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Eccentric Signatures of Stellar-Mass Binary Black Holes with Circumbinary Disks in LISA

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arxiv 2407.03869 v3 pith:L5PVUWB7 submitted 2024-07-04 astro-ph.HE gr-qc

Isobel M. Romero-Shaw , Samir Goorachurn , Magdalena Siwek , Christopher J. Moore This is my paper · ORCID
classification astro-ph.HEgr-qc
keywords binaryblackholesevolutionstellar-massdisksbinarieslisa
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abstract

Stellar-mass binary black holes may have circumbinary disks if formed through common-envelope evolution or within gaseous environments. Disks can drive binaries into wider and more eccentric orbits, while gravitational waves harden and circularise them. We combine cutting-edge evolution prescriptions for disk-driven binaries with well-known equations for gravitational-wave-driven evolution, and study the evolution of stellar-mass binary black holes. We find that binaries are driven by their disk to an equilibrium eccentricity, $0.2\lesssim e_\mathrm{eq} \lesssim0.5$, that dominates their evolution. Once they transition to the GW-dominated regime their eccentricity decreases rapidly; we find that stellar-mass binary black holes with long-lived disks will likely be observed in LISA with detectable eccentricities $\sim 10^{-2}$ at $0.01$ Hz, with the precise value closely correlating with the binary's initial mass ratio. This may lead stellar-mass binary black holes with CBDs observed in LISA to be confused with dynamically-formed binary black holes.

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Cited by 3 Pith papers

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

  1. A parametrized test of general relativity for inspiralling eccentric binaries in LISA

    gr-qc 2026-08 conditional novelty 6.0 of 10

    For eccentric black-hole binaries observed by LISA, a parametrized deformation of the periastron-precession rate could be constrained to |δα|≲10^-4 at 90% credibility with the full-model template.

  2. Revisiting GW150914 with a non-planar, eccentric waveform model

    gr-qc 2025-05 conditional novelty 5.0 of 10

    Using a waveform model that includes both eccentricity and spin precession, the authors confirm GW150914 was a quasi-circular, slowly spinning black hole merger, with eccentricity below 0.08 at 15 Hz.

  3. Population Synthesis of Gravitational Wave Sources

    astro-ph.HE 2025-02 accept novelty 1.0 of 10

    A review of population synthesis: the codes, the environments, and the predicted rates and features of gravitational wave sources, with an emphasis on breaking degeneracies.

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