Detectability of f-mode Unstable Neutron Stars by the Schenberg Spherical Antenna

TL;DR

This paper evaluates the potential of the Brazilian Schenberg spherical antenna to detect high-frequency gravitational waves from f-mode unstable neutron stars, estimating event rates and detection prospects.

Contribution

It provides the first detailed analysis of Schenberg's capability to detect GWs from f-mode unstable neutron stars and estimates relevant event rates.

Findings

Schenberg can potentially detect GWs from f-mode unstable neutron stars.

Estimated event rates suggest feasible detection within certain astrophysical scenarios.

The study compares detection prospects with the Dutch Mini-Grail antenna.

Abstract

The Brazilian spherical antenna (Schenberg) is planned to detect high frequency gravitational waves (GWs) ranging from 3.0 kHz to 3.4 kHz. There is a host of astrophysical sources capable of being detected by the Brazilian antenna, namely: core collapse in supernova events; (proto)neutron stars undergoing hydrodynamical instability; f-mode unstable neutron stars, caused by quakes and oscillations; excitation of the first quadrupole normal mode of 4-9 solar mass black holes; coalescence of neutron stars and/or black holes; exotic sources such as bosonic or strange matter stars rotating at 1.6 kHz; and inspiralling of mini black hole binaries. We here address our study in particular to the neutron stars, which could well become f-mode unstable producing therefore GWs. We estimate, for this particular source of GWs, the event rates that in principle can be detected by Schenberg and by the Dutch Mini-Grail antenna.