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Our previous paper outlined the general aspects of the theory of radio lightcurve and polarization formation for pulsars. We predicted the one-to-onecorrespondence between the tilt of the linear polarization position angle ofthe and the circular polarization. However, some of the radio pulsars indicatea clear deviation from that correlation. In this paper we apply the theory ofthe radio wave propagation in the pulsar magnetosphere for the analysis ofindividual effects leading to these deviations. We show that within our theorythe circular polarization of a given mode can switch its sign, without the needto introduce a new radiation mode or other effects. Moreover, we show that thegeneration of different emission modes on different altitudes can explainpulsars, that presumably have the X-O-X light-curve pattern, different fromwhat we predict. General properties of radio emission within our propagationtheory are also discussed. In particular, we calculate the intensity patternsfor different radiation altitudes and present light curves for differentobserver viewing angles. In this context we also study the light curves andpolarization profiles for pulsars with interpulses. Further, we explain thecharacteristic width of the position angle curves by introducing the concept ofa wide emitting region. Another important feature of radio polarizationprofiles is the shift of the position angle from the center, which in somecases demonstrates a weak dependence on the observation frequency. Here wedemonstrate that propagation effects do not necessarily imply a significantfrequency-dependent change of the position angle curve.

On the mean profiles of radio pulsars II: Reconstruction of complex pulsar light-curves and other new propagation effects