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Three-dimensional models of metal-poor stars
I present here the main results of recent realistic, 3D, hydrodynamical simulations of convection at the surface of metal-poor red giant stars. I discuss the application of these convection simulations as time-dependent, 3D, hydrodynamical model atmospheres to spectral line formation calculations and abundance analyses. The impact of 3D models on derived elemental abundances is investigated by means of a differential comparison of the line strengths predicted in 3D under the assumption of localdoi:10.1088/0031-8949/2008/t133/014004 fatcat:t5ibmijlv5bhvmdwobrhapzaiq