Impact of population III stars on the astrophysical gravitational-wave background

Nikolaos Kouvatsos; Mairi Sakellariadou

doi:10.1103/PhysRevD.110.023017

Impact of population III stars on the astrophysical gravitational-wave background

Nikolaos Kouvatsos, Mairi Sakellariadou

Research output: Contribution to journal › Article › peer-review

1 Citation (Scopus)

Abstract

We probe the astrophysical gravitational-wave background resulting from compact binary coalescences, focusing on population III binary black holes. We exploit results of state-of-the-art simulations on the evolution of population I-II and III binaries, considering a variety of initial condition and star formation rate models for the latter. The contribution from population III binary black holes is found to be very small, with no effect on the gravitational-wave spectrum. A network of third-generation detectors will detect easier individual population III binaries, due to their significantly higher masses, hence decreasing even further their residual contribution.

Original language	English
Article number	023017
Number of pages	10
Journal	Physical Review D
Volume	110
Issue number	2
DOIs	https://doi.org/10.1103/PhysRevD.110.023017
Publication status	Published - 12 Jul 2024

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10.1103/PhysRevD.110.023017

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abstract = "We probe the astrophysical gravitational-wave background resulting from compact binary coalescences, focusing on population III binary black holes. We exploit results of state-of-the-art simulations on the evolution of population I-II and III binaries, considering a variety of initial condition and star formation rate models for the latter. The contribution from population III binary black holes is found to be very small, with no effect on the gravitational-wave spectrum. A network of third-generation detectors will detect easier individual population III binaries, due to their significantly higher masses, hence decreasing even further their residual contribution.",

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AB - We probe the astrophysical gravitational-wave background resulting from compact binary coalescences, focusing on population III binary black holes. We exploit results of state-of-the-art simulations on the evolution of population I-II and III binaries, considering a variety of initial condition and star formation rate models for the latter. The contribution from population III binary black holes is found to be very small, with no effect on the gravitational-wave spectrum. A network of third-generation detectors will detect easier individual population III binaries, due to their significantly higher masses, hence decreasing even further their residual contribution.

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Impact of population III stars on the astrophysical gravitational-wave background

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