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The remnant of neutron star mergers is dense in neutrinos. By employinginputs from one hydrodynamical simulation of a binary neutron star mergerremnant with a black hole of $3\ M_\odot$ in the center, dimensionless spinparameter $0.8$ and an accretion torus of $0.3\ M_\odot$, the neutrino emissionproperties are investigated as the merger remnant evolves. Initially, the localnumber density of $\bar{\nu}_e$ is larger than that of $\nu_e$ everywhere abovethe remnant. Then, as the torus approaches self-regulated equilibrium, thelocal abundance of neutrinos overcomes that of antineutrinos in a funnel aroundthe polar region. The region where the fast pairwise flavor conversions canoccur shrinks accordingly as time evolves. Still, we find that fast flavorconversions do affect most of the neutrino-driven ejecta. Assuming that fastflavor conversions lead to flavor equilibration, a significant enhancement ofnuclei with mass numbers $A>130$ is found as well as a change of the lanthanidemass fraction by more than a factor of a thousand. Our findings hint towards apotentially relevant role of neutrino flavor oscillations for the prediction ofthe kilonova (macronova) lightcurves and motivate further work in thisdirection.

Imprints of neutrino-pair flavor conversions on nucleosynthesis in ejecta from neutron-star merger remnants