Relativistic Simulations of Eccentric Binary Neutron Star Mergers: One-arm Spiral Instability and Effects of Neutron Star Spin

TL;DR

This study uses relativistic hydrodynamical simulations to explore how neutron star spins influence binary merger outcomes, ejecta, and gravitational wave signals, revealing the emergence of a one-arm spiral instability in some cases.

Contribution

It demonstrates the significant impact of neutron star spin on merger dynamics, ejecta, and gravitational wave signatures, including the development of a one-arm spiral instability.

Findings

Neutron star spin affects the likelihood of black hole formation post-merger.

Moderate spins increase ejecta mass and velocities, enhancing electromagnetic signals.

The one-arm spiral instability can develop in hypermassive neutron stars, aiding gravitational wave detection.

Abstract

We perform general-relativistic hydrodynamical simulations of dynamical capture binary neutron star mergers, emphasizing the role played by the neutron star spin. Dynamical capture mergers may take place in globular clusters, as well as other dense stellar systems, where most neutron stars have large spins. We find significant variability in the merger outcome as a function of initial neutron star spin. For cases where the spin is aligned with the orbital angular momentum, the additional centrifugal support in the remnant hypermassive neutron star can prevent the prompt collapse to a black hole, while for antialigned cases the decreased total angular momentum can facilitate the collapse to a black hole. We show that even moderate spins can significantly increase the amount of ejected material, including the amount unbound with velocities greater than half the speed of light, leading to brighter electromagnetic signatures associated with kilonovae and interaction of the ejecta with the interstellar medium. Furthermore, we find that the initial neutron star spin can strongly affect the already rich phenomenology in the postmerger gravitational wave signatures that arise from the oscillation modes of the hypermassive neutron star. In several of our simulations, the resulting hypermassive neutron star develops the one-arm ($m=1$) spiral instability, the most pronounced cases being those with small but non-negligible neutron star spins. For long-lived hypermassive neutron stars, the presence of this instability leads to improved prospects for detecting these events through gravitational waves, and thus may give information about the neutron star equation of state.