Extreme pebble accretion in ringed protoplanetary discs

Axisymmetric dust rings containing tens to hundreds of Earth masses of solids have been observed in protoplanetary discs with (sub-)millimetre imaging. Here, we investigate the growth of a planetary embryo in a massive (150 M-circle plus) axisymmetric dust trap through dust and gas hydrodynamics simulations. When accounting for the accretion luminosity of the planetary embryo from pebble accretion, the thermal feedback on the surrounding gas leads to the formation of an anticyclonic vortex. Since the vortex forms at the location of the planet, this has significant consequences for the planet's growth: as dust drifts towards the pressure maximum at the centre of the vortex, which is initially co-located with the planet, a rapid accretion rate is achieved, in a distinct phase of 'vortex-assisted' pebble accretion. Once the vortex separates from the planet due to interactions with the disc, it accumulates dust, shutting off accretion on to the planet. We find that this rapid accretion, mediated by the vortex, results in a planet containing approximate to 100 M-circle plus of solids. We follow the evolution of the vortex, as well as the efficiency with which dust grains accumulate at its pressure maximum as a function of their size, and investigate the consequences this has for the growth of the planet as well as the morphology of the protoplanetary disc. We speculate that this extreme formation scenario may be the origin of giant planets that are identified to be significantly enhanced in heavy elements.

Automated summary

This study investigates the growth of a planetary embryo in a massive dust trap and finds that the thermal feedback from the accretion of pebbles leads to the formation of a vortex. The vortex allows for a rapid accretion rate, resulting in a planet with a significant amount of solids. The authors speculate that this extreme formation scenario may explain the origin of giant planets enriched in heavy elements.