{
  "id": "1502.05740",
  "version": "v1",
  "published": "2015-02-19T22:33:41.000Z",
  "updated": "2015-02-19T22:33:41.000Z",
  "title": "Ultra-Close Encounters of Stars With Massive Black Holes: Tidal Disruption Events With Prompt Hyperaccretion",
  "authors": [
    "Christopher Evans",
    "Pablo Laguna",
    "Michael Eracleous"
  ],
  "comment": "5 pages, 1 table, 4 figures",
  "categories": [
    "astro-ph.GA",
    "astro-ph.HE",
    "gr-qc"
  ],
  "abstract": "A bright flare from a galactic nucleus followed at late times by a $t^{-5/3}$ decay in luminosity is often considered to be the signature of a tidal disruption of a star by a massive black hole. The flare and afterglow are produced when the stream of stellar debris released by the disruption returns to the vicinity of the black hole, self-intersects, and eventually forms an accretion disk or torus. In the canonical scenario of a solar-type star disrupted by a $10^{6}\\; M_\\odot$ black hole, the time between the disruption of the star and the formation of the accretion torus could be years. We present fully general relativistic simulations of a new class of tidal disruption events involving ultra-close encounters of solar-type stars with intermediate mass black holes. In these encounters, a thick disk forms promptly after disruption, on timescales of hours. After a brief initial flare, the accretion rate remains steady and highly super-Eddington for a few days at $\\sim 10^2\\,M_\\odot\\,{\\rm yr}^{-1}$.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2015-02-19T22:33:41.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "tidal disruption events",
      "massive black hole",
      "ultra-close encounters",
      "prompt hyperaccretion",
      "solar-type star"
    ],
    "publication": {
      "doi": "10.1088/2041-8205/805/2/L19"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 5,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1345427
    }
  }
}