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We present general relativistic numerical simulations of binary neutron star(BNS) mergers with different initial spin configurations. We focus on modelswith stars of mass 1.4 M_sol each, which employ the equation of state (EOS) byShen, Horowitz, and Teige, and which result in stable NSs as merger remnants.For comparison, we consider two irrotational equal mass (M=1.35 M_sol) andunequal mass (M=1.29,1.42 M_sol) BNS models using the APR4 EOS, which result ina supramassive merger remnant. We present visualizations of the fluid flow andtemperature distribution and find a strong impact of the spin on vortexstructure and nonaxisymmetric deformation. We compute the radial massdistribution and the rotation profile in the equatorial plane using recentlydeveloped measures independent of spatial gauge, revealing slowly rotatingcores that can be well approximated by the cores of spherical stars. We alsostudy the influence of the spin on the inspiral phase and the gravitationalwave (GW) signal. Using a newly developed analysis method, we further show thatgravitational waveforms from BNS mergers can exhibit one or more phase jumpsafter merger, which occur together with minima of the strain amplitude. Weprovide a natural explanation in terms of the remnant's quadrupole moment, andshow that cancellation effects due to phase jumps can have a strong impact onthe GW power spectrum. Finally, we discuss the impact of the spin on the amountof ejected matter.

Structure of Stable Binary Neutron Star Merger Remnants: Role of Initial Spin