{
  "id": "1011.3731",
  "version": "v1",
  "published": "2010-11-16T15:39:56.000Z",
  "updated": "2010-11-16T15:39:56.000Z",
  "title": "Neutron Stars in Supernovae and Their Remnants",
  "authors": [
    "Roger A. Chevalier"
  ],
  "comment": "8 pages, for Proceedings of Astrophysics of Neutron Stars 2010, Cesme, Turkey",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "The magnetic fields of neutron stars have a large range (~3e10 - 1e15 G). There may be a tendency for more highly magnetized neutron stars to come from more massive stellar progenitors, but other factors must also play a role. When combined with the likely initial periods of neutron stars, the magnetic fields imply a spindown power that covers a large range and is typically dominated by other power sources in supernovae. Distinctive features of power input from pulsar spindown are the time dependence of power and the creation of a low density bubble in the interior of the supernova; line profiles in the late phases are not centrally peaked after significant pulsar rotational energy has been deposited. Clear evidence for pulsar power in objects <300 years old is lacking, which can be attributed to large typical pulsar rotation periods at birth.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2010-11-16T15:39:56.000Z"
    }
  ],
  "analyses": {
    "subjects": [
      "96.60.Hv",
      "96.10.+i",
      "98.58.Mj",
      "97.10.Bt"
    ],
    "keywords": [
      "neutron stars",
      "large typical pulsar rotation periods",
      "significant pulsar rotational energy",
      "magnetic fields",
      "large range"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1063/1.3629476"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 8,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 877465,
      "adsabs": "2011AIPC.1379....5C"
    }
  }
}