{
  "id": "1302.1702",
  "version": "v1",
  "published": "2013-02-07T10:38:16.000Z",
  "updated": "2013-02-07T10:38:16.000Z",
  "title": "The Supergiant Fast X-ray Transient with the shortest orbital period: Suzaku observes one orbit in IGRJ16479-4514",
  "authors": [
    "L. Sidoli",
    "P. Esposito",
    "V. Sguera",
    "A. Bodaghee",
    "J. A. Tomsick",
    "K. Pottschmidt",
    "J. Rodriguez",
    "P. Romano",
    "J. Wilms"
  ],
  "comment": "Proceedings of \"An INTEGRAL view of the high-energy sky (the first 10 years)\" the 9th INTEGRAL Workshop, October 15-19, 2012, Paris, France, in Proceedings of Science (INTEGRAL 2012), Eds. A. Goldwurm, F. Lebrun and C. Winkler, (http://pos.sissa.it/cgi-bin/reader/conf.cgi?confid=176), id: PoS(INTEGRAL 2012)034",
  "categories": [
    "astro-ph.HE",
    "astro-ph.GA"
  ],
  "abstract": "The eclipsing hard X-ray source IGR J16479-4514 is the Supergiant Fast X-ray Transient (SFXT) with the shortest orbital period (3.32 days). This allowed us to perform a 250 ks long X-ray observation with Suzaku in 2012 February, covering most of its orbit, including the eclipse egress. Outside the eclipse, the source luminosity is around a few 1E34erg/s. The X-ray spectrum can be fit with an absorbed power law together with a neutral iron emission line at 6.4 keV. The column density is constant at 1E23 cm-2 outside the X-ray eclipse. During the eclipse it is lower, consistent with a scattering origin for the low X-ray emission during the eclipse by the supergiant companion wind. The scattered X-ray emission during the X-ray eclipse is used to directly probe the density of the companion wind at the orbital separation, resulting in 7E-14 g/cm3, which translates into a ratio Mdot_w/v_terminal = 7E-17 solar masses/km of the wind mass loss rate to the wind terminal velocity. This ratio, assuming reasonable terminal velocities in the range 500-3000 km/s, translates into an accretion luminosity two orders of magnitude higher than that observed. We conclude that a mechanism reducing the accretion rate onto the compact object is at work, likely due to the neutron star magnetosphere.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2013-02-07T10:38:16.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "supergiant fast x-ray transient",
      "shortest orbital period",
      "hard x-ray source igr",
      "ks long x-ray observation"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1217992,
      "adsabs": "2013arXiv1302.1702S"
    }
  }
}