Abstract
High temperatures or intense photon fluxes create highly charged ions in astrophysical plasmas. The atomic properties of these ions determine heating and cooling rates and opacities. The intensities of X-ray and ultraviolet spectral lines provide diagnostics for plasma temperature, density, ionization state and elemental composition. Here we discuss the solar corona, X-ray emitting binary stars and supernova remnants, emphasizing the kinds of observations made, the important ions and atomic processes, and the current and desirable levels of accuracy needed for the atomic rates.KeywordsNeutron StarSolar FlareSupernova RemnantCompact StarDielectronic RecombinationThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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