Evolutions of eccentric binary neutron stars with improved initial data

We describe the first evolutions of eccentric binary neutron stars using initial data constructed with a new method that solves the Einstein constraints and Euler equation self-consistently, which previously had only been done in the quasicircular case. We show that these data indeed lead to considerable improvement in the initial spurious oscillation of the neutron stars, compared with the superposed data used in previous evolutions. We also consider the convergence of the constraints, the gravitational wave signal (including the tidally induced oscillations), and the properties of the final remnant and ejecta, again comparing the evolutions of the new data with those of the old, superposed data.