{
  "id": "2010.07796",
  "version": "v1",
  "published": "2020-10-15T14:40:08.000Z",
  "updated": "2020-10-15T14:40:08.000Z",
  "title": "FRB 181112 as a Rapidly-Rotating Massive Neutron Star just after a Binary Neutron Star Merger?: Implications for Future Constraints on Neutron Star Equations of State",
  "authors": [
    "Shotaro Yamasaki",
    "Tomonori Totani",
    "Kenta Kiuchi"
  ],
  "comment": "9 pages, 3 figures; submitted to ApJL",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "The light curve of the fast radio burst (FRB) 181112 is resolved into four successive pulses, and the time interval ($\\sim0.8$ ms) between the first and third pulses coincides with that between the second and fourth pulses, which can be interpreted as a neutron star (NS) spinning at a period of about $0.8$ ms. Although this period is shorter than the most rapidly rotating pulsar currently known ($1.4$ ms), it is typical for a simulated massive NS formed immediately after the coalescence of binary neutron stars (BNS). Therefore, a BNS merger is a good candidate for the origin of this FRB if the periodicity is real. We discuss the future implications that can be obtained if such a periodicity is detected from FRBs simultaneously with gravitational waves (GW). The remnant spin period $P_{\\rm rem}$ inferred from the FRB observation is unique information which is not readily obtained by current GW observations at the post-merger phase. If combined with the mass of the merger remnant $M_{\\rm rem}$ inferred from GW data, it would set a new constraint on the equation of state of nuclear matter. Furthermore, the post-merger quantity $P_{\\rm rem}/M_{\\rm rem}$, or the tidal deformability of the merger remnant, is closely related to the binary tidal deformability parameter $\\Lambda$ of NSs before they merge, and a joint FRB-GW observation will establish a new limit on $\\Lambda$. Thus, if $\\Lambda$ is also well measured by GW data, a comparison between these two will provide further insights into the nature of nuclear matter and BNS mergers.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2020-10-15T14:40:08.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "binary neutron star merger",
      "rapidly-rotating massive neutron star",
      "neutron star equations",
      "implications",
      "constraint"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 9,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}