High-resolution calculations of merging neutron stars - I. Model description and hydrodynamic evolution
We present the results of 3D high-resolution calculations of the last inspiral stages and the final coalescence of neutron star binary systems. The equations of hydrodynamics are solved using the smoothed particle hydrodynamics method with up to 106 particles. Using Newtonian gravity, but adding the forces emerging from the emission of gravitational waves, we focus on the impact of microphysics on