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We present the results of realistic, 3D, hydrodynamical, simulations ofsurface convection in red giant stars with varying effective temperatures andmetallicities. We use the convection simulations as time-dependent,hydrodynamical, model atmospheres to compute spectral line profiles for anumber of ions and molecules under the assumption of local thermodynamicequilibrium (LTE). We compare the results with the predictions of lineformation calculations based on 1D, hydrostatic, model stellar atmospheres inorder to estimate the impact of 3D models on the derivation of elementalabundances. We find large negative 3D-1D LTE abundance corrections (typically-0.5 to -1 dex) for weak low-excitation lines from molecules and neutralspecies in the very low metallicity cases. Finally, we discuss the extent ofdepartures from LTE in the case of neutral iron spectral line formation.

Beyond 1D: spectral line formation with 3D hydrodynamical model atmospheres of red giants