Dynamics of pebbles in the vicinity of a growing planetary embryo: hydro-dynamical simulations

TL;DR

This study uses hydrodynamical simulations to analyze how pebble-sized objects interact with planetary embryos, providing insights into core growth mechanisms of giant planets and supporting the pebble accretion model.

Contribution

The paper offers detailed hydrodynamical simulations of pebble dynamics near planetary embryos, validating and extending previous theoretical estimates of accretion rates.

Findings

Accretion rates are within an order of magnitude of previous estimates.

Pebble size significantly influences the dynamics and accretion rates.

The pebble accretion model can explain rapid giant planet core growth.

Abstract

Understanding the growth of the cores of giant planets is a difficult problem. Recently, Lambrechts and Johansen (2012; LJ12) proposed a new model in which the cores grow by the accretion of pebble-size objects, as the latter drift towards the star due to gas drag. Here, we investigate the dynamics of pebble-size objects in the vicinity of planetary embryos of 1 and 5 Earth masses and the resulting accretion rates. We use hydrodynamical simulations, in which the embryo influences the dynamics of the gas and the pebbles suffer gas drag according to the local gas density and velocities. The pebble dynamics in the vicinity of the planetary embryo is non-trivial, and it changes significantly with the pebble size. Nevertheless, the accretion rate of the embryo that we measure is within an order of magnitude of the rate estimated in LJ12 and tends to their value with increasing pebble-size. We conclude that the model by LJ12 has the potential to explain the rapid growth of giant planet cores. The actual accretion rates however, depend on the surface density of pebble size objects in the disk, which is unknown to date.