Notes. Listed are (i) parameters of the hydrostatic initial model; (ii) quantities derivable from these parameters; (iii) attributes of the inner boundary (piston) used to simulate the pulsating stellar interior as well as the resulting bolometric amplitude Δm_bol; and (iv) properties of the resulting wind. The notation was adopted from previous papers (DMA3, NHA10): 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 – mass loss rate and outflow velocity at the outer boundary;  ⟨ f_c ⟩  – mean degree of condensation of carbon into dust at the outer boundary. The radial coordinates in Figs. A.1 and A.2 are plotted in units of the corresponding stellar radius R _⋆  of the hydrostatic initial model, calculated from the luminosity L _⋆  and temperature T _⋆  via the relation L _⋆  = 4π σ.