Spectral line changes across a stellar disk, predicted from 3D simulations with the CO ⁵BOLD code of an “F3 V” main-sequence star. Fe I lines of three different strengths (λ = 620 nm, χ = 3 eV) are shown at disk center (viewing angle against the normal to the stellar surface θ = 0; cos θ = μ = 1) and close to the limb (μ = 0.21). Relative to a frame of rest, lines are displaced toward shorter wavelengths (“convective blueshift”), which is an effect that changes from disk center toward the limb. Profiles are here normalized to the local continuum intensity at each center-to-limb position; the wavelength scale is in equivalent Doppler velocities.