  We continue our study of the binary neutron star parameter space by
investigating the effect of the spin orientation on the dynamics, gravitational
wave emission, and mass ejection during the binary neutron star coalescence. We
simulate seven different configurations using multiple resolutions to allow a
reasonable error assessment. Due to the particular choice of the setups, five
configurations show precession effects, from which two show a precession
("wobbling") of the orbital plane, while three show a "bobbing" motion, i.e.,
the orbital angular momentum does not precess, while the orbital plane moves
along the orbital angular momentum axis. Considering the ejection of mass, we
find that precessing systems can have an anisotropic mass ejection, which could
lead to a final remnant kick of $\sim 40 \rm km/s$ for the studied systems.
Furthermore, for the chosen configurations, antialigned spins lead to larger
mass ejecta than aligned spins, so that brighter electromagnetic counterparts
could be expected for these configurations. Finally, we compare our simulations
with the precessing, tidal waveform approximant IMRPhenomPv2_NRTidalv2 and find
good agreement between the approximant and our numerical relativity waveforms
with phase differences below 1.2 rad accumulated over the last $\sim$ 16
gravitational wave cycles.
