  Heavy elements like gold, platinum or uranium are produced in the r-process,
which needs neutron-rich and explosive environments. Neutron star mergers are a
promising candidate for an r-process site. They exhibit three different
channels for matter ejection fulfilling these conditions: dynamic ejecta due to
tidal torques, neutrino-driven winds and evaporating matter from the accretion
disk. We present a first study of the integrated nucleosynthesis for a
neutrino-driven wind from a neutron star merger with a hyper-massive neutron
star. Trajectories from a recent hydrodynamical simulation are divided into
four different angle regions and post-processed with a reaction network. We
find that the electron fraction varies around $Y_e \approx 0.1 - 0.4$, but its
distribution differs for every angle of ejection. Hence, the wind ejecta do not
undergo a robust r-process, but rather possess distinct nucleosynthesis yields
depending on the angle range. Compared to the dynamic ejecta, a smaller amount
of neutron-rich matter gets unbound, but the production of lighter heavy
elements with $A \lesssim 130$ in the neutrino-driven wind can complement the
strong r-process of the dynamic ejecta.
