Streaming instability can be a very efficient way of overcoming growth and
drift barriers to planetesimal formation. However, it was shown that strong
clumping, which leads to planetesimal formation, requires a considerable number
of large grains. State-of-the-art streaming instability models do not take into
account realistic size distributions resulting from the collisional evolution
of dust. We investigate whether a sufficient quantity of large aggregates can
be produced by sticking and what the interplay of dust coagulation and
planetesimal formation is. We develop a semi-analytical prescription of
planetesimal formation by streaming instability and implement it in our dust
coagulation code based on the Monte Carlo algorithm with the representative
particles approach. We find that planetesimal formation by streaming
instability may preferentially work outside the snow line, where sticky icy
aggregates are present. The efficiency of the process depends strongly on local
dust abundance and radial pressure gradient, and requires a super-solar
metallicity. If planetesimal formation is possible, the dust coagulation and
settling typically need ~100 orbits to produce sufficiently large and settled
grains and planetesimal formation lasts another ~1000 orbits. We present a
simple analytical model that computes the amount of dust that can be turned
into planetesimals given the parameters of the disk model.Comment: 12 pages, 6 figures, 1 table, accepted for publication in A&A (minor
corrections with respect to v1
