Role of input atomic data in spectroscopic analyses of the Sun and metal-poor stars
2011
Analysis of high-resolution stellar spectra relies heavil y upon atomic data. These include energy levels, wavelengths, cross-sections for va rious types of interactions between particles and photons, such as photoionization and collision induced transitions. Quantum-
mechanical calculationsprovide largest part of these data. In this paper I describe atomic data necessary to compute model atmospheres and
line formationfor the
late-type starsboth in the assumption of local
thermodynamic equilibrium(LTE) and in a more general case of non-LTE. I will focus on transition metals with 21< Z< 29 and discuss whether (and where) more complete and/or accurate atomic data are necessary.
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