  Accreting magnetic white dwarfs offer an opportunity to understand the
interplay between spin-up and spin-down torques in binary systems. Monitoring
of the white dwarf spin may reveal whether the white dwarf spin is currently in
a state of near-equilibrium, or of uni-directional evolution towards longer or
shorter periods, reflecting the recent history of the system and providing
constraints for evolutionary models. This makes the monitoring of the spin
history of magnetic white dwarfs of high interest. In this paper we report the
results of a campaign of follow-up optical photometry to detect and track the
39 sec white dwarf spin pulses recently discovered in Hubble Space Telescope
data of the cataclysmic variable V1460 Her. We find the spin pulsations to be
present in g-band photometry at a typical amplitude of 0.4%. Under favourable
observing conditions, the spin signal is detectable using 2-meter class
telescopes. We measured pulse-arrival times for all our observations, which
allowed us to derive a precise ephemeris for the white dwarf spin. We have also
derived an orbital modulation correction that can be applied to the
measurements. With our limited baseline of just over four years, we detect no
evidence yet for spin-up or spin-down of the white dwarf, obtaining a lower
limit of |P/Pdot|> 4e7 years, which is already 4 to 8 times longer than the
timescales measured in two other cataclysmic variable systems containing
rapidly rotating white dwarfs, AE Aqr and AR Sco.
