{
  "id": "2407.03869",
  "version": "v1",
  "published": "2024-07-04T12:06:14.000Z",
  "updated": "2024-07-04T12:06:14.000Z",
  "title": "Eccentric Signatures of Stellar-Mass Binary Black Holes with Circumbinary Disks in LISA",
  "authors": [
    "Isobel M. Romero-Shaw",
    "Samir Goorachurn",
    "Magdalena Siwek",
    "Christopher J. Moore"
  ],
  "comment": "7 pages, 3 figures. Submitted to MNRAS Letters. Comments welcome!",
  "categories": [
    "astro-ph.HE",
    "gr-qc"
  ],
  "abstract": "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 binaries 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 binary black holes with CBDs observed in LISA to be confused with dynamically-formed binary black holes.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2024-07-04T12:06:14.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "stellar-mass binary black holes",
      "circumbinary disks",
      "eccentric signatures",
      "binarys initial mass ratio",
      "eccentricity"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 7,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}