  We present phase-resolved optical spectroscopy and CCD photometry of the
faint eclipsing polar EP Dra (H1907+690). A revised ephemeris is derived which
connects all 32000 binary cycles since its discovery by Remillard et al.
(1991). We found no difference between spin and and orbital periods of the
white dwarf. Changes in the light curve morphology are attributed to a
different beaming behaviour which might change on timescales as short as one or
several orbital periods. Optical light curve modelling was used to estimate the
co-latitude of the accretion spot, which must be larger than 40 degrees. We
have detected Zeeman absorption lines of Halpha originating in an accretion
halo in a field of 16MG. The low-resolution spectra reveal no indication of
resolved cyclotron harmonics, which is also suggestive of a relatively low
field strength in the accretion region. The Balmer emission lines contain
significant contributions from the UV-illuminated hemisphere of the companion
star, whereas the HeII4686 emission originates predominantly from the accretion
stream. The emission lines have a multi-component structure and we could single
out a narrow emission line in the Hbeta and Hgamma lines. Its radial velocity
amplitude suggests a low mass for the white dwarf, if the lines are interpreted
as being of reprocessed origin from the whole illuminated hemisphere of the
companion star.
