Models of solar magnetic structures

The models have been derived from non-LTE inversions of high-resolution spectropolarimetric observations of four CaII and FeI lines. The observed targets are dark and bright components of a sunspot umbra; dark and bright components of a sunspot penumbra; a canopy between two sunspots; a facula; and a network element.

These models may be employed, e.g., to compute realistic synthetic Stokes spectra of photospheric and chromospheric lines.