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

Abstract

Context: Anticyclonic vortices are considered as 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 which migrates toward it or a planet which 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 in a way that RWI is triggered. After a large vortex is established, we implanted a low mass planet 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 and checked the validity of the final result in the presence of self-gravity. Results: We noticed regardless of the planet's initial position, the planet is finally locked to the vortex or its migration is stopped in a farther orbital distance in case of a stronger vortex. For the model with the weaker vortex, 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_{\star} comes out from the vortex and is locked to it at the same orbital distance. For a stronger vortex, both in non-self-gravitated 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.

13 pages, 21 figures,Accepted to be published in A&A

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• Gap formation and stability in non-isothermal protoplanetary discs
• Survival of planet-induced vortices in 2D disks
• Planetesimal formation in self-gravitating discs -- dust trapping by vortices
• Vortex Formation and Evolution in Planet Harboring Disks under Thermal Relaxation
• Dust traps as planetary birthsites: basics and vortex formation
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• Trapping (sub-)Neptunes similar to TOI-216b at the inner disk rim: Implications for the disk viscosity and the Neptunian desert
• Accreting luminous low-mass planets escape from migration traps at pressure bumps
• Spreading pressure bumps in gas-dust discs can stall planet migration via planet-vortex interactions
• Increased isolation mass for pebble accreting planetary cores in pressure maxima of protoplanetary discs
• On wave interference in planet migration: dead zone torques modified by active zone forcing