Dependence of the resultant planetesimal belt on Ṁ_g. Left to right panels are the cases of Ṁ_g=10⁻⁹,10⁻⁸, and 10⁻⁷ M_⊙ yr⁻¹, respectively. The gray lines represent the surface density of solids in the classical minimum mass solar nebula model (MMSN; Σ_pla = 30(r/1 au)^−3/2 gcm⁻²) of Weidenschilling (1977) for reference. By t ≃ 1 × 10⁵ yr, the system reaches a steady-state in ρ_p/ρ_g and width of the planetesimal ring. Here, α_acc = 10⁻², τ_s = 0.1, and k_SI = 10⁻³ are used.