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.
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