Numerical-relativity simulations of long-lived remnants of binary neutron star mergers
R. De Pietri, Alessandra Feo, José A. Font, Frank Löffler, Michele Pasquali, Nikolaos Stergioulas
Abstract
We analyze the properties of the gravitational wave signal emitted after the merger of a binary neutron star system when the remnant survives for more than a 80 ms (and up to 140 ms). We employ four different piecewise polytropic equations of state supplemented by an ideal fluid thermal component. We find that the postmerger phase can be subdivided into three phases: an early postmerger phase (where the quadrupole mode and a few subdominant features are active), the intermediate postmerger phase (where only the quadrupole mode is active) and the late postmerger phase (where convective instabilities trigger inertial modes). The inertial modes have frequencies somewhat smaller than the quadrupole modes. In one model, we find an interesting association of a corotation of the quadrupole mode in parts of the star with a revival of its amplitude. The gravitational wave emission of inertial modes in the late postmerger phase is concentrated in a narrow frequency region and is potentially detectable by the planned third-generation detectors. This allows for the possibility of probing not only the cold part of the equation of state, but also its dependence on finite temperature. In view of these results, it will be important to investigate the impact of various type of viscosities on the potential excitation of inertial modes in binary neutron star merger remnants.