Towards observing the neutron star collapse with gravitational wave detectors

TL;DR

This paper explores how advanced gravitational wave detectors could observe neutron star collapse post-merger, either indirectly through emission shut-off or directly via collapse signals, to better understand neutron star physics and gamma-ray bursts.

Contribution

It proposes novel detector designs optimized for observing neutron star collapse signals, enhancing the potential to study post-merger dynamics.

Findings

High-frequency detector could detect collapse signals at 50 Mpc with SNR 0.5-8.6

Narrow-band detector could achieve SNR 0.3-1.9 for direct collapse detection

Detector designs are limited by classical and quantum noise at high power levels

Abstract

Gravitational waves from binary neutron star inspirals have been detected along with the electromagnetic transients coming from the aftermath of the merger in GW170817. However, much is still unknown about the post-merger dynamics that connects these two sets of observables. This includes if, and when, the post-merger remnant star collapses to a black hole, and what are the necessary conditions to power a short gamma-ray burst, and other observed electromagnetic counterparts. Observing the collapse of the post-merger neutron star would shed led on these questions, constraining models for the short gamma-ray burst engine and the hot neutron star equation of state. In this work, we explore the scope of using gravitational wave detectors to measure the timing of the collapse either indirectly, by establishing the shut-off of the post-merger gravitational emission, or---more challengingly---directly, by detecting the collapse signal. For the indirect approach, we consider a kilohertz high-frequency detector design that utilises a previously studied coupled arm cavity and signal recycling cavity resonance. This design would give a signal-to-noise ratio of 0.5\,-\,8.6 (depending on the variation of waveform parameters) for a collapse gravitational wave signal occurring at 10\,ms post-merger of a binary at 50\,Mpc and with total mass $2.7 M_\odot$. For the direct approach, we propose a narrow-band detector design, utilising the sensitivity around the frequency of the arm cavity free spectral range. The proposed detector achieves a signal-to-noise ratio of 0.3\,-\,1.9, independent of the collapse time. This detector is limited by both the fundamental classical and quantum noise with the arm cavity power chosen as 10\,MW.