Comparison between the evolution of the solid mass reservoir according to Eq. (56) for different initial disk sizes R₁. We indicate the median dust masses derived by Tychoniec et al. (2020) for Class 0 and Class I sources in Perseus, and for Class II sources in Lupus by Ansdell et al. (2016). The dashed lines indicate the median value for each evolutionary class. We assume that the evolutionary phases Class 0 and I last approximately 0.1 and 0.5 Myr, respectively (Dunham et al. 2014). We assume that Z₀ = 0.01 remains constant until solids grow to the drift or fragmentation limit at R₁ as in Fig. 2. For R₁ = 10, 30,100 AU, we estimate t₀ = 0.007, 0.03, 0.2 Myr and St = 0.02, 0.03, 0.03, respectively. Gray dotted lines indicate solid mass decrease solely due to gas accretion onto the star, i.e., M_s(t) = Z₀M_g(t).