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Line contribution functions are useful diagnostics for studying spectral lineformation in stellar atmospheres. I derive an expression for the contributionfunction to the abso- lute flux depression that emerges from three-dimensionalbox-in-a-star model stellar atmospheres. I illustrate the result by comparingthe local thermodynamic equilibrium (LTE) spectral line formation of thehigh-excitation permitted OI777nm lines with the non-LTE case.

On line contribution functions and examining spectral line formation in 3D model stellar atmospheres