shaped vortices. Aims. We wish to investigate how effectively dust can accumulate along the azimuthal direction. We also want to find out if the size-sorting resulting from this accumulation can produce detectable signatures at millimeter wavelengths. Methods. To keep the numerical cost under control we developed a 1+1D method in which the azimuthal variations are treated separately from the radial variations. The azimuthal structure was calculated analytically for a steady-state between mixing and azimuthal drift. We derived equilibration time scales and compared the analytical solutions to time-dependent numerical simulations. Results. We found that weak, but long-lived azimuthal density gradients in the gas can induce very strong azimuthal accumulations of dust. The strength of the accumulations depends on the Péclet number, which describes the relative importance of advection and diffusion. We applied our model to transition disks and our simulated observations show that this effect would be easily observable with the Atacama Large Millimeter/submillimeter Array (ALMA) and could be used to put constraints on the strength of turbulence and the local gas density.

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Formation and long-term evolution of 3D vortices in protoplanetary discs

Cited by 78 publications

References 44 publications

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

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

Dust-trapping Rossby vortices in protoplanetary disks

Lopsided dust rings in transition disks

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