Stochastic gravitational wave background due to core collapse resulting in neutron stars

TL;DR

This paper models the stochastic gravitational wave background from core-collapse supernovae, fitting energy spectra from simulations and assessing detectability with current and future detectors.

Contribution

It introduces a simplified multi-peak waveform model for gravitational waves from core collapse, aligning with simulation data and evaluating detector sensitivities.

Findings

Maximum energy density around 650 Hz is ~10^{-12}.

Current detectors need increased sensitivity to detect the background.

Model fits various core-collapse scenarios from simulations.

Abstract

The stochastic background of gravitational wave signals arising from the core-collapse supernovae is produced through various complex mechanisms that need detailed and careful investigation. We proposed a simplified multi-peak waveform of the amplitude spectrum. The corresponding energy spectra of our model fit the energy spectra obtained from different numerical simulations of various types of core-collapse events such as non-rotating, slow and fast rotating massive progenitors resulting in neutron stars. The maximum dimensionless energy density $\Omega_{gw}$ corresponding to our model is of $\mathcal{O}(10 {^{-12})} $ around 650 Hz. Assuming some degree of uncertainty, we estimated the parameters for the core collapse waveform using BILBY. We studied the detectability of the signal of our model against gravitational-wave detectors like the Einstein Telescope, advanced LIGO and Virgo. Our study indicates that these detectors have to gain more sensitivity to pick up the gravitational wave signals of stochastic background.