The growth of super-Earths

The conditions in the protoplanetary disc are determinant for various planet formation mechanisms. We present a framework which combines self-consistent structures with calculations of growth rates planetary embryos via pebble accretion, order to study Super-Earths. first perform 2D hydrodynamical simulations inner discs, considering grain size distribution multiple chemical species and their corresponding composition dependent opacities. resulting aspect ratios almost constant orbital distance, radially isolation masses, mass where accretion stops. This supports "peas-in-a-pod" constraint from Kepler observations. derived sizes used calculate accretion. Discs low levels turbulence (expressed through $\alpha$-viscosity) and/or high dust fragmentation velocities allow larger particles, hence lead smaller contrary. At same time, small rates. find that there is trade-off between timescale best set parameters being an $\alpha$-viscosity $10^{-3}$ velocity 10 m/s, mainly initial gas surface density (at 1 AU) greater than 1000 $\rm{g/cm^2}$. A treatment thus crucial importance simulations.