A polarization analysis of E-limb prominences on November 3, 1994 is presented. Photometry and data reduction of 24 prominence pictures based on IDL software and Stokes-vector presentation and applied to Ea emission resulted in an accuracy of 1-1.5% in determination of the polarization degree and of 1.5-2.0° in the polarization direction. Distributions of polarization degree (polarization images) for prominences and the "white light" corona are presented. A polarization degree of 25% for prominences and 10-25% for the nearby white light corona are found. The polarization direction is found to be tangential to the solar limb. It is noted that eclipse observations can provide a powerful method for deriving the magnetic field at high altitudes in the coronal volume.

Preliminary data reduction of the color index polarization wave experiment carried out in Brazil (Chapeco town) is described. Distributions of polarization degree (polarization images) in the range 1.1-1.6 R. are obtained by an algorithm developed on the basis of the Stokes vector presentation and IDL software. The polarization image of the ''quasi-white-light'' corona (summary of the blue and red spectral region emissions) is analyzed. On the average, no fitt is found with the van de Hulst model for the inner corona at heliographic latitudes of +/-45 degrees. The polarization degree reaches a plateau at 1.2-1.35 R..