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• W2108451036 abstract "Context. Three-dimensional (3D) radiative hydrodynamic model atmospheres of metal-poor late-type stars are characterized by cooler upper photospheric layers than their one-dimensional counterparts. This property of 3D model atmospheres can dramatically affect the determination of elemental abundances from temperature-sensitive spectral features, with profound consequences on galactic chemical evolution studies. Aims. We investigate whether the cool surface temperatures predicted by 3D model atmospheres of metal-poor stars can be ascribed to approximations in the treatment of scattering during the modelling phase. Methods. We use the Bifrost code to construct 3D model atmospheres of metal-poor stars and test three different ways to handle scattering in the radiative transfer equation. As a first app roach, we solve iteratively the radiative transfer equatio n for the general case of a source function with a coherent scattering term, tr eating scattering in a correct and consistent way. As a second approach, we solve the radiative transfer equation in local thermodynamic equilibrium approximation, neglecting altogether the contribution of continuum scattering to extinction in the optically thin la yers; this has been the default mode in our previous 3D modelling as well as in present Stagger-Code models. As our third and final approach, we treat continuum sc attering as pure absorption everywhere, which is the standard case in the 3D modelling by the CO 5 BOLD collaboration. Results. For all simulations, we find that the second approach produce s temperature structures with cool upper photospheric layers very similar to the case in which scattering is treated corre ctly. In contrast, treating scattering as pure absorption l eads instead to significantly hotter and shallower temperature stratificat ions. The main differences in temperature structure between our published models computed with the Stagger- and Bifrost codes and those generated with the CO 5 BOLD code can be traced to the different treatments of scattering. Conclusions. Neglecting the contribution of continuum scattering to extinction in optically thin layers provides a good approximation to the full, iterative solution of the radiative transfer eq uation in metal-poor stellar surface convection simulatio ns, and at a much lower computational cost. Our results also demonstrate that the cool temperature stratifications predicted for metal-poor l ate-type stars by previous models by our collaboration are not an artifact of the approximated treatment of scattering." @default.
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• W2108451036 date "2011-04-01" @default.
• W2108451036 modified "2023-09-23" @default.
• W2108451036 title "Three-dimensional surface convection simulations of metal-poor stars The effect of scattering on the photospheric temperature stratification" @default.
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