{
  "id": "1701.09153",
  "version": "v1",
  "published": "2017-01-31T17:53:30.000Z",
  "updated": "2017-01-31T17:53:30.000Z",
  "title": "What we recently learnt about Crab: structure of the wind, the shock, flares and reconnection",
  "authors": [
    "Maxim Lyutikov"
  ],
  "comment": "Proceedings, Shklovsky 100",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "We can probe observationally and reproduce theoretically intricate properties of the Crab Nebula nearest to the pulsar - The Inner Knot. The tiny knot is indeed a bright spot on the surface of a quasi-stationary magnetic relativistic shock that accelerates particles. It is required that the part of the wind that produces the Inner Knot has low magnetization; thus, it is not a site of gamma-ray flares. We develop a model of particle acceleration during explosive reconnection events in relativistic highly magnetized plasma and apply the model to explain the Crab gamma-ray flares. Particles are efficiently accelerated by charge-starved DC-type electric fields during initial stages of magnetic flux merges. By implication, the magnetic reconnection is an important, and possibly dominant process of particle acceleration in high energy astrophysical sources.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2017-01-31T17:53:30.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "particle acceleration",
      "quasi-stationary magnetic relativistic shock",
      "inner knot",
      "reproduce theoretically intricate properties",
      "crab gamma-ray flares"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}