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

Understand

We present general relativistic numerical simulations of binary neutron star (BNS) mergers with different initial spin configurations.

• We focus on models with stars of mass 1.4 M_sol each, which employ the equation of state (EOS) by Shen, 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) and unequal mass (M=1.29,1.42 M_sol) BNS models using the APR4 EOS, which result in a supramassive merger remnant.
• We present visualizations of the fluid flow and temperature distribution and find a strong impact of the spin on vortex structure and nonaxisymmetric deformation.