The spin evolution of accreting and radio pulsars in binary systems
2018
Pulsars were first
discovered in 1967 and since then the population has grown and expanded over
several wavelengths. In this thesis three different X-ray pulsars and three
black widow radio pulsars and their evolution has been examined. The pulsars in
this work all show variability that was not expected of their type of sources,
e.g. the pulsar 2A 1822-371 is found to have an orbital period that is
expanding over time more than what is expected. We suggest this to be due to
the pulsar being a super Eddington source. Another part of the thesis uncovers
that the magnetic field may have a significant influence in the behavior of the
pulsars. Low magnetic field pulsars often show a correlation between their
pulse phase and their flux, whereas we find that this correlation is not
present in high magnetic field pulsars. This could mean that the hot spot,
where the pulsations origin, is not moving in high magnetic field pulsars but
could be moving in low magnetic field pulsars. The first black widow pulsars
discovered had unstable timing solutions, whereas the black widow pulsars in
this work all have stable timing solutions, and we look into possible
explanations to this difference.
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