The Fontenla et al. analysis comprises a set of models representing different features of the solar atmosphere. The objective in creating these models was to represent spectral irradiance variability based on image partition into the different features. These are classical 1D "semi-empirical" models which smooth out all of the rest of the variability, and so the physical parameters only represent mean values in some general sense. The height scale is based upon optical depth in these mean parameters and is known to be insufficiently extended in height.
We have chosen three representative models for estimating plasma parameters with these approximations in mind. Note that the nature of these models imposes the restriction Te = Ti. Model 1001 represents the quiet solar atmosphere.
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