  We present a comprehensive nucleosynthesis study of the neutrino-driven wind
in the aftermath of a binary neutron star merger. Our focus is the initial
remnant phase when a massive central neutron star is present. Using tracers
from a recent hydrodynamical simulation, we determine total masses and
integrated abundances to characterize the composition of unbound matter. We
find that the nucleosynthetic yields depend sensitively on both the life time
of the massive neutron star and the polar angle. Matter in excess of up to $9
\cdot 10^{-3} M_\odot$ becomes unbound until $\sim 200~{\rm ms}$. Due to
electron fractions of $Y_{\rm e} \approx 0.2 - 0.4$ mainly nuclei with mass
numbers $A < 130$ are synthesized, complementing the yields from the earlier
dynamic ejecta. Mixing scenarios with these two types of ejecta can explain the
abundance pattern in r-process enriched metal-poor stars. Additionally, we
calculate heating rates for the decay of the freshly produced radioactive
isotopes. The resulting light curve peaks in the blue band after about $4~{\rm
h}$. Furthermore, high opacities due to heavy r-process nuclei in the dynamic
ejecta lead to a second peak in the infrared after $3-4~{\rm d}$.
