  Our previous paper outlined the general aspects of the theory of radio light
curve and polarization formation for pulsars. We predicted the one-to-one
correspondence between the tilt of the linear polarization position angle of
the and the circular polarization. However, some of the radio pulsars indicate
a clear deviation from that correlation. In this paper we apply the theory of
the radio wave propagation in the pulsar magnetosphere for the analysis of
individual effects leading to these deviations. We show that within our theory
the circular polarization of a given mode can switch its sign, without the need
to introduce a new radiation mode or other effects. Moreover, we show that the
generation of different emission modes on different altitudes can explain
pulsars, that presumably have the X-O-X light-curve pattern, different from
what we predict. General properties of radio emission within our propagation
theory are also discussed. In particular, we calculate the intensity patterns
for different radiation altitudes and present light curves for different
observer viewing angles. In this context we also study the light curves and
polarization profiles for pulsars with interpulses. Further, we explain the
characteristic width of the position angle curves by introducing the concept of
a wide emitting region. Another important feature of radio polarization
profiles is the shift of the position angle from the center, which in some
cases demonstrates a weak dependence on the observation frequency. Here we
demonstrate that propagation effects do not necessarily imply a significant
frequency-dependent change of the position angle curve.

High Energy Astrophysical Phenomena