Detectability of stochastic gravitational wave background from weakly hyperbolic encounters

Abstract

We compute the stochastic gravitational wave (GW) background generated by black hole-black hole (BH-BH) hyperbolic encounters with eccentricities close to one and compare them with the respective sensitivity curves of planned GW detectors. We use the Keplerian potential to model the orbits of the encounters and the quadrupole formula to compute the emitted GWs. We take into account hyperbolic encounters that take place in clusters up to redshift $5$ and with BH masses spanning from $5M_{\odot }$ to $55M_{\odot }$. We assume the clusters to be virialized and study several cluster models with different mass and virial velocity, and finally obtain an accumulative result, displaying the background as an average. Using the maxima and minima of our accumulative result for each frequency, we provide analytical expressions for both optimistic and pessimistic scenarios. Our results suggest that the background from these encounters is likely to be detected by the third-generation detectors Cosmic explorer and Einstein telescope, while the tail section at lower frequencies intersects with DECIGO, making it a potential target source for both ground- and space-based future GW detectors.

8 pages, 3 figures, 1 table

References in corpus (6)

• Exploring the Sensitivity of Next Generation Gravitational Wave Detectors
• The NANOGrav 15-year Data Set: Constraints on Supermassive Black Hole Binaries from the Gravitational Wave Background
• Detection Rate Estimates of Gravity-waves Emitted During Parabolic Encounters of Stellar Black Holes in Globular Clusters
• Gravitational wave energy spectrum of hyperbolic encounters
• Simultaneous estimation of astrophysical and cosmological stochastic gravitational-wave backgrounds with terrestrial detectors
• A note on the gravitational wave energy spectrum of parabolic and hyperbolic encounters

Cited by in corpus (8)

• The Science of the Einstein Telescope
• Challenges and Opportunities of Gravitational Wave Searches above 10 kHz
• Evolution of a black hole cluster in full general relativity
• Spin induction from scattering of two spinning black holes in dense clusters
• Mass octupole and current quadrupole corrections to gravitational wave emission from close hyperbolic encounters
• Compact Binary Coalescence Gravitational Wave Signals Counting and Separation
• Spin-up and mass-gain in hyperbolic encounters of spinning black holes
• Detecting stochastic gravitational wave background from cosmic strings with next-generation detector networks: Component separation based on a multi-source astrophysical foreground noise model