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Stochastic Gravitational-Wave Background from Binary Black Holes and Binary Neutron Stars and Implications for LISA

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arxiv 1809.10360 v2 pith:6W7U6PFQ submitted 2018-09-27 gr-qc astro-ph.CO

Stochastic Gravitational-Wave Background from Binary Black Holes and Binary Neutron Stars and Implications for LISA

Zu-Cheng Chen , Fan Huang , Qing-Guo Huang This is my paper
classification gr-qc astro-ph.CO
keywords bbhsbinaryblacklisaholessgwbbnssbackground
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The advent of gravitational wave (GW) and multi-messenger astronomy has stimulated the research on the formation mechanisms of binary black holes (BBHs) observed by LIGO/Virgo. In literature, the progenitors of these BBHs could be stellar-origin black holes (sBHs) or primordial black holes (PBHs). In this paper we calculate the Stochastic Gravitational-Wave Background (SGWB) from BBHs, covering the astrophysical and primordial scenarios separately, together with the one from binary neutron stars (BNSs). Our results indicate that PBHs contribute a stronger SGWB than that from sBHs, and the total SGWB from both BBHs and BNSs has a high possibility to be detected by the future observing runs of LIGO/Virgo and LISA. On the other hand, the SGWB from BBHs and BNSs also contributes an additional source of confusion noise to LISA's total noise curve, and then weakens LISA's detection abilities. For instance, the detection of massive black hole binary (MBHB) coalescences is one of the key missions of LISA, and the largest detectable redshift of MBHB mergers can be significantly reduced.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Signal-to-Noise Ratio Contours for LISA

    gr-qc 2026-07 accept novelty 6.0

    LISA auto-correlation SNR equals the square root of T_obs times the integral of (signal/(noise+signal))^2 and is therefore bounded by sqrt(T_obs(f_max-f_min)).

  2. Effects of formation channels and gravitational lensing on stochastic gravitational wave background

    gr-qc 2026-05 unverdicted novelty 4.0

    Using HBI on GWTC-4 data the authors compute lensed SGWBs for ABHs and PBHs and conclude that LIGO and ET can distinguish the two formation channels in specific frequency ranges, with ET offering broader coverage.