The mapping of the polarized light over the surface of Venus is examined. An upper haze layer at a 70 km altitude does not extend in latitude up to the poles, and temporary patches of anomalous polarization denote particle size variations that are not related to the clouds observed in UV. Variations of polarization directions may involve filamentary structures in the cloud configurations. The overall altitude of the cloud top layer and global increases of altitude are discussed, and it was shown that above the two polar regions, the altitude of the upper cloud layer is depressed by an amount variable with time by typically of the order of 3 to 5 km. The particle radius in these regions is variable with years, ranging from 0.75 to 1.65 microns, and these size variations involve the two poles approximately similarly.
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Dollfus et al. (1979) studied this question.