  If we want to understand planetesimal formation, the only data set we have is
our own Solar System. It is particularly interesting as it is so far the only
planetary system we know of that developed life. Understanding the conditions
under which the Solar Nebula evolved is crucial in order to understand the
different processes in the disk and the subsequent dynamical interaction
between (proto-)planets, once the gas disk is gone. Protoplanetary disks
provide a plethora of different parameters to explore. The question is whether
this parameter space can be constrained, allowing simulations to reproduce the
Solar System. Models and observations of planet formation provide constraints
on the initial planetesimal mass in certain regions of the Solar Nebula. By
making use of pebble flux-regulated planetesimal formation, we perform a
parameter study with nine different disk parameters like the initial disk mass,
initial disk size, initial dust-to-gas ratio, turbulence level, and more. We
find that the distribution of mass in planetesimals in the disk depends on the
planetesimal formation timescale and the pebbles' drift timescale. Multiple
disk parameters can influence pebble properties and thus planetesimal
formation. However, it is still possible to draw some conclusions on potential
parameter ranges. Pebble flux-regulated planetesimal formation seems to be very
robust, allowing simulations with a wide range of parameters to meet the
initial planetesimal constraints for the Solar Nebula. I.e., it does not
require a lot of fine tuning.
