Abstract

The role of pebble accretion has becoming increasingly important in the core accretion scenario over recent years. Traditionally, core accretion utilised large planetesimals as the main source of growth for planetary cores. The main problem with using large planetesimals was that the growth timescales to form the cores of giant planets were typically longer than expected protoplanetary disc lifetimes. Growth timescales when using pebbles however, are much shorter, due to the greater efficiency at which pebbles can be accreted. Recent works have utilised these shorter timescales to examine the growth of giant planets, ice giants, and the terrestrial planets. In most of these works however, only a single planet has been assumed to form in the disc.

In this talk I will present new models of pebble accretion where multiple planetary embryos have been considered to form in a single disc. To do this, we have coupled the N-body integrator Mercury6 to the Bern population synthesis model, including up-to-date prescriptions for disc evolution, planet migration, accretion and internal structure. The effects of planet multiplicity on their accretion and migration rates will be discussed, as well as the final planetary systems that emerge from the system.