The Gravitational Wave Background From Coalescing Compact Binaries: A New Method

TL;DR

This paper introduces a novel method to estimate the stochastic gravitational wave background produced by coalescing compact binaries, aiding future detection efforts by characterizing the superimposed signals from neutron star and black hole systems.

Contribution

The paper presents a new approach to calculate the gravitational wave background from binary coalescences, improving upon previous models and enabling better predictions for upcoming detectors.

Findings

Developed a new method for background estimation

Applied the method to neutron star and black hole binaries

Provided predictions for future gravitational wave detectors

Abstract

Gravitational waves are perturbations in the spacetime that propagate at the speed of light. The study of such phenomenon is interesting because many cosmological processes and astrophysical objects, such as binary systems, are potential sources of gravitational radiation and can have their emissions detected in the near future by the next generation of interferometric detectors. Concerning the astrophysical objects, an interesting case is when there are several sources emitting in such a way that there is a superposition of signals, resulting in a smooth spectrum which spans a wide range of frequencies, the so-called stochastic background. In this paper, we are concerned with the stochastic backgrounds generated by compact binaries (i.e. binary systems formed by neutron stars and black holes) in the coalescing phase. In particular, we obtain such backgrounds by employing a new method developed in our previous studies.