Speaker
Description
Using the data from FAST and MeerKAT radio telescope surveys, we carried out a detailed statistical analysis of the distributions of the observed widths of mean radio pulsar profiles. The availability of the high-quality polarization data made it possible to separately consider mean profiles formed by the ordinary (O) and extraordinary (X) orthogonal polarization modes. We performed an analysis of the dependency of the profile widths on pulsar periods, which revealed statistically significant differences between the O and X mode profiles subsamples. It was shown that the pulsar profiles, formed by the O mode are on average wider than the profiles, formed by the X mode, which can be explained by the O mode refraction in pulsar magnetosphere. Thus, we have statistically confirmed the main theoretical predictions regarding orthogonal modes propagation, using large and homogeneous data sample.