  Based on high-resolution optical spectroscopy in the blue and the near
infra-red spectral range, we derived velocity images (Doppler tomograms) of the
mass-donating secondary star and the accretion stream of the long-period
eclipsing polar V1309 Ori (RX J0515.41+0104.6). Combined with HST-spectroscopy
of high time resolution and optical photometry we were able to derive the main
system parameters and to determine the accretion geometry of the binary. The
length of the eclipse of the white dwarf is Delta t_{ecl} = 2418 +/- 60 s, the
mass ratio Q = 1.37 - 1.63, and the orbital inclination i=76.6 - 78.9 degrees.
The surface of the secondary star could be resolved in the Doppler image of NaI
absorption lines, where it shows a marked depletion on the X-ray irradiated
side. The accretion geometry proposed by us with a nearly aligned rotator,
co-latitude delta ~ 10 degrees, tilted away from the ballistic stream, azimuth
chi ~ -35 degrees, explains the shape of the emission-line Doppler tomograms
and the shape of optical/UV eclipse light curves.
