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In this work we have used 3D hydrodynamical (CO5BOLD) and 1D hydrostatic(LHD) stellar atmosphere models to study the importance of convection andhorizontal temperature inhomogeneities in stellar abundance work related tolate-type giants. We have found that for a number of key elements, such as Na,Mg, Si, Ca, Ti, Fe, Ni, Zn, Ba, Eu, differences in abundances predicted by 3Dand 1D models are typically minor (< 0.1 dex) at solar metallicity. However, at[M/H] = -3 they become larger and reach to -0.5...-0.8 dex. In case of neutralatoms and fixed metallicity, the largest abundance differences were obtainedfor the spectral lines with lowest excitation potential, while for ionizedspecies the largest 3D-1D abundance differences were found for lines of highestexcitation potential. The large abundance differences at low metallicity arecaused by large horizontal temperature fluctuations and lower mean temperaturein the outer layers of the 3D hydrodynamical model compared with its 1Dcounterpart.

Chemical abundances in metal-poor giants: limitations imposed by the use of classical 1D stellar atmosphere models