Emergent intensity and surface vertical velocities in different stellar types for models with and without magnetic field. From top to bottom: snapshot of the bolometric intensity and v_z at τ = 1 for the HD case (rows 1 and 2), bolometric intensity and v_z at τ = 1 for the SSD case (row 3 and 4), and the corresponding vertical magnetic field at τ = 1 (row 5, from left to right) for spectral types F, G, K, and M, respectively. The green circles indicate the bright points and corresponding magnetic field concentrations.