Non-LTE Model Atom Construction
arXiv:1012.0600 · doi:10.1051/eas/1043008
Abstract
Model atoms are an integral part in the solution of non-LTE problems. They comprise the atomic input data that are used to specify the statistical equilibrium equations and the opacities and emissivities of radiative transfer. A realistic implementation of the structure and the processes governing the quantum-mechanical system of an atom is decisive for the successful modelling of observed spectra. We provide guidelines and suggestions for the construction of robust and comprehensive model atoms as required in non-LTE line-formation computations for stellar atmospheres. Emphasis is given on the use of standard stars for testing model atoms under a wide range of plasma conditions.
19 pages, 8 figures
References in corpus (4)
- Neutral oxygen spectral line formation revisited with new collisional data: large departures from LTE at low metallicity
- C II abundances in early-type stars: solution to a notorious non-LTE problem
- Carbon abundances of early B-type stars in the solar vicinity. Non-LTE line-formation for C II/III/IV and self-consistent atmospheric parameters
- Non-LTE Balmer line formation in late-type spectra: Effects of atomic processes involving hydrogen atoms