Binary neutron star merger simulations with different initial orbital frequency and equation of state

Understand

We present results from three-dimensional general relativistic simulations of binary neutron star coalescences and mergers using public codes.

• We considered equal mass models where the baryon mass of the two Neutron Stars (NS) is $1.4M_{\odot}$, described by four different equations of state (EOS) for the cold nuclear matter (APR4, SLy, H4, and MS1; all parametrized as piecewise polytropes).
• We started the simulations from four different initial interbinary distances ($40, 44.3, 50$, and $60$ km), including up to the last 16 orbits before merger.
• That allows to show the effects on the gravitational wave phase evolution, radiated energy and angular momentum due to: the use of different EOSs, the orbital eccentricity present in the initial data and the initial separation (in the simulation) between the two stars.