Detectability of gravitational wave events by spherical resonant-mass antennas

TL;DR

This paper evaluates the potential of spherical resonant-mass antennas to detect gravitational waves from neutron star mergers and stellar instabilities, showing promising detection distances with upcoming technology.

Contribution

It provides calculated signal-to-noise ratios for spherical antennas detecting specific gravitational wave sources, highlighting their future detection capabilities.

Findings

Detect neutron star inspirals up to 15 Mpc

Detect stellar instabilities up to 2 Mpc

Uses technology feasible in the next few years

Abstract

We have calculated signal-to-noise ratios for eight spherical resonant-mass antennas interacting with gravitational radiation from inspiralling and coalescing binary neutron stars and from the dynamical and secular bar-mode instability of a rapidly rotating star. We find that by using technology that could be available in the next several years, spherical antennas can detect neutron star inspiral and coalescence at a distance of 15 Mpc and the dynamical bar-mode instability at a distance of 2 Mpc.