  Most population studies of pulsars have hitherto focused on the disc of the
Galaxy, the Galactic centre, globular clusters, and nearby galaxies. It is
expected that pulsars, by virtue of their natal kicks, are also to be found in
the Galactic halo. We investigate the possible population of canonical (i.e.
non-recycled) radio pulsars in the halo, estimating the number of such pulsars,
and the fraction that is detectable via single pulse and periodicity searches.
Additionally, we explore the distributions of flux densities and dispersion
measures of this population. We also consider the effects of different velocity
models and the evolution of inclination angle and magnetic field on our
results. We show that $\sim$33 % of all pulsars beaming towards the Earth are
in the halo but the fraction reduces to $\sim$1.5 % if we let the inclination
angle and the magnetic field evolve as a falling exponential. Moreover, the
fraction that is detectable is significantly limited by the sensitivity of
surveys. This population would be most effectively probed by surveys using
time-domain periodicity search algorithms. The current non-detections of
pulsars in the halo can be explained if we assume that the inclination angle
and magnetic field of pulsars evolve with time. We also highlight a possible
confusion between bright pulses from halo pulsars and Fast Radio Bursts with
low dispersion measures where further follow-up is warranted.
