  The accretion of pebbles on planetary cores has been widely studied in recent
years and is found to be a highly effective mechanism for planetary growth.
While most studies assume planetary cores as an initial condition in their
simulation, the question how, where and when these cores form is often
neglected. We study the impact of pebble accretion during the formation phase
and subsequent evolution of planetary embryos in the early stages of
circumstellar disk evolution. In doing so we aim to quantify the timescales and
local dependency of planetary embryo formation, based on the solid evolution of
the disk. We connect a one dimensional two population model for solid evolution
and pebble flux regulated planetesimal formation to the N-body code LIPAD. In
our study we focus on the growth of planetesimals with an initial size of 100
km in diameter by planetesimal collisions and pebble accretion for the first 1
million years of a viscously evolving disk. We compare 18 different N-body
simulations in which we vary the total planetesimal mass after 1 million years,
the surface density profile of the planetesimal disk, the radial pebble flux
and the possibility of pebble accretion. Pebble accretion leads to the
formation of fewer, but substantially more massive embryos. The area of
possible embryo formation is weakly influenced by the accretion of pebbles and
the innermost embryos tend to form slightly earlier compared to the simulations
in which pebble accretion is neglected. Pebble accretion strongly enhances the
formation of super earths in the terrestrial planet region, but it does not
enhance the formation of embryos at larger distances.
