We want to include the opacity of millions or hundreds of millions of lines in model stellar atmosphere calculations, then generate detailed, realistic spec-tra from those model atmospheres, then model the observation process, and finally compare the calculated spectra to observed spectra to determine the properties of stars so that we can understand their evolution and the evolution of galaxies.
CITATION STYLE
Kurucz, R. L. (2014). How to Build a Model of the Atmosphere and Spectrum (pp. 25–37). https://doi.org/10.1007/978-3-319-06956-2_3
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