The measurements by Brfickner (1963) of the Ca 1 4227 polarization at the Sun's limb provides us with a test for the theory of line polarization. Computations are developed taking into account: (a) the transfer polarization, due to the anisotropy of radiation field; (b) the depolarizing collisions acting in the wings. The magnetic field is not taken into account and the theory is not valid in the Doppler core. In the wings a very good fit is obtained, using appropriate source-functions fitting the observed profiles at the center of the disk, and from center to limb.

Si IV, C IV, and O vI resonance lines have been measured above quiet and active solar regions from both pointed OSO-8 instruments. From calibrated profiles, optical depths are computed with three different methods. All three methods provide evidence that the opacity above faculae is lower than above the quiet Sun.From lower and upper limits of the opacity, we derive limits of the electron density. Our first method assumes only that the source function is constant without any geometrical constraint. We find higher densities above faculae than above quiet regions (about a factor 10). A second method allows us to compute the density, temperature gradient and thickness of a plane-parallel model, for active and quiet Sun. Electron densities agree with those of the first method but they lie in the lower range of values previously determined from Skylab. This result can be explained by the moderate level activity of the observed faculae.Appendices give relevant elements of transfer theory and newly computed values of collisional rates.

This paper reviews the motivations and the principles of the measurements which aim at a systematic exploration, from photosphere to corona, of the facular regions (plages). The sequence of observation actually achieved is described. Preliminary results are given, in a purely indicative way. Detailed analyses will be made in further papers.

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