Speaker
Jaroslaw Dyks
(Copernicus Astronomical Center)
Description
Observed radio pulsar polarization exhibits a range of complicated phenomena which
cannot be explained by the rotating vector model. These
include strong distortions of a polarization angle curve and high levels of
circular polarization V. Properties of the circular polarization are quite
peculiar: V tends to peak in coincidence with orthogonal
mode transitions, and can have both signs within the same (single) orthogonal
polarization mode. All these properties can be interpreted in terms of
empirical model in which the observed polarization results from coherent addition of
orthogonal polarization modes. The main model parameter is the relative phase lag
and the amplitude ratio of the interacting modal waves. I will show what are the model's
generic predictions for the pulsar polarization, and how these results compare with the well-known
observations of complex pulsar polarization, e.g. the core-component polarization of B1237+25.
Primary author
Jaroslaw Dyks
(Copernicus Astronomical Center)
