The continuum contrast between fluxtubes and their quiet background, and the magnetic řlux carried by these magnetic elements, have been determined at different points of a solar facula, In the frame of a
two-component model from spectropolarimetric observations of 1^11 spatial resolution. Local spatial variations of these two parameters have been obtained.
High resolution (better than 1") magnetograms obtained at the Sacramento Peak Vacuum Tower Telescope were used to study the decay of a small active region. The reduction process allows one to match intensity and magnetic pictures exactly. Some of the main results are; (i) The granulation massages a magnetic pore, probably inducing its fragmentation. The supergranules get rid of the decayed pieces transporting them away from the pere. (ii) Magnetic flux is removed from the photosphere through its submergence.
Here we presant a method for reconstructing the intensity profile, I, formed in tho magnetic elements which have diameters smaller than the best presently achlevable spatial resolutlon. It follows the same line as In Solankl and Stenflo (1984). As a starting point we use I and V (fourth Stokes parameter, whIch originates oniy In magnetic reglons) of the facula and the I observed In the quiet Sun. The filling factor, and the ratio between the continuum intensity of the magnetic and non-magnetic parts of the photosphere can be obtalned Indlrectly. For that purpose onIy the Unno equatlons, a triplet Zeeman pattern, a longitudinal magnetic field and a
two-component model are needed. The method has been applied to some Fourier transform spectrometer (FTS) data (Stenflo et al., 1984) wlth promlsing results. As the absolute continuum intensities are unknown, rendering inaccurate the evaluatlon of the filling factor and the continuum contrast, oniy the normalised I profile Is obtained.
Preliminary results of a search for the variation of the solar granulation properties with the heliographic laitude are presented. Within errors, no changes are found in the power spectra and sizes between N-S and E-W scans.