Abstract
We first consider the general information scheme for the interpretation of observational data (Figure 1). From the relations plotted it is evident that (in going from left to right) this scheme can only be solved if distances are known and if we are able to determine the atmospheric parameters: effective temperature, T eff, surface gravity, g,and chemical composition from observations of colors and spectra — which is the genuine task of the theory of stellar atmospheres.
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Weidemann, V. (1971). White Dwarf Atmospheres. In: Luyten, W.J. (eds) White Dwarfs. International Astronomical Union/Union Astronomical International, vol 42. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-3081-6_14
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