Relationship between polarization and intensity of the green line in different coronal structures

The effect of anticorrelation between the polarization and intensity of the coronal green line Fe XIV 530.3 nm, revealed by the July 11, 1991 eclipse observations, is investigated. To simplify the general character of this ef fect, we have created the diagrams p versus log I-lambda for the points ins ide a narrow ring, at fixed distances from the solar disk centre. In this c ase, the global anticorrelation dependence disintegrated into two branches with 'a void zone' between them. The subsequent analysis has shown that the points, corresponding to the individual coronal structures of different ty pes, are clustered in specific places of the diagram. While the upper branc h is related to the huge high-latitude streamers, the lower branch contains the equatorial coronal condensations of different brightness. These branch es are best evident at the distance similar to 1.2 R., and they vary with t he distance from the disk centre. Model calculations, performed within the scope of generally accepted concepts, cannot explain the observed peculiari ties of the anticorrelation dependence, in particular, the presence of the gap between the two branches. The way out of these difficulties could be so ught in assuming that the coronal magnetic held affects the generation of t he polarized radiation in the emission green line.