Predicted intensity profiles normalized with respect to the Eddington flux for plane-parallel model stellar atmosphere (top) and spherically-symmetric model atmospheres (middle) in V-band (left) and K-band (right) wavebands. The bottom panels show the difference between intensity profiles computed from spherically-symmetric and plane-parallel model atmospheres. Spherical models predict much smaller intensities near the stellar limb relative to the plane-parallel models. For spherical models, intensity profiles for short-period Cepheids have smaller central intensities and sharp declines at smallest value of μ. Each line represents a step of Δlog P = 0.1 from log P = 0.4–2.