  Pulsar glitches are rapid spin-up events that occur in the rotation of
neutron stars, providing a valuable probe into the physics of the interiors of
these objects. Long-term monitoring of a large number of pulsars facilitates
the detection of glitches and the robust measurements of their parameters. The
Jodrell Bank pulsar timing programme regularly monitors more than 800 radio
pulsars and has accrued, in some cases, over 50 years of timing history on
individual objects. In this paper we present 106 new glitches in 70 radio
pulsars as observed up to the end of 2018. For 70% of these pulsars, the event
we report is its only known glitch. For each new glitch we provide measurements
of its epoch, amplitude and any detected changes to the spin-down rate of the
star. Combining these new glitches with those listed in the Jodrell Bank glitch
catalogue we analyse a total sample of 543 glitches in 178 pulsars. We model
the distribution of glitch amplitudes and spin-down rate changes using a
mixture of two Gaussian components. We corroborate the known dependence of
glitch rate and activity on pulsar spin-down rates and characteristic ages, and
show that younger pulsars tend to exhibit larger glitches. Pulsars whose
spin-down rates between $10^{-14}$ Hz s$^{-1}$ and $10^{-10.5}$ Hz s$^{-1}$
show a mean reversal of 1.8% of their spin-down as a consequence of glitches.
Our results are qualitatively consistent with the superfluid vortex unpinning
models of pulsar glitches.
