Balmer line comparison between the PoWR models (red, solid line) and the TLUSTY models (black, dashed line) for dwarfs (upper panels), giants (middle panels), and supergiants (lower panels). The stellar parameters used in the PoWR models are as in Table 2, but with negligible mass-loss rates (log Ṁ = −9 [ M_⊙ yr^-1 ]), small terminal velocities (500 km s^-1), and large radii, to avoid wind and curvature effects.