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The conditions in the protoplanetary disc are determinant for the variousplanet formation mechanisms. We present a framework which combinesself-consistent disc structures with the calculations of the growth rates ofplanetary embryos via pebble accretion, in order to study the formation ofSuper-Earths. We first perform 2D hydrodynamical simulations of the innerdiscs, considering a grain size distribution with multiple chemical species andtheir corresponding size and composition dependent opacities. The resultingaspect ratios are almost constant with orbital distance, resulting in radiallyconstant pebble isolation masses, the mass where pebble accretion stops. Thissupports the "peas-in-a-pod" constraint from the Kepler observations. Thederived pebble sizes are used to calculate the growth rates of planetaryembryos via pebble accretion. Discs with low levels of turbulence (expressedthrough the $\alpha$-viscosity) and/or high dust fragmentation velocities allowlarger particles, hence lead to smaller pebble isolation masses, and thecontrary. At the same time, small pebble sizes lead to low accretion rates. Wefind that there is a trade-off between the pebble isolation mass and the growthtimescale with the best set of parameters being an $\alpha$-viscosity of$10^{-3}$ and a dust fragmentation velocity of 10 m/s, mainly for an initialgas surface density (at 1 AU) greater than 1000 $\rm{g/cm^2}$. Aself-consistent treatment between the disc structures and the pebble sizes isthus of crucial importance for planet formation simulations.

The growth of super-Earths: the importance of a self-consistent treatment of disc structures and pebble accretion