Notes. The parameters for the planetesimal formation are the same for every simulation. The total mass in planetesimals within 10 au is given as 525 M_⊕ in the Σ_P∝ r^−2.1 system, 327 M_⊕ in the Σ_P ∝ r^−1.5 system, and 132 M_⊕ in the Σ_P ∝ r^−0.9 system. The dynamical model leads to a total planetesimal mass within 10 au after one million years of 407 M_⊕. The high planetesimal mass in the dynamical formation run is a result of the high initial dust mass that results from the metallicity (dust-to-gas ratio) and the high total gas mass of 0.128 M_⊙. The efficiency for planetesimal formation ɛ is given low enough so that a large fraction of the outer mass can drift inward and contribute to planetesimal formation in the inner regions. A higher efficiency would lead to a lower mass within 10 au because most of the outer material would quickly be transformed into planetesimals outside and not contribute to substantial planetesimal formation in the inner region of the disk.