{
  "id": "1106.5125",
  "version": "v2",
  "published": "2011-06-25T13:06:00.000Z",
  "updated": "2011-06-30T10:53:47.000Z",
  "title": "XMM-Newton observations of IGRJ18410-0535: The ingestion of a clump by a supergiant fast X-ray transient",
  "authors": [
    "E. Bozzo",
    "A. Giunta",
    "G. Cusumano",
    "C. Ferrigno",
    "R. Walter",
    "S. Campana",
    "M. Falanga",
    "G. Israel",
    "L. Stella"
  ],
  "comment": "Accepted for publication on A&A. V2: Inserted correct version of Fig.16",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "IGRJ18410-0535 is a supergiant fast X-ray transients. This subclass of supergiant X-ray binaries typically undergoes few- hour-long outbursts reaching luminosities of 10^(36)-10^(37) erg/s, the occurrence of which has been ascribed to the combined effect of the intense magnetic field and rotation of the compact object hosted in them and/or the presence of dense structures (\"clumps\") in the wind of their supergiant companion. IGR J18410-0535 was observed for 45 ks by XMM-Newton as part of a program designed to study the quiescent emission of supergiant fast X-ray transients and clarify the origin of their peculiar X-ray variability. We carried out an in-depth spectral and timing analysis of these XMM-Newton data. IGR J18410-0535 underwent a bright X-ray flare that started about 5 ks after the beginning of the observation and lasted for \\sim15 ks. Thanks to the capabilities of the instruments on-board XMM-Newton, the whole event could be followed in great detail. The results of our analysis provide strong convincing evidence that the flare was produced by the accretion of matter from a massive clump onto the compact object hosted in this system. By assuming that the clump is spherical and moves at the same velocity as the homogeneous stellar wind, we estimate a mass and radius of Mcl \\simeq1.4\\times10^(22) g and Rcl \\simeq8\\times10^(11) cm. These are in qualitative agreement with values expected from theoretical calculations. We found no evidence of pulsations at \\sim4.7 s after investigating coherent modulations in the range 3.5 ms-100 s. A reanalysis of the archival ASCA and Swift data of IGR J18410-0535, for which these pulsations were previously detected, revealed that they were likely to be due to a statistical fluctuation and an instrumental effect, respectively.",
  "revisions": [
    {
      "version": "v2",
      "updated": "2011-06-30T10:53:47.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "supergiant fast x-ray transient",
      "xmm-newton observations",
      "supergiant x-ray binaries typically undergoes",
      "compact object",
      "instruments on-board xmm-newton"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1051/0004-6361/201116726",
      "journal": "Astronomy and Astrophysics",
      "year": 2011,
      "month": "Jul",
      "volume": 531
    },
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 915979,
      "adsabs": "2011A&A...531A.130B"
    }
  }
}