Polarised radio emission from pulsars and the influenceof the magnetosphere
2019
Since the discovery of pulsars 50 years ago, a lot
of progress has been made in understanding how the radio emission
mechanism of pulsars works. Nevertheless, explaining the wealth of
observational phenomenology has proven difficult. In this thesis,
we investigated the radio polarisation properties of pulsars. It
has become clear that the propagation of radio emission in the
pulsar magnetosphere plays a major role in shaping the observed
radiation, especially where polarisation is considered. We started
by studying the time-dependence of radio polarisation by observing
the polarisation properties of individual pulses of PSR B0031-07, a
pulsar with multiple stable drift modes. Furthermore, using a
larger sample of 31 pulsars, we aimed to explore if it is common
for switches between orthogonal polarisation modes (OPMs) to be
linked to periodic intensity variability. Eleven pulsars in the
sample showed both a mixture of OPMs and drifting subpulses. Out of
these, nine showed synchronous switching of OPMs with the drifting
subpulses and for the remaining two pulsars we showed that the
drifting might well be too complex to reveal the link between
polarisation and the periodic intensity variations. So if the
pulsar has OPM switches, it is most likely linked to drifting
subpulses if present. This is argued to be a consequence of
propagation effects in the pulsar magnetosphere. Even if no
periodic intensity variations are observed, it was established that
changes in polarisation are coupled to variability in intensity.
The frequency dependence of radio polarisation was studied by
conducting the largest investigation to date into the origin of
phase resolved apparent rotation measure (RM) variations in the
polarised signals of 98 radio pulsars. A total of 42 pulsars showed
significant phase resolved apparent RM variations. Our results are
inconsistent with all variations being caused by interstellar
scattering. Instead, magnetospheric propagation is argued to be
important, and thus leaving a frequency dependent imprint in the
observed polarised radiation. Lastly, we investigated the
polarisation properties of three newly discovered pulsars from the
GMRT High Resolution Southern Sky Survey to get geometrical
information about the pulsar and its emission beams. We conclude
that the magnetic axis of PSR J0514-4407 is highly inclined with
respect to the rotation axis. This is consistent with what we would
expect given that is it a gamma-ray emitting
pulsar.
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