Various variables along a flow line anchored at 1 AU, for the dense MHD disk wind solution and three typical classes of stars: class 0 (M_⋆ = 0.1 M_⊙, Ṁ_acc = 5  ×  10^-6   M_⊙ yr^-1; dotted blue curves), class I (M_⋆ = 0.5 M_⊙, Ṁ_acc = 10^-6   M_⊙ yr^-1; solid red curves) and active class II (M_⋆ = 0.5 M_⊙, Ṁ_acc = 10^-7   M_⊙ yr^-1; dashed green curves). a) The gas temperature T; b) the number density of hydrogen nuclei n_H; c) the visual extinction A_V to the star, in magnitudes; d) the poloidal components of the bulk flow speed v (smooth top curves) and calculated drift speed v_in (lower 3 curves); Note that the Class II and Class I have the same M_⋆, hence the same bulk flow speed for r₀  =  1 AU; e) the X-ray H₂ ionization rate per molecule ; f) the effective radiation field in Draine units χexp ^− 3A_V (attenuation factor appropriate for carbon photoionisation); g) the fractional abundance of ions; h) the fractional abundance of H₂ (upper limit in the Class II model, see Sect. 3.1.3); i) the fractional abundance of CO (upper limits in the Class I/II models, see Sect. 3.1.4).