Intensity profiles in fluxtubes

A method is presented for reconstructing the intensity profile I formed in the magnetic elements which have diameters smaller than the best presently achievable spatial resolution. It follows the same line as in Solanki and Stenfio (1984). As a starting point, I and V (fourth Stokes parameter which originates only in magnetic regions) of the facula and the I observed in the quiet Sun were used. The filling factor and the ratio between the continuum intensity of the magnetic and non-magnetic parts of the photosphere can be obtained indirectly. For that purpose only the Unno equations, a triplet Zeeman pattern, a longitudinal magnetic field and a two-component model are needed. The method was aplied to some Fourier transform spectrometer data (Stenfio et al., 1984) with promising results. As the absolute continuum intensities are unknown, rendering inaccurate the evaluation of the filling factor and the continuum contrast, only the standardized profile is obtained. (author). 2 figs., 12 refs