We perform long-term simulations of spinning binary neutron stars , with our highest dimensionless spin being \chi \sim 0.32 .
To assess the importance of spin during the inspiral we vary the spin , and also use two equations of state , one that consists of plain nuclear matter and produces compact stars ( SLy ) , and a hybrid one that contains both nuclear and quark matter and leads to larger stars ( ALF2 ) .
Using high resolution that has grid spacing \Delta x \sim 98 m on the finest refinement level , we find that the effects of spin in the phase evolution of a binary system can be larger than the one that comes from tidal forces .
Our calculations demonstrate explicitly that although tidal effects are dominant for small spins ( \lesssim 0.1 ) , this is no longer true when the spins are larger , but still much smaller than the Keplerian limit .