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

Ataiee, Sareh; Dullemond, C. P.; Kley, W.; Regály, Zs.; Méheut, H.

doi:10.1051/0004-6361/201322715

Cited by 22 publications

(23 citation statements)

References 49 publications

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“…In agreement with Ataiee et al (2014), we find that this occurs because the planet and vortex undergo horseshoe interaction that causes the vortex and planet to migrate together. -The inward migration of the vortex into the inner viscous region of the disk causes its eventual destruction, and this releases the planet.…”

Section: Resultssupporting

confidence: 85%

“…As expected from Ataiee et al (2014), we find that the vortex drags the planet with it during its migration, and when the vortex is destroyed it leaves the planet at some radius closer to the star. The subsequent evolution then depends on the planet mass and the disk mass, providing an effective filter for planets arriving at the dead zone inner edge.…”

Section: Introductionsupporting

confidence: 80%

“…The gravitational interaction between a massive vortex and a planetary mass body has been addressed by Regály et al (2013), Ataiee et al (2014). They found that under some circumstances a vortex can capture a planet at its front or at its back and cause it to migrate with the vortex.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Resultssupporting

confidence: 85%

Section: Introductionsupporting

confidence: 80%

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

Faure

Nelson

2016

A&A

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“…However, migration might push the formed planet inside the transition disc cavity after the vortex has formed but before it has dissipated. The vortex will certainly qualitatively effect the migration of such a low-mass planet (we note again we do not consider migration of our planet in our simulations presented here), as demonstrated by Ataiee et al (2014). This might mean that over a Myr lifetime of planet formation, the cycles of vortex generation and dissipation in the disc may dump a handful of low-mass planets inside the transition disc cavity, which could subsequently scatter.…”

Section: Long Term Evolutionmentioning

confidence: 88%

“…As discussed above, if a large scale vortex is able to form it will trap all the pebbles in the vortex itself. As none of the vortices seen in the simulations are co-located with the orbiting planet (see Ataiee et al 2014, for a discussion of how the planet and vortex may interact), then the vortex will starve the planet of pebbles and the rapid pebble accretion will cease.…”

Section: Long Term Evolutionmentioning

confidence: 99%

Dust traps as planetary birthsites: basics and vortex formation

Owen

Kollmeier

2017

Monthly Notices of the Royal Astronomical Society

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We present a simple model for low-mass planet formation and subsequent evolution within "transition" discs. We demonstrate quantitatively that the predicted and observed structure of such discs are prime birthsites of planets. Planet formation is likely to proceed through pebble accretion, should a planetary embryo (M 10 −4 M ⊕ ) form. Efficient pebble accretion is likely to be unavoidable in transition disc dust traps, as the size of the dust particles required for pebble accretion are those which are most efficiently trapped in the transition disc dust trap. Rapid pebble accretion within the dust trap gives rise, not only to low-mass planets, but to a large accretion luminosity. This accretion luminosity is sufficient to heat the disc outside the gravitational influence of the planet and makes the disc locally baroclinic, and a source of vorticity. Using numerical simulations we demonstrate that this source of vorticity can lead to the growth of a single large scale vortex in ∼ 100 orbits, which is capable of trapping particles. Finally, we suggest an evolutionary cycle: planet formation proceeds through pebble accretion, followed by vortex formation and particle trapping in the vortex quenching the planetary accretion and thus removing the vorticity source. After the vortex is destroyed the process can begin anew. This means transition discs should present with large scale vortices for a significant fraction of their lifetimes and remnant planets at large 10AU radii should be a common outcome of this cycle.

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The Effect of Convective Overstability on Planet Disk Interactions

Klahr

Gomes

2015

Proc. IAU

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We run global two dimensional hydrodynamical simulations, using the PLUTO code and the planet-disk model of Uribe et al. 2011, to investigate the effect of the convective overstability (CO) on planet-disk interactions. First, we study the long-term evolution of planet-induced vortices. We found that the CO leads to smoother planetary gap edges, thus weaker planet-induced vortices. The main result was the observation of two generation of vortices, which can pose an explanation for the location of the vortex in the Oph IRS48 system. The lifetime of the primary vortices, as well as the birth time of the secondary vortices are shown to be highly dependent on the thermal relaxation timescale. Second, we study the long-term evolution of the migration of low mass planets and assess whether the CO can prevent the saturation of the horseshoe drag. We found that the disk parameters that favour slow inward or outward migration oppose the amplification of vortices, meaning that the CO does not seem to be a good mechanism to prevent the saturation of the horseshoe drag. On the other hand, we observed a planetary trap, caused by vortices formed in the horseshoe region. This trap may be an alternative mechanism to prevent the fast type I migration rates.

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

Cited by 22 publications

References 49 publications

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

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

Dust traps as planetary birthsites: basics and vortex formation

The Effect of Convective Overstability on Planet Disk Interactions

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