Notes.Listed are (i) parameters of the hydrostatic initial models; (ii) quantities derivable from these parameters; (iii) attributes of the inner boundary conditions (piston) used to simulate the pulsating stellar interiors as well as the resulting bolometric amplitudes Δm_bol; (iv) properties of the resulting wind; and (v) dust optical depths of the formed circumstellar envelope. The notation follows previous papers (Höfner et al. 2003; Nowotny et al. 2010, 2011a): R_⋆ – stellar radius of the hydrostatic initial model calculated from the luminosity L_⋆ and temperature T_⋆ via the relation L_⋆ = 4; P, Δu_p – period and velocity amplitude of the piston at the inner boundary; f_L – free parameter to adjust the luminosity amplitude at the inner boundary; ⟨ Ṁ ⟩, ⟨ u ⟩ – mean mass-loss rate and outflow velocity at the outer boundary; ⟨ f_c ⟩ – mean degree of condensation of the element carbon into amC dust grains at the outer boundary; ⟨ ρ_d/ρ_g ⟩ – mean dust-to-gas ratio at the outer boundary (cf. Eq. (2) of Höfner & Dorfi 1997); τ_dust – optical depth of the dust envelope at the specified wavelength (V-, H-, L′-band) based on radial structures at φ_bol ≈ 0.25 (see Sect. 4.2). The radial coordinates in this work are plotted in units of the corresponding stellar radii R_⋆ of the hydrostatic initial models, calculated from their luminosities L_⋆ and temperatures T_⋆ (as given in the table) via the relation L_⋆ = 4.