Based on observations of the pulsar B0329+54 with the LPA telescope at the Pushchino Radio Astronomy Observatory, we show that the Faraday rotation of the polarization plane of the polarized part of the main pulse leads not only to the well-known frequency modulation of the signal intensity, but also to two new effects: (i) a periodic frequency modulation of the time of arrival of its peak at the antenna receiving a linearly polarized emission and (ii) a frequency–time drift of the emerging bands of signal minima and maxima in the main-pulse propagation time interval. The detection of these effects constrains the admissible schemes and mechanisms for the generation of a partially polarized emission and allows one not only to improve significantly the accuracy of determining the dispersion measure, but also to judge the relative shift of the profiles of the unpolarized and linearly polarized parts of the main pulse as well as their asymmetry and steepness for pulsars with a large rotation measure. Under certain conditions, using such effects, it is possible to obtain information about the geometry and motion of the emission sources in pulsar magnetospheres and about the rotation of the polarization plane of the main pulse, which, in particular, can reveal a shear of neutron-star magnetic field lines in the regions of generation and limiting polarization of radiation.
Vdovin et al. (Wed,) studied this question.