出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：We investigate the influence of convection on the formation of molecular spectral lines in the atmospheres of late-type giants. For this purpose we use the 3D hydrodynamical CO5BOLD and classical 1D LHD stellar atmosphere codes and synthesize a number of fictitious lines belonging to a number of astrophysically relevant molecules, C2, CH, CN, NH, OH.We find that differences between the abundances obtained from molecular lines using the 3D and 1D model atmospheres are generally small at [M/H]=0.0, but they quickly increase at sub-solar metallicities and may reach ∼−0.9 dex at [M/H]=–3.0. The 3D–1D abundance corrections show a significant dependence on the spectral line parameters, such as wavelength and excitation potential. Our comparison, therefore, points to a complex interplay between the spectral line formation and convection that should be properly adressed in stellar abundance analysis.
